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XIV Latin American Regional IAU Meeting iii Contents XIV Latin American Regional IAU Meeting Preface vii Programme ix List of participants xiii Review & Invited Talks Short Talks Planetary Systems 27 Stars & Stellar Systems 41 Star Formation 85 ISM 95 Galaxies 103 AGN 141 Cosmology 153 High Energy Astrophysics 165 Instrumentation 173 Teaching & Outreach 183 Posters Planetary Systems 195 Stars & Stellar Systems 235 Star Formation 321 ISM 339 Galaxies 357 AGN 419 Cosmology 447 High Energy Astrophysics 473 Instrumentation 487 Author index v Preface From Santiago (1978), to Mérida (Venezuela, 1981), Buenos Aires (1983), Rio de Janeiro (1984), Mérida (México, 1986), Gramado (1989), Viña del Mar (1992), Montevideo (1995), Tonantzintla (1998), Córdoba (2001), Pucón (2005), Isla Margarita (2007), and Morélia (2010), Latin American Regional IAU Meetings (LARIM) have witnessed tremendous advances in astronomy world-wide, and particularly in Latin America. Throughout its 35-year-long history, LARIMs have played an important role in bringing together scientists from our countries, fostering collaborations and interchanges at various levels and different areas. Following this successful tradition, this 14th LARIM covers topics across the whole field of astronomy, comprising plenary, parallel and poster sessions dedicated to areas such as planetary systems, stars, stellar systems, star formation, ISM, galaxies, AGN, cosmology, high energy astrophysics, instrumentation, history, teaching and outreach. Scientific Organizing Committee: Zulema Abraham, IAG/USP, Brasil (chair) Roberto Cid Fernandes, UFSC, Brasil (chair) Alejandro Córsico, UNLP, Argentina Fernando Roig, ON, Brasil Leopoldo Infante, PUC, Chile William Lee, IA-UNAM, Mexico Tabaré Gallardo, Facultad de Ciencias, Uruguay Cesar Briceño Avila, CIDA, Venezuela Local Organizing Committee: Roberto Cid Fernandes, UFSC, Brasil Jane Gregorio-Hetem, IAG/USP, Brasil Abı́lio Mateus, UFSC, Brasil Bernardo Borges, UFSC, Brasil Daniela Pavani, UFRGS, Brasil Maria Jaqueline Vasconcelos, UESC, Brasil Natalia Vale Asari, UFSC, Brasil Silvia H. P. Alencar, UFMG, Brasil Sponsors: CAPES, CNPq, FAPEMIG, FAPESC, FAPESP, IAG, IAU, SAB, UFSC. Cover credits: Eduardo Lacerda; photos by Eduardo Schumacher & ESO/VVV Survey. vii viii Programme Final Programme Sun (24/Nov) Mon (25/Nov) Tue (26/Nov) Wed (27/Nov) Thu (28/Nov) Fri (29/Nov) 08:45 Opening 09:00 Review talk Review talk Review talk Review talk Review talk 09:40 Invited talk Invited talk Invited talk Invited talk Invited talk 10:10 Coffee & Posters Coffee & Posters Coffee & Posters Coffee & Posters Coffee & Posters 11:00 Parallel sessions Parallel sessions Parallel sessions Parallel sessions Parallel sessions 12:40 Lunch Lunch Lunch Lunch Lunch 15:00 Invited talk Invited talk Invited talk Invited talk 15:30 Review talk Review talk Review talk Invited talk 16:10 Invited talk Invited talk Invited talk Invited talk Coffee & Posters Coffee & Posters Coffee & Posters Coffee & Posters Parallel sessions Parallel sessions Parallel sessions Parallel sessions LARIM Assembly SAB Assembly 16:40 Registration 17:30 Free 19:10 20:00 Cocktail Conference Dinner Detailed program Parallel sessions are divided into the following areas: Planetary Systems (PS), Star formation (SF), Interstellar Medium (ISM), Galaxies (GAL), Active Galactic Nuclei (AGN), ix Stars & Stellar Systems (SSS), Vista Variables in the Via Lactea (VVV), Cosmology (COS), High Energy Astrophysics (HEAP), Instrumentation (INST), Teaching & Outreach (TO). For details click on individual links. Outreach (TO). For details click on individual links. Mon (25/Nov) 08:459:00 Tue (26/Nov) Wed (27/Nov) Thu (28/Nov) Fri (29/Nov) Opening Solar Transient Activity: Magnetic Energy Release and Topology C. Mandrini (IAFE, Argentina) White Dwarf Stars S. O. Kepler (UFRGS, Brazil) Galaxies at High Redshift F. Bauer (PUC, Chile) Testing Fundamental Hypotheses in Cosmology J. Alcaniz (ON, Brazil) 09:4010:10 Impact studies in Latin America G. Tancredi (IFFC, Uruguay) The SNC Meteorites M. E. Varela (ICATE, Argentina) The evolution of protoplanetary disk M. Schreiber (UV, Chile) The star formation history of galaxies in the CALIFA survey R. GonzálezDelgado (IAA, Spain) Multiple-tracer surveys of the large-scale structure of the Universe R. Abramo (USP, Brazil) 10:1011:00 Coffee & Posters Sessions GAL-1 SSS-1 PS-1 SF-1 Coffee & Posters Sessions GAL-2 SSS-3 PS-2 SF-2 Coffee & Posters Sessions GAL-3 SSS-5 PS-3 COS-1 Coffee & Posters Sessions GAL-4 SSS-6 HEAP-1 COS-2 Coffee & Posters Sessions GAL-6 SSS-8 HEAP-2 COS-3 11:0012:40 Short talks Parallel Sessions GAL-1 SSS-1 PS-1 SF-1 Short talks Parallel Sessions GAL-2 SSS-3 PS-2 SF-2 Short talks Parallel Sessions GAL-3 SSS-5 PS-3 COS-1 Short talks Parallel Sessions GAL-4 SSS-6 HEAP-1 COS-2 Short talks Parallel Sessions GAL-6 SSS-7 HEAP-2 COS-3 12:4015:00 Lunch Lunch Lunch Lunch Lunch A New Chinese Astronomy New Opportunities with the 09:0009:40 Distribution and Origin of Hot Planets C. Beauge (OAC, Argentina) ESO: Present x Outreach (TO). For details click on individual links. Mon (25/Nov) 08:459:00 15:0015:30 09:0009:40 15:3016:10 09:4010:10 10:1016:1011:00 16:40 11:0012:40 16:4017:30 12:4015:00 17:3019:10 15:0015:30 A New Chinese Opening Astronomy Center in Chile Z. Wang (CASSACA, Chile) Distribution and Origin of Hot Planets C. Beauge (OAC, Argentina) Supergiants, Stellar Winds and Mass-loss L. Cidale Impact (UNLP, studies in Latin Argentina) America G. Tancredi (IFFC, Uruguay) Tue (26/Nov) New Opportunities with the Gemini Observatory Solar M. Boccas Transient (Gemini Activity: Observatory, Magnetic USA) Energy Release and Topology C. Mandrini (IAFE, Argentina) Active Galactic Nuclei P. Arévalo The SNC (PUC, Chile) Meteorites M. E. Varela (ICATE, Argentina) Abundance determinations Coffee & in ionized Posters nebulae and Sessions their GAL-1 sensitivity to SSS-1 temperature PS-1 M. Rodríguez SF-1 (INAOE, Mexico) Short talks Parallel Coffee & Sessions Posters GAL-1 Sessions SSS-1 SSS-2 PS-1 AGN-1 SF-1 ISM-1 INST-1 Diversity of protoplanetary Coffee & disks in stellar Posters clusters: the Sessions case of the GAL-2 sigma Orionis SSS-3 cluster PS-2 J. Hernández SF-2 (CIDA, Venezuela) Short talks Parallel Coffee & Sessions Posters GAL-2 Sessions SSS-3 SSS-4 PS-2 AGN-2 SF-2 ISM-2 INST-2 Lunch Lunch Short talks Parallel Sessions SSS-2 A New Chinese AGN-1 Astronomy ISM-1 in Chile Center INST-1 Z. Wang (CASSACA, Chile) Short talks Parallel New Sessions Opportunities SSS-4 with the AGN-2 Gemini ISM-2 Observatory INST-2 M. Boccas (Gemini Observatory, USA) Wed (27/Nov) White Dwarf Stars S. O. Kepler (UFRGS, Brazil) The evolution of protoplanetary disk M. Schreiber (UV, Chile) Free Coffee & Posters Sessions GAL-3 SSS-5 PS-3 COS-1 Short talks Parallel Sessions GAL-3 SSS-5 PS-3 COS-1 Lunch xi Thu (28/Nov) Fri (29/Nov) ESO: Present and Future A. Kaufer (ESO, Chile) Mmtron T. de Graauw (ALMA, Chile) Galaxies at High Redshift F. Bauer (PUC, Chile) Testing Fundamental Hypotheses in Cosmology J. Alcaniz The SOFIA (ON, Brazil) Airborne Galactic Dynamics: Origin, History, The starand Present formation Prospect history of B. Pichardo galaxies (UNAM, in the CALIFA survey Mexico) R. GonzálezDelgado (IAA, Spain) Determining Coffee & the distances Posters of the Sessions structures GAL-4 surrounding SSS-6 super-massive HEAP-1 black holes COS-2 K. Steenbrugge (UCN, Chile) Short talks Parallel Coffee & Sessions Posters GAL-4 Sessions SSS-6 SSS-7 HEAP-1 GAL-5 COS-2 AGN-3 TO-1 Infrared Observatory first science highlights and Multiple-tracer future science surveys of the potential large-scale H. Zinnecker structure of (SOFIA the Universe Science Center, R. Abramo NASA, USA) (USP, Brazil) Star and planet Coffee & formation Posters in the era of the Sessions submillimeter GAL-6 observatories SSS-8 SMA/ALMA HEAP-2 L. Zapata COS-3 (UNAM, Mexico) Short talks Parallel Sessions Coffee & GAL-6 Posters SSS-7 Sessions HEAP-2 SSS-9 COS-3 GAL-7 TO-2 Lunch Lunch Short talks Parallel Sessions VVV-1 GAL-5 ESO: Present AGN-3 and Future TO-1 A. Kaufer (ESO, Chile) Short talks Parallel Sessions SSS-8 GAL-7 Mmtron VVV-2 T. de Graauw TO-2 (ALMA, Chile) xii List of participants Mario Gabriel ABADI, Observatorio Astronómico-IATE, Universidad Nacional de Cordoba-CONICET, Argentina [email protected] Zulema ABRAHAM, IAG/USP, Brazil [email protected] Luis Raul ABRAMO, Instituto de Fı́sica, Universidade de São Paulo, Brazil [email protected] Ximena Celeste ABREVAYA, IAG - Universidade de Sao Paulo, Brazil [email protected] Gustavo Adolfo AGUAYO, Universidad de Concepcion, Chile [email protected] Michel AGUENA DA SILVA, Universidade de São Paulo - Instituto de Fı́sica, Brazil [email protected] Paula AGUIRRE, Universidad Andrés Bello, Chile, Chile [email protected] Carolina Belen AGURTO GANGAS, Universidad de Valparaiso, Chile [email protected] Lara ALBANESE, INAF, OSSERVATORIO DI ARCETRI, Italy [email protected] Jailson ALCANIZ, Observatório Nacional , Brazil [email protected] Silvia Helena Paixão ALENCAR, Dep. de Fisica - ICEx - UFMG, Brazil [email protected] Silvia Teixeira ALEXANDRE, Federal University of Rio de Janeiro, Brazil [email protected] Leonardo Andrade ALMEIDA, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas - IAG/USP, Brazil [email protected] Pedro Viana ALMEIDA, Universidade Federal de Minas Gerais, Portugal [email protected] Javier ALONSO-GARCÍA, Pontificia Universidad Católica de Chile, Chile [email protected] xiii Alvaro ALVAREZ-CANDAL, Observatório Nacional, Brazil [email protected] Virgı́nia Mello ALVES, Universidade Federal de Pelotas (UFPel), Brazil [email protected] Eliana Maritza AMAZO-GOMEZ, Universidad Nacional de Colombia, Colombia [email protected] Alexandre AMORIM, Núcleo de Estudo e Observação Astronômica ”José Brazilı́cio de Souza”, Brazil [email protected] Inaiara Saraceni de ANDRADE, Universidade de São Paulo, Brazil [email protected] Ileana ANDRUCHOW, Instituto de Astrofı́sica de La Plata - IALP/CONICET, Facultad de Ciencias Astronómicas y Geofı́sicas - FCAGLP/UNLP, Argentina [email protected] Mateus de Souza ANGELO, Universidade Federal de Minas Gerais, Brazil [email protected] Rodolfo ANGELONI, Departamento de Astronomı́a y Astrofı́sica - Pontificia Universidad Católica de Chile, Chile [email protected] Ignacio ARAYA, Universidad de Valparaı́so, Chile [email protected] Santiago ARCEO-DIAZ, Universidad de Guanajuato, Mexico., Mexico [email protected] Catalina Alejandra ARCOS, Universidad de Valparaı́so, Chile [email protected] Patricia AREVALO, Universida Andrés Bello & Pontificia Universidad Católica, Chile [email protected] Julia Ines ARIAS, Universidad de La Serena, Chile [email protected] Cristóbal ARMAZA, Pontifica Universidad Católica de Chile, Chile [email protected] Edmundo Marcelo ARNAL, Instituto Argentino de Radioastronomia (IAR), CONICET, CCT-La PLata y Facultad de Ciencias Astronómicas y Geofı́sicas (FCAG), Universidad Nacional de La Plata, Argentina [email protected] Maria Celeste ARTALE, Instituto de Astronomı́a y Fı́sica del Espacio (IAFE), Argentina [email protected] Hernán ASOREY, GIRG, Escuela de Fı́sica, Universidad Industrial de Santander, Colombia [email protected] Anelise AUDIBERT, Universidade Federal do Rio Grande do Sul, Brazil [email protected] Vladimir AVILA-REESE, Instituto de Astronomı́a, UNAM, Mexico [email protected] Luiz Mauricio AZANHA, Universidade de São Paulo, Brazil [email protected] xiv Eduardo BALBINOT, Universidade Federal do Rio Grande do Sul, Brazil [email protected] Raymundo BAPTISTA, Universidade Federal de Santa Catarina (UFSC), Brazil [email protected] Laura Daniela BARAVALLE, Facultad de Matemática, Astronomı́a y Fı́sica. Universidad Nacional de Córdoba, Argentina [email protected] Rodolfo H. BARBA, Universidad de La Serena, Chile [email protected] Ulisses BARRES DE ALMEIDA, Centro Brasileiro de Pesquisas Fisicas (CBPF/MCTI), Brazil [email protected] Caio BARROS SIMÕES DE ALMEIDA, Universidade Federal do ABC (UFABC), Brazil [email protected] Franz Erik BAUER, Pontificia Universidad Católica de Chile, Chile [email protected] Juan Carlos BEAMÍN, Pontificia Universidad Católica de Chile, Chile [email protected] Cristian BEAUGE, Observatorio Astronomico, Universidad Nacional de Cordoba, Argentina [email protected] Dino BEGHETTO JUNIOR, UNIVAP - Universidade do Vale do Paraı́ba, Brazil [email protected] Diogo BELLONI, Universidade Federal do Rio de Janeiro, Brazil [email protected] Rodrigo BERNADELLI, Universidade Federal de Santa Catarina, Brazil [email protected] Cristian Giovanny BERNAL, Instituto de Astronomı́a - UNAM, Mexico [email protected] Rafael Luiz BERNARDI, Universidade Federal de Santa Catarina, Brazil [email protected] Armando BERNUI, Observatório Nacional, MCTI, Brazil [email protected] Beatriz BLANCO SIFFERT, Instituto de Fı́sica - Universidade Federal do Rio de Janeiro, Brazil [email protected] Maxime BOCCAS, Gemini Observatory, Chile [email protected] Bernardo Walmott BORGES, Universidade Federal de Santa Catarina (UFSC) - Campus Araranguá, Brazil [email protected] Daniela BORGES PAVANI, Departamento de Astronomia/IF/UFRGS, Brazil [email protected] Jura BORISSOVA, Departamento de Fı́sica y Astronomı́a, Facultad de Ciencias, UNIVERSIDAD DE VALPARAÍSO, Chile [email protected] xv Germano BORTOLOTTO, Universidade Federal de Santa Catarina, Brazil [email protected] Rodrigo Carlos BOUFLEUR, Observatório Nacional - MCTI, Brazil [email protected] Joao BRAGA, INPE, Brazil [email protected] Pedro Ivo de Oliveira BRASIL, Instituto Nacional de Pesquisas Espaciais - INPE, Brazil pedro [email protected] Paulo Sergio BRETONES, Universidade Federal de São Carlos, Brazil [email protected] Eduardo Rondon BRICEÑO, Observatorio nacional , Brazil [email protected] Albert BRUCH, Laboratório Nacional de Astrofı́sica, Brazil [email protected] Carine BRUM, Universidade Federal De Santa Maria, Brazil [email protected] Gustavo BRUZUAL, CRyA, UNAM, Campus Morelia, Mexico [email protected] Julio Ignacio BUENO DE CAMARGO, Observatório Nacional / MCTI, Brazil [email protected] Filomena BUFANO, Universidad Andres Bello, Chile [email protected] Blakesley BURKHART, University of Wisconsin Madison (USA), Universidade Federal do Rio Grande do Norte (Brazil), United States [email protected] Claudio CACERES, Universidad de Valparaiso, Chile [email protected] Rolando CALDERÓN ARDILA, Universidad Industrial de Santander, Colombia [email protected] Diego Nicolás CALDERÓN ESPINOZA, Pontificia Universidad Católica de Chile, Chile [email protected] Marcos Rogerio CALIL, Planetário e Teatro Digital de Santo André - Johannes Kepler, Brazil [email protected] Nelson CALLEGARI JR., UNESP, Brazil [email protected] Hugo Orlando CAMACHO CHAVEZ, Departamento de Fı́sica Matemática. Instituto de Fı́sica. Universidade de São Paulo, Brazil [email protected] Jose Iván CAMPOS-ROZO, Universidad Nacional de Colombia, Colombia [email protected] Luis E. CAMPUSANO, Departamento de Astronomia, Universidad de Chile, Chile [email protected] xvi Graeme Nicholas CANDLISH, Universidad de Concepción, Chile [email protected] Hector CANOVAS, Departamento de Fisica y Astronomı́a, Universidad de Valparaı́so, Valparaı́so, Chile, Chile [email protected] Elenna CAPOTE, Massachusetts Institute of Technology, Pontifica Universidad Catolica de Chile, United States [email protected] Cristina Elisabet CAPPA, Instituto Argentino de Radioastronomı́a, CONICET, Argentina, y Facultad de Ciencias Astronómicas y Geofı́sicas, UNLP, Argentina , Argentina [email protected] Anderson CAPRONI, Universidade Cruzeiro do Sul, Brazil [email protected] Julio A. CARBALLO-BELLO, Universidad de Chile, Chile [email protected] Alex C. CARCIOFI, IAG/USP, Brazil [email protected] Adair CARDOSO, Universidade Federal de Santa Catarina, Brazil [email protected] Marı́lia Gabriela CARDOSO CORRÊA CARLOS, Instituto Nacional de Pesquisas Espaciais, Brazil [email protected] César Augusto CARETTA, Universidad de Guanajuato (Departamento de Astronomı́a), Mexico, Mexico [email protected] Carolina Moura CARNEIRO, Observatório do Valongo - Universidade Federal do Rio de Janeiro, Brazil [email protected] Eleazar Rodrigo CARRASCO, Gemini Observatory, Southern Operations Center, Chile [email protected] Maiara Sampaio CARVALHO, Laboratorio de Astrofisica Teorica e Observacional, Universidade Estadual de Santa Cruz, Brazil [email protected] Jorge M. CARVANO, Observatório Nacional , Brazil [email protected] Rigoberto CASAS MIRANDA, Universidad Nacional de Colombia, Colombia [email protected] Hector O. CASTAÑEDA, Escuela Superior de Fisica y Matematicas - Instituto Politécnico Nacional, Mexico [email protected] Camile Mendes CASTILHO, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo, Brazil [email protected] Márcio CATELAN, Pontificia Universidad Católica de Chile, Chile [email protected] João Paulo Nogueira CAVALCANTE, Observatório do Valongo - Universidade Federal do Rio de Janeiro, Brazil [email protected] xvii Oscar CAVICHIA, Universidade de São Paulo, Brazil [email protected] José R. CECATTO, DAS-INPE, Brazil [email protected] Jan CECHURA, Astronomical Institute, Academy of Sciences of the Czech Republic, Faculty of Mathematics and Physics, Charles University in Prague, Czech Republic [email protected] César Alexander CHACÓN-CARDONA, Universidad Nacional de Colombia, Colombia [email protected] Julio CHANAMÉ, Pontificia Universidad Católica de Chile, Chile [email protected] Germán CHAPARRO, Kapteyn Astronomical Institute (previous), Universidad Sergio Arboleda (current), Colombia [email protected] Ana CHIES-SANTOS, University of Nottingham, UK, United Kingdom Ana.Chies [email protected] Marcel CHOW MARTINEZ, Universidad de Guanajuato, Mexico [email protected] Nathália CIBIRKA, Universidade de São Paulo, Brazil [email protected] Silvina CICHOWOLSKI, Instituto de Astronomı́a y Fı́sica del Espacio, Argentina [email protected] Roberto CID FERNANDES, Universidade Federal de Santa Catarina, Brazil [email protected] Lydia Sonia CIDALE, Universidad de La Plata, Argentina [email protected] Alejandro CLOCCHIATTI, Pontificia Universidad Catolica de Chile, Chile [email protected] Bruno COELHO, Observatório do Valongo/UFRJ, Brazil [email protected] Paula R. T. COELHO, Universidade Cruzeiro do Sul, Brazil [email protected] Valeria COENDA, IATE - Observatorio Astronómico de Córdoba, Argentina [email protected] Roger COHEN, Universidad de Concepcion, Chile [email protected] Georgina COLDWELL, ICATE - CONICET, FCEFyN - Universidad Nacional de San Juan, Argentina [email protected] Cesar Augusto Huanca CONDORI, Observatório Nacional, Brazil [email protected] Sergio Antonio CONTRERAS, Pontificia Universidad Católica de Chile, Chile [email protected] xviii Rodrigo CONTRERAS RAMOS, Universidad Catolica de Chile, Chile [email protected] Fernando CORTÉS-SERRANO, Escuela de Fı́sica, Universidad Industrial de Santander, Colombia [email protected] Arianna CORTESI, Nottingham University, United Kingdom [email protected] Mariela Alejandra CORTI, FCAG(UNLP) - IAR(CONICET), Argentina [email protected] Marcus Vinı́cius COSTA DUARTE, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas - Universidade de São Paulo, Brazil [email protected] Guilherme COUTO, IF-UFRGS, Brazil [email protected] Alicia CRUZADO, Facultad de Ciencias Astronómicas y Geofı́sicas, Universidad Nacional de La Plata, Argentina [email protected] Jorge CUADRA, P. Universidad Católica de Chile, Chile [email protected] Pablo Andrés CUARTAS-RESTREPO, Universidad de Antioquia, Colombia [email protected] Héctor CUEVAS, Universidad de La Serena, Chile [email protected] Katia CUNHA, Observatorio Nacional - MCTI, Brazil [email protected] Michel CURÉ, Departamento de Fisica y Astronomia, Facultad de Ciencias, Universidad de Valparaiso, Chile [email protected] Flavio D’AMICO, Instituto Nacional de Pesquisas Espaciais - INPE, Brazil [email protected] Clayton Garcia DA SILVA, Universidade de São Paulo, Brazil [email protected] Luidhy Santana DA SILVA, Universidade Estadual do Ceará, Brazil [email protected] Giannina DALLE MESE, Instituto Nacional de Astrofisica, Optica y Electronica, Mexico [email protected] Natacha Zanon DAMETTO, Universidade Federal do Rio Grande do Sul, Brazil [email protected] Jorge Gonzales DAVALOS, Observatorio Nacional, Brazil [email protected] André Luiz DE AMORIM, Universidade Federal de Santa Catarina, Brazil [email protected] Marcio Guilherme Bronzato DE AVELLAR, Universidade de São Paulo (IAG), Brazil [email protected] xix Marı́a Silvina DE BIASI, Instituo de Astrofı́sica de La Plata (CCT-La PLata CONICET) y Facultad de Ciencias Astronómicas y Geofı́sicas, Universidad Nacional de La Plata, Argentina , Argentina mariasilvina [email protected] Elisabete M. DE GOUVEIA DAL PINO, Universidade de Sao Paulo, Brazil [email protected] Thijs DE GRAAUW, ESO, Chile [email protected] Jose Ignacio Garcia DE LA ROSA, Observatorio do Valongo, Brazil [email protected] Luiz Alberto DE PAULA, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas da Universidade de São Paulo, Brazil [email protected] Mario Nascimento DE PRA, Observatório Nacional, Brazil [email protected] Cleiton Carillo DE SOUZA, Universidade Estadual de Santa Cruz, Brazil [email protected] João Eduardo DE SOUZA DA FONSECA, Universidade Estadual Paulista - UNESP, Brazil [email protected] Istvan DEKANY, Instituto de Astrofisica, Pontificia Universidad Catolica de Chile, Chile [email protected] Maria Victoria DEL VALLE, Instituto Argentino de Radioastronomia IAR, Argentina [email protected] Gloria DELGADO INGLADA , Instituto de Astronomı́a, Universidad Nacional Autónoma de México , Mexico [email protected] Josselin DESMARS, Observatorio Nacional de Rio de Janeiro, Brazil [email protected] Bruno DIAS, IAG/Universidade de São Paulo, Brazil [email protected] Rafael Augusto Garcia DIAS, Universidade Federal do Rio Grande do Sul, Brazil [email protected] Wilton S. DIAS, Universidade Federal de Itajuba, Brazil [email protected] Alex DIAS DE OLIVEIRA, Observatório Nacional, Brazil [email protected] Marlon R. DINIZ, Universidade Federal de Santa Maria, Brazil [email protected] Suzi Izaquiel Ferreira DINIZ, Universidade Federal do Rio Grande do Sul, Brazil [email protected] Isadora Bicalho DOMINGOS, Observatório Nacional, Brazil [email protected] Josué Cardoso DOS SANTOS, Universidade Estadual Paulista-UNESP (São Paulo State University), Brazil [email protected] xx Hélio DOTTO PEROTTONI, Universidade Federal do Rio de Janeiro, Brazil [email protected] Horacio Alberto DOTTORI, Universidade Federal do Rio Grande do Sul, Brazil [email protected] Daniel Alf DREHMER, Instituto de Fı́sica - Universidade Federal do Rio Grande do Sul, Brazil [email protected] João Pedro Wojcikiewicz DUARTE SILVA, Universidade Federal de Santa Catarina, Brazil [email protected] Jânia DUHA, Instituto Federal do Paraná, Brazil [email protected] Fernanda DUPLANCIC, Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE), Argentina [email protected] Paul EIGENTHALER, Instituto de Astronomı́a y Astrofı́sica, Pontificia Universidad Católica de Chile, Chile [email protected] Andres ESCALA, Universidad de Chile, Chile [email protected] Cyril ESCOLANO, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Brazil [email protected] Cesar ESTEBAN, Instituto de Astrofı́sica de Canarias, Spain [email protected] Daniel Moser FAES, Instituto de Astronomia, Geofı́sica e Ciências Atmosféicas, Universidade de São Paulo, Brazil [email protected] Adriano FAGUNDES, Universidade Federal de Santa Catarina, Brazil [email protected] Jacqueline Kelly FAHERTY, Universidad de Chile/Carnegie Institute (DTM), Chile [email protected] Nelson FALCON, Universidad de Carabobo, Venezuela [email protected] Marcos Antonio Fonseca FARIA, Universidade Federal de Itajubá, Brazil [email protected] Jamille Almeida FEITOSA, Universidade Estadual de Santa Cruz, Brazil [email protected] Michael FELLHAUER, Departamento de Astronomia, Universidad de Concepcion, Chile, Chile [email protected] Oscar Luis FERLE, Universidade Cruzeiro do Sul, Brazil [email protected] Mateus César FERNANDES, Universidade Federal do Rio de Janeiro, Brazil [email protected] Sylvio FERRAZ MELLO, IAG-USP, Brazil [email protected] xxi Andressa Cristina Silva FERREIRA, Universidade de São Paulo, Brazil [email protected] Carlos Eduardo FERREIRA LOPES, Universidade Federal do Rio Grande do Norte, Brazil carlos [email protected] Natasha FIORETTO AGUERO, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas (IAG), Universidade de São Paulo (USP), Brazil [email protected] Verónica FIRPO, Universidad de La Serena, Chile [email protected] Matias Gastón FLORES, Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE) , Argentina [email protected] Jaime FORERO-ROMERO, Universidad de los Andes, Colombia [email protected] Fabrı́cio Catani FREITAS, Universida de São Paulo, Brazil [email protected] Priscila FREITAS-LEMES, Universidade do Vale do Paraı́ba, Brazil [email protected] Amancio Cesar Santos FRIACA, IAG-USP, Brazil [email protected] Lucas FROZZA SECCO, University of São Paulo, Brazil [email protected] Isaura L. FUENTES-CARRERA, Escuela Superior de Fı́sica y Matemáticas, Instituto Politécnico Nacional, Mexico [email protected] Gaspar GALAZ, Instituto de Astronomia, P. Universidad Catolica de Chile, Chile [email protected] Lluis GALBANY, CENTRA - Centro Multidisciplinar de Astrofı́sica, Instituto Superior Técnico, Departamento de Astronomı́a, Universidad de Chile, Chile [email protected] Tabare GALLARDO, Instituto de Fisica, Facultad de Ciencias, Universidad de la Republica, Uruguay [email protected] Alexandre GALLENNE, Universidad de Concepcion, Chile [email protected] Phillip GALLI, Universidade de São Paulo, IAG, Brazil [email protected] Diana GAMA, IAG/USP, Brazil [email protected] Juan Nicolas GARAVITO, Universidad de los Andes, Colombia [email protected] Federico GARCÍA, Instituto Argentino de Radioastronomı́a (IAR-CONICET), Argentina [email protected] Miguel Angel GARCIA CALDERON, Universidad Distrital Francisco Jose de Caldas, Colombia [email protected] xxii Alejandro GARCÍA VARELA, Universidad de los Andes, Bogotá, Colombia [email protected] Felipe GARRIDO, P. Universidad Católica de Chile, Chile [email protected] Hernán Enrique GARRIDO, Universidad de Concepción, and European Southern Observatory, Chile [email protected] Claudio GERMANÀ, Departamento de Fı́sica, Universidade Federal do Maranhão, Brazil [email protected] Elsa Beatriz GIACANI, Instituto de Astronomı́a y Fı́sica del Espacio, Argentina [email protected] Breno Loureiro GIACCHINI, Centro Brasileiro de Pesquisas Fı́sicas, Brazil [email protected] Ricardo GIL-HUTTON, Complejo Astronómico El Leoncito - CONICET, Argentina [email protected] Rafael Santiago GIROLA, Universidad Nacional de Tres de Febrero, Argentina [email protected] Silvia Maria GIULIATTI WINTER, UNESP-Univ. Estadual Paulista, Brazil [email protected] Cristian Alberto GOEZ, OLIMPIADAS COLOMBIANAS DE ASTRONOMIA Y ASTROFISICA, Colombia [email protected] Rodney S. GOMES, Observatório Nacional, Brazil [email protected] Altair Ramos GOMES JUNIOR, Observatório do Valongo - Universidade Federal do Rio de Janeiro, Brazil [email protected] Matias GOMEZ, Universidad Andres Bello, Chile [email protected] Maria Fernanda GÓMEZ ÁLVAREZ , Universidad de los Andes, Colombia [email protected] Denise R. GONÇALVES, Observatório do Valongo - UFRJ, Brazil [email protected] Thiago Signorini GONÇALVES, Observatório do Valongo, Universidade Federal do Rio de Janeiro, Brazil [email protected] Oscar A. GONZALEZ, European Southern Observatory, Chile [email protected] Roberto GONZALEZ, Departamento de Astronomı́a y Astrofı́sica, Pontificia Universidad Catolica, Chile [email protected] Rosa Marı́a GONZÁLEZ DELGADO, Instituto de Astrofı́sica de Andalucı́a (CSIC), Spain [email protected] Danilo GONZALEZ DIAZ, Universidad Nacional de Colombia, Colombia [email protected] xxiii Santiago GONZALEZ GAITAN, Universidad de Chile, Chile [email protected] Javier Ernesto GONZÁLEZ SÁNCHEZ , Observatório Nacional, Brazil [email protected] Kevin GOVENDER, International Astronomical Union Office of Astronomy for Development, South Africa (zuid Afrika) [email protected] Jane GREGORIO-HETEM, Universidade de Sao Paulo - IAG/USP, Brazil [email protected] Monica Gladys GROSSO, Instituto de Ciencias Astronómicas de la Tierra y del Espacio, ICATE-CONICET, Argentina [email protected] Rafael Fraga GUERÇO, Observatório Nacional - Rio de Janeiro - Brasil, Brazil [email protected] Walter Robert GUEVARA DAY, CONIDA - AGENCIA ESPACIAL DEL PERU, Peru [email protected] Sebastian GUROVICH, Observatorio Astronomico de Cordoba, Argentina [email protected] Claudia Patricia GUTIÉRREZ, Universidad de Chile, Chile [email protected] Gergely HAJDU, Pontificia Universidad Católica de Chile, Chile [email protected] Margaret M. HANSON, University of Cincinnati, USA, United States [email protected] Moiré Gonçalves HENNIG, Universidade Federal de Santa Maria, Brazil [email protected] Herman HENSBERGE, Royal Observatory of Belgium, Brazil [email protected] Jesus Omar HERNANDEZ, Centro de Investigaciones de Astronomia, Venezuela [email protected] Jose Andres HERNANDEZ, Universidade Federal do Rio Grande do Sul, Brazil [email protected] Fábio Rafael HERPICH, Universidade Federal de Santa Catarina, Brazil [email protected] Annibal HETEM, UFABC - Universidade Federal do ABC, Brazil [email protected] Gabriel Rodrigues HICKEL, Universidade Federal de Itajubá, Brazil [email protected] Ana Maria HIDALGO-GÁMEZ, Escuela Superior de Fı́sica y Matemáticas, Instituto Politécnico Nacional, Mexico [email protected] Mario Armando HIGUERA GARZÓN, Universidad Nacional de Colombia, Colombia [email protected] xxiv Karianne HOLHJEM, Southern Astrophysical Research (SOAR) telescope, Chile, Chile [email protected] Mariela HUAMAN ESPINOZA, UNESP - UNIVERSIDADE ESTADUAL PAULISTA ”Júlio de Mesquita Filho”, Brazil [email protected] Jiasheng HUANG, Chinese Academy of Sciences South America Center for Astronomy, Chile [email protected] Hector Javier IBARRA MEDEL, INAOE, Mexico [email protected] Francisco JABLONSKI, Astrophysics Division, INPE/MCTI, Brazil [email protected] Yara Lorena JAFFE, Universidad de Concepcion, Chile [email protected] Eduardo JANOT PACHECO, USP-IAG, Brazil [email protected] Marcelo Daniel JAQUE, ICATE-CONICET/Universidad Nacional de San Juan , Argentina [email protected] Vera JATENCO-PEREIRA, Universidade de São Paulo, Brazil [email protected] Noelia JIMENEZ, CONICET, University of Trieste, Italy [email protected] Emiliano JOFRÉ, Observatorio Astronómico de Córdoba, Argentina [email protected] Matias JONES, Universidad de Chile, Chile [email protected] Astor João Schönell JÚNIOR, Universidade Federal do Rio Grande do Sul, Brazil [email protected] Luı́s Henrique Sinki KADOWAKI, Universidade de São Paulo (IAG/USP), Brazil [email protected] Antonio KANAAN, Universidade Federal de Santa Catarina., Brazil [email protected] Samer KANAAN, Universidad de Valparaiso , Chile [email protected] Andreas KAUFER, European Southern Observatory, Chile [email protected] Pierre KAUFMANN, Universidade Presbiteriana Mackenzie, Brazil [email protected] S. O. KEPLER, Universidade Federal do Rio Grande do Sul, Brazil [email protected] Behrouz KHIALI, University of Sao Paulo- IAG/USP, Brazil [email protected] xxv Jessica Reis KITAMURA, Universidade Cruzeiro do Sul, Brazil [email protected] Radostin Georgiev KURTEV, Universidad de Valparaiso, Chile [email protected] Eduardo Alberto Duarte LACERDA, Universidade Federal de Santa Catarina, Brazil [email protected] Régis LACHAUME, P. Universidad Catolica de Chile, Chile [email protected] Paulo Jakson Assunção LAGO, Universidade de São Paulo, Brazil [email protected] Natália Rezende LANDIN, Universidade Federal de Viçosa - campus UFV Florestal, Brazil [email protected] Gustavo A. LANFRANCHI, NAT - Universidade Cruzeiro do Sul, SP-Brasil, Brazil [email protected] Rodolfo LANGHI, UNESP/Bauru - Universidade Estadual Paulista ”Julio de Mesquita Filho”, Brazil [email protected] Maritza Arlene LARA-LOPEZ, Australian Astronomical Observatory, Australia [email protected] Andres Baquero LARRIVA, Escuela Politecnica Nacional del Ecuador, Ecuador [email protected] Daniela LAZZARO, Observatório Nacional, Brazil [email protected] Rodrigo Andrés LEIVA ESPINOZA, Instituto de Astrofı́sica, Pontificia Universidad Católica de Chile, Chile [email protected] Jacques R. D. LEPINE, Universidade de São Paulo, Brazil [email protected] Peter LEROY, PONTIFICIA UNIVERSIDADE CATOLICA DE MINAS GERAIS,MUSEU DE CIENCIAS NATURAIS, Brazil [email protected] Orlando Hugo LEVATO, Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE) , Argentina [email protected] Eliade Ferreira LIMA, Universidade Federal do Rio Grande do Sul, Brazil [email protected] Gustavo Henrique R. de Araújo LIMA, Departamento de Fı́sica - Universidade Federal de Minas Gerais, Brazil [email protected] Marcos LIMA, Universidade de São Paulo, Brazil [email protected] Maria Luiza LINHARES DANTAS, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas da Universidade de São Paulo, Brazil [email protected] Gianluca LOMBARDI, European Southern Observatory, Chile [email protected] xxvi Alexandre Roman LOPES, Universidad de La Serena, Chile [email protected] Amanda LOPES, Observatório do Valongo (OV/UFRJ), Brazil [email protected] Raimundo LOPES DE OLIVEIRA FILHO, Universidade Federal de Sergipe, Brazil [email protected] Sebastian LOPEZ , Universidad de Chile, Chile [email protected] Paula Carolina LÓPEZ ESPINOZA, Universidad de Chile, Chile [email protected] Rafael LÓPEZ FERNÁNDEZ, Instituto de Astrofı́sica de Andalucı́a - CSIC, Spain [email protected] Francisco LÓPEZ-GARCÍA, UNSJ Argentina, Argentina [email protected] Zulema LÓPEZ-GARCÍA, ICATE ARGENTINA, Argentina [email protected] Diego LORENZO DE OLIVEIRA, Universidade Federal do Rio de Janeiro - Observatório do Valongo, Brazil [email protected] Eduardo LOURENCO DE ANDRADE, Universidade Federal de Santa Catarina, Brazil [email protected] Gerardo Juan Manuel LUNA, Instituto de Astronomia y Fı̀sica del Espacio (IAFE), Argentina [email protected] Elmer Fidel LUQUE, Universidade Estadual de Santa Cruz, Brazil [email protected] Josué Antunes de MACÊDO, Instituto Federal de Educação, Ciência e Tecnologia do Norte de Minas Gerais, Brazil [email protected] Daniel Iria MACHADO, Unioeste / Foz do Iguaçu, Brazil [email protected] Antonio Mario MAGALHAES, IAG - Universidade de Sao Paulo, Brazil [email protected] Victor de Souza MAGALHÃES, Currently unaffiliated , Brazil [email protected] Marcelo Tucci MAIA, Instituto de Astronomia, Geofı́sca e Ciências Atmosfericas, Universidade de São Paulo., Brazil [email protected] Vincenzo MAINIERI, ESO, Germany [email protected] Martin MAKLER, Brazilian Center for Physics Research, CBPF/ICRA, Brazil [email protected] Stella Maris MALARODA, ICATE-CONICET, Argentina [email protected] xxvii Victoria Eugenia MALDONADO, Instituto de Astronomı́a Teórica y Experimental (IATE), Argentina [email protected] Brisa Llaneth MANCILLAS VAQUERA, Universidad Nacional Autónoma de México, Mexico [email protected] Cristina H. MANDRINI, Instituto de Astronomı́a y Fı́sica del Espacio, Argentina [email protected] Paula MARCHIANO, Facultad de Ciencias Astronómicas y Geofı́sicas, Universidad Nacional de La Plata, Argentina paula [email protected] Gabriela Antunes MARQUES, Observatório Nacional, Brazil [email protected] Hector Julian MARTINEZ, IATE - Observatorio Astronomico Universidad Nacional de Cordoba, Argentina, Argentina [email protected] Sandra M. MARTÍNEZ, Escuela de Fı́sica, Universidad Industrial de Santander, Colombia [email protected] Louise Giansante MARTINS, Universidade de São Paulo, Brazil [email protected] Lucimara MARTINS, Núcleo de Astrofı́sica Teórica -Universidade Cruzeiro do Sul (NAT-UCS), Brazil [email protected] Roberto Vieira MARTINS, Observatório Nacional, Brazil [email protected] Silvia Lorenz MARTINS, Universidade Federal do Rio de Janeiro - Observatório do Valongo, Brazil [email protected] Walter Silva MARTINS-FILHO, Observatório Nacional, Brazil [email protected] Eder MARTIOLI, Laboratorio Nacional de Astrofisica - LNA/MCTI, Brazil [email protected] Abı́lio MATEUS, Universidade Federal de Santa Catarina, Brazil [email protected] Salomé MATOS, Royal Observatory of Edinburgh, University of Edinburgh, United Kingdom [email protected] Maria Fátima MATTIELLO-FRANCISCO, Instituto Nacional de Pesquisas Espaciais (INPE), Brazil [email protected] Ana Carolina MATTIUCI, Universidade Estadual do Rio Grande do Norte, Brazil [email protected] Francesco MAURO, Universidad de Concepcion, Chile [email protected] Daniel MAY, Instituto de Astronomia e Ciências Atmosféricas - USP, Brazil [email protected] Natalia Lorena MAZA, Instituto de Ciencias Astronómicas, de la Tierra y del Espacio , Argentina [email protected] xxviii Alfredo Javier MEJÍA, Centro de Investigaciones de Astronomı́a, Venezuela [email protected] Brenda Eliana MELENDEZ, Facultad de Ciencias Astronómicas y Geofı́sicas, Universidad Nacional de La Plata (UNLP), Instituto de Astrofı́sica de la Plata, UNLP-CONICET, Argentina [email protected] Claudio MELIOLI, IAG-USP, Brazil [email protected] Alexandre Tuoto MELLO, Universidade Federal de Santa Catarina, Brazil [email protected] Claudio MELO, ESO/Chile, Chile [email protected] Paulo Henrique Guimarães MELQUIADES, Grupo de Astronomia e Astrofı́sica(GAIA). Museu de Ciência Naturais. Pontifı́cia Universidade Católica de Minas Gerais., Brazil [email protected] Luiz Themystokliz Sanctos MENDES, Universidade Federal de Minas Gerais, Brazil [email protected] Sandro MENDOZA-CASTREJÓN, Instituto de Astronomı́a, Universidad Nacional Autónoma de México., Mexico [email protected] Karin MENENDEZ-DELMESTRE, Valongo Observatory, Federal University of Rio de Janeiro, Brazil [email protected] Roberto Bertoldo MENEZES, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo , Brazil [email protected] Adal MESA-DELGADO, Pontificia Universidad Católica de Chile, Chile [email protected] Hugo G. MESSIAS, Universidad de Concepcion, Chile [email protected] Steffen MIESKE, European Southern Observatory, Chile, Chile [email protected] Andre de Castro MILONE, Instituto Nacional de Pesquisas Espaciais (INPE/MCTI), Brazil [email protected] Dante MINNITI, Instituto de Astrofisica, Pontificia Universidad Catolica de Chile, Chile [email protected] Felix Igor MIRABEL, Instituto de Astronomia y Fisica del Espacio. Conicet-UBA, Argentina [email protected] Dayvid de Sousa Miranda Sousa MIRANDA, Universidade Estadual do Rio Grande do Norte, Brazil [email protected] Mercedes MOLLA, IAG, Universidade de Sao Paulo and CIEMAT(Madrid, Spain), Brazil [email protected] Thiago MONFREDINI, Universidade Federal do Rio de Janeiro, Brazil [email protected] xxix Christian MONI BIDIN, Universidad Catolica del Norte, Chile [email protected] Hektor MONTEIRO, Universidade Federal de Itajubá, Brazil [email protected] Felipe Antonio MONTEIRO GOMES NOGUEIRA, Observatório do Valongo - Universidade Federal do Rio de Janeiro, Brazil [email protected] Thierry MONTMERLE, Institut d’Astrophysique de Paris, France [email protected] Habib Salomon Dumet MONTOYA, CENTRO BRASILEIRO DE PESQUISAS FISICAS, Brazil [email protected] Marcelo D. MORA, Instituto de Astrofı́sica, Pontificia Universidad Católica de Chile, Chile [email protected] Bruno MORAES, Centro Brasileiro de Pesquisas Fı́sicas, Brazil [email protected] Christophe MORISSET, Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Mexico [email protected] Juliana Cristina MOTTER, Universidade de São Paulo, Brazil [email protected] Décio Cardozo MOURÃO, UNESP - Univ. Estadual Paulista, Brazil [email protected] Maximiliano Leonardo MOYANO DANGELO, Universidad Católica del Norte, Chile [email protected] Francisco MUELLER-SANCHEZ, UCLA, United States [email protected] César Alejandro MUÑOZ, Universidad de Concepción, Concepción, Chile, Chile [email protected] Alejandra Marı́a MUÑOZ ARANCIBIA, Pontificia Universidad Católica de Chile, Chile [email protected] Juan Carlos MUÑOZ CUARTAS, Instituto de Fisica, Universidad de Antioquia, Colombia [email protected] Deisy Lorena MUÑOZ SERNA, Fundación Universitaria Luis Amigó, Colombia [email protected] Koraljka MUZIC, European Southern Observatory (ESO), Chile, Chile [email protected] Orlando Antonio NARANJO, Universidad de Los Andes. Grupo de Astrofı́sica Teórica. Mérida. Venezuela., Venezuela [email protected] John Alexander NARVAEZ, Universidad Nacional de Colombia, Colombia [email protected] Raquel Santiago NASCIMENTO, Observatório do Valongo/ Universidade Federal do Rio de Janeiro, Brazil [email protected] xxx Felipe NAVARETE, Universidade de São Paulo, Brazil [email protected] Camila NAVARRETE, Pontificia Universidad Catolica de Chile, Chile [email protected] Giuliat NAVAS, Centro de Investigaciones de Astronomia ”Francisco José Duarte” (CIDA) , Venezuela [email protected] Daniel Marcos NERI-LARIOS, The University of Melbourne, Australia [email protected] Oswaldo NIETO, Escuela de Fı́sica, Universidad Industrial de Santander, Colombia [email protected] Robert NIKUTTA, Universidad Andres Bello, Chile [email protected] Jose Luis NILO CASTELLON, Universidad de La Serena, Chile [email protected] Erica Cristina NOGUEIRA, Universidade Federal Fluminense, Observatório Nacional, Brazil [email protected] Patricia Martins de NOVAIS, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas - IAG/USP, Brazil [email protected] Rafael da Costa NUNES, Universidade Estudual do Rio Grande do Norte, Brazil [email protected] Mónica Alejandra ODDONE, Observatorio Astronómico Córdoba, Universidad Nacional de Córdoba, Argentina [email protected] Gabriel Andrés OIO, Instituto de Astronomı́a Teórica y Experimental (IATE), Argentina [email protected] Paola Cecilia OLIVA-ALTAMIRANO, Swinburne University of Technology/ Australian Astronomical Observatory (AAO), Honduras [email protected] Felipe OLIVARES E., Physics Department, Universidad Andrés Bello, Chile [email protected] Alexandre Soares OLIVEIRA, IP&D-Univap, Brazil [email protected] Carolyne Santos OLIVEIRA, Valongo Observatory at the Federal University of Rio de Janeiro, Brazil [email protected] Murilo Marinello Assis OLIVEIRA, Universidade Federal de Itajubá., Brazil [email protected] Alcides ORTEGA, Dirección de Informática Universidad de Carabobo , Venezuela [email protected] René Alberto ORTEGA-MINAKATA, Departamento de Astronomı́a, Universidad de Guanajuato, Mexico, Mexico [email protected] Roberto ORTIZ, Universidade de São Paulo, Brazil [email protected] xxxi Luis Javier OTINIANO, CONIDA (Comisión Nacional de Investigación y Desarrollo Aeroespacial), Peru [email protected] Tania PAEZ TAGLIAFERRO, Universidad Nacional del Córdoba, Argentina [email protected] Leonardo Gaston PAIZ, Facultad de Ciencias Astronomicas y Geofisicas - Universidad Nacional de La Plata, Argentina [email protected] Tali PALMA, Observatorio Astronómico, Universidad Nacional de Córdoba, Argentina [email protected] Miriani Griselda PASTORIZA, Universidade Federal de Rio Grande do Sul, Brazil [email protected] Diogo PAULETTI, Universidade Federal de Santa Maria, Brazil [email protected] Manuel PEIMBERT, Universidad Nacional Autonoma de Mexico, Instituto de Astronomia, Mexico [email protected] Ana PELINSON, UFSC, Brazil [email protected] Miriam PEÑA, Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Mexico [email protected] Paulo F. PENTEADO, Northern Arizona University, United States [email protected] Maria Elidaiana da Silva PEREIRA, Centro Brasileiro de Pesquisas Fı́sicas, Brazil [email protected] Margarita PEREYRA, Insituto de Astronomı́a de la Universidad Nacional Autónoma de México, Mexico [email protected] Alice Gabriela PÉREZ BLANCO , Centro de Investigaciones de Astronomı́a ”Francisco J. Duarte” (CIDA), , Venezuela [email protected] Angeles PEREZ-VILLEGAS, Centro de Radioastronomia y Astrofisica, UNAM, Mexico [email protected] Romina Paola PETRUCCI, Instituto de Astronomia y Fisica del Espacio (IAFE), Argentina [email protected] Barbara PICHARDO, Instituto de Astronomı́a, Universidad Nacional Autónoma de México (IA-UNAM), Mexico [email protected] Giuliano PIGNATA, Universidad Andrès Bello, Chile [email protected] Marcio do Carmo PINHEIRO, Universidade Federal da Fronteira Sul, Brazil [email protected] Rafael PINOTTI, Observatório do Valongo - Universidade Federal do Rio de Janeiro - UFRJ, Brazil [email protected] Olga PINTADO, INSUGEO-CONICET, Argentina [email protected] xxxii Nelson PINTO-NETO, Centro Brasileiro de Pesquisas Fı́sicas, Brazil [email protected] Giovanni PINZON, Universidad Nacional de Colombia, Colombia [email protected] Priscilla Firmino POLIDO, Instituto Nacional de Pesquisas Espaciais, Brazil [email protected] Bogdan POPESCU, University of Cincinnati, USA, United States [email protected] Gustavo Frederico PORTO DE MELLO, Observatório do Valongo/Universidade Federal do Rio de Janeiro, Brazil [email protected] Ivanio PUERARI, INAOE, Mexico [email protected] Thomas H. PUZIA, Institute of Astrophysics, Pontificia Universidad Catolica, Chile [email protected] Carolina QUEIROZ DE ABREU SILVA, Universidade de São Paulo, Brazil [email protected] Bruno Correa QUINT, Universidade de São Paulo, Brazil [email protected] Seditsira Andrea QUINTERO VILLAMIZAR, Universidad Nacional de Colombia-Sede Bogotá, Colombia [email protected] Jonathan Alexander QUIROLA, Escuela Politécnica Nacional. Quito-Ecuador., Ecuador [email protected] Edgar Andre RAMIREZ ALONSO, IAG-USP, Brazil [email protected] Liz Angélica RAMOS MEDINA, Universidad Distrital Francisco Jose de Caldas, Colombia [email protected] Andres Felipe RAMOS PADILLA, Department of Physics, National University of Colombia. , Colombia [email protected] Aline Beatriz RAUBER, Universidade Federal de Santa Maria, Brazil [email protected] Henrique Marques REGGIANI, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas (IAG)-Universidade de São Paulo (USP), Brazil [email protected] Marı́a Camila REMOLINA GUTIÉRREZ, Universidad de los Andes, Colombia [email protected] Paolo Scarsi REPETTO, Laboratorio Nacional de Astrofisica, Brazil [email protected] Felipe Braga RIBAS, Observatório Nacional / MCTI, Brazil [email protected] Anderson de Oliveira RIBEIRO, Observatório Nacional, Brazil [email protected] xxxiii Brunno Augusto Gomes RIBEIRO, Pontificia universidade catolica de minas gerais, museu de ciencias naturais, GAIA, Brazil [email protected] Evandro Martinez RIBEIRO, Observatório Nacional, Brazil [email protected] Filipe Batista RIBEIRO, UNESP - Rio Claro, Brazil [email protected] Nadili Louise RIBEIRO, Universidade de São Paulo, Brazil [email protected] Tiago RIBEIRO, Universidade Federal de Sergipe, Brazil [email protected] Tiago Vecchi RICCI, IAG - Universidade de São Paulo, Brazil [email protected] Rogemar A. RIFFEL, Universidade Federal de Santa Maria, Brazil [email protected] Rogerio RIFFEL, Universidade Federal do Rio Grande do Sul, Brazil [email protected] Leandro Rocha RÍMULO, Universidade de São Paulo, Brazil [email protected] Angel Erasmo RINCON, Universidad de Chile, Chile [email protected] Gustavo ROCHA DA SILVA, Universidade de São Paulo, Brazil [email protected] Javier A. RODÓN, European Southern Observatory, Chile [email protected] Bárbara H. G. RODRIGUES, Instituto Nacional de Pesquisas Espaciais (INPE), Brazil [email protected] Claudia Vilega RODRIGUES, INSTITUTO NACIONAL DE PESQUISAS ESPACIAIS, Brazil [email protected] Fábio Pinto RODRIGUES, Universidade Federal de Itajubá (UNIFEI), Brazil [email protected] Teresinha RODRIGUES, Observatório Nacional, Brazil [email protected] Irapuan RODRIGUES DE OLIVEIRA FILHO, Universidade do Vale do Paraı́ba, Brazil [email protected] Ana Maria RODRIGUEZ, Universidad Nacional de Colombia, Colombia [email protected] David RODRIGUEZ, Universidad de Chile, Chile [email protected] Facundo RODRIGUEZ, Instituto de Astronomı́a Teórica y Experimental- Universidad Nacional de Córdoba - CONICET, Argentina [email protected] xxxiv Monica RODRIGUEZ, Instituto Nacional de Astrofisica, Optica y Electronica (INAOE), Mexico [email protected] Christian David RODRÍGUEZ CAMARGO, Physics Department, National University of Colombia, Colombia [email protected] Alberto RODRIGUEZ-ARDILA, Laboratório Nacional de Astrofı́sica, Brazil [email protected] Fernando ROIG, Observatório Nacional, Brazil [email protected] Alejandra ROJAS, Pontificia Universidad Católica de Chile, Chile [email protected] Gustavo de Araujo ROJAS, Universidade Federal de São Carlos, Brazil [email protected] Karina Alexandra ROJAS, Departamento de Fı́sica y Astronomı́a, Universidad de Valparaı́so, Chile [email protected] Carlos Gerardo ROMÁN-ZÚÑIGA, Instituto de Astronomı́a, Unidad Académica en Ensenada, Universidad Nacional Autónoma de México, Mexico [email protected] Alessio D. ROMEO, INAF, Italy, Italy [email protected] Alejandra Daniela ROMERO, Instituto de Fı́sica, UFRGS, Brazil [email protected] Julia Maria Torres ROQUETTE, Universidade Federal de Minas Gerais, Brazil [email protected] Deise Aparecida ROSA, Universidade do Vale do Paraı́ba- Univap, Brazil [email protected] Fernando Fabián ROSALES-ORTEGA, Instituto Nacional de Astrofı́sica, Óptica y Electrónica, Mexico [email protected] Marcelo Soares RUBINHO, Instituto de Astronomia, Geociência e Ciências Atmosféricas, Brazil [email protected] Beatriz Eugenia SABOGAL MARTÍNEZ, Universidad de los Andes, Bogotá, Colombia [email protected] Roberto SAITO, Universidade Federal de Sergipe, Brazil [email protected] Pedro SALAS, Instituto de Astrofı́sica, Facultad de Fı́sica, P. Universidad Católica de Chile, Chile [email protected] Andrea Sanchez SALDIAS, Departamento de Astronomia - Facultad de Ciencias - Universidad de la República, Uruguay [email protected] Dinalva A. SALES, Rochester Institute of Technology, United States [email protected] João Victor SALES SILVA, Observatório Nacional, Brazil [email protected] xxxv Jorge Enrique SAMANES, Comisión Nacional de Investigación y Desarrollo Aeroespacial (CONIDA), Peru [email protected] Astrid Elizabeth SAN MARTIN, Universidad Andres Bello, Chile [email protected] Paula Andrea SÁNCHEZ, Universidad de Chile, Chile [email protected] Hillysson Bruno SANTOS, Universidade Estadual do Rio Grande do Norte, Brazil [email protected] Jéssica Pereira SANTOS, Universidade Federal de Sergipe, Brazil [email protected] Jullian Henrique Barbosa SANTOS, Universidade de São Paulo (USP), Brazil [email protected] Patricia SANTOS, Universidade Federal de Itajubá, Brazil [email protected] Rafael Gonzaga SANTOS , NAT - Universidade Cruzeiro do Sul, Brasil, Brazil [email protected] Reinaldo SANTOS DE LIMA, Instituto de Astronomia, Geofı́sica e C. Atmosféricas - Universidade de São Paulo, Brazil [email protected] Joao Francisco Coelho SANTOS JR., Universidade Federal de Minas Gerais, Brazil [email protected] Erick Rohan SANTOS OLIVEIRA MAGALHAES, Universidade Estadual de Santa Cruz, Brazil [email protected] Marı́a Victoria SANTUCHO, Instituto de Astronomı́a Téorico y Experimental (IATE-CONICET). , Argentina [email protected] Maria de Fátima Oliveira SARAIVA , Universidade Federal do Rio Grande do Sul, Brazil [email protected] Christian Andres SARMIENTO CANO , Universidad Industrial de Santander, Colombia [email protected] Tiago Abreu SAURIN, Universidade Federal do Rio Grande do Sul, Instituto de Fı́sica, Departamento de Astronomia, Brazil [email protected] Jaderson Silva SCHIMOIA, Universidade Federal de Santa Maria, Brazil [email protected] Mischa SCHIRMER, Gemini Observatory, Chile [email protected] Marielli de Souza SCHLICKMANN, Universidade Federal de Santa Catarina, Brazil [email protected] Wagner SCHLINDWEIN, Universidade Federal de Santa Catarina, Brazil [email protected] William SCHOENELL, Instituto de Astrofı́sica de Andalucı́a - CSIC, Spain [email protected] xxxvi Matthias R. SCHREIBER, Universidad de Valparaiso, Departamento de Fisica y Astronomia, Chile, Chile [email protected] Steve SCHULZE, Pontificia Universidad Católica de Chile , Chile [email protected] Daiane Breves SERIACOPI, Universidade de São Paulo, Brazil [email protected] Diah SETIA GUNAWAN, Joint ALMA Office, Santiago, Chile, Chile [email protected] Mario Agustı́n SGRÓ, Instituto de Astronomı́a Teórica y Experimental - UNC - CONICET, Argentina [email protected] Costantino SIGISMONDI, Observatório Nacional/MCTI & ICRANet/Sapienza Universitá di Roma and Ateneo Pontificio Regina Apostolorum, Italy [email protected] André Rodrigo da SILVA, Universidade Federal de São Paulo, Brazil [email protected] Gabriel Gonçalves SILVA, Universidade Federal de São Carlos, Brazil [email protected] José Ronaldo Pereira da SILVA, Universidade do Estado do Rio Grande do Norte, Brazil [email protected] Karleyne SILVA, Instituto Nacional de Pesquisas Espaciais, INPE, Brazil [email protected] Raquel Boesso SILVA, Observatório do Valongo - Universidade Federal do Rio de Janeiro, Brazil [email protected] Thais Santos SILVA, Universidade de São Paulo, Brazil [email protected] Vinicius Branco SILVA, Universidade de São Paulo, Brazil [email protected] José Sergio SILVA CABRERA, Observatório Nacional, Brazil [email protected] Carlos Roberto SILVEIRA, Universidade de São Paulo, Brazil [email protected] Marcelo Kenji SIME, Universidade de São Paulo, Brazil [email protected] Mirko SIMUNOVIC, Pontificia Universidad Catolica de Chile, Chile [email protected] Anna SIPPEL, ESO Santiago / Swinburne University, Australia, Chile [email protected] Marcos Felipe Faria Terra SIQUEIRA, Universidade Federal de Itajubá, Brazil [email protected] Cesar SIQUEIRA MELLO, IAG - Universidade de São Paulo, Brazil [email protected] xxxvii Camila Maria SITKO, Universidade Estadual de Londrina (UEL), Brazil [email protected] Rodolfo SMILJANIC, Nicolaus Copernicus Astronomical Center, Poland [email protected] Braulio Batista SOARES, Universidade do Estado do Rio Grande do Norte, Brazil [email protected] Laerte SODRE , USP - Instituto de Astronomia, Geofisica e Ciências Atmosfericas, Brazil [email protected] Piera Andrea SOTO KING, Universidad de La Serena, Chile [email protected] Alana Paixão de SOUSA, Universida Federal de Minas Gerais, Brazil [email protected] Diogo Martins SOUTO, Observatorio Nacional - MCT, Brazil [email protected] Julio César SPAGNOTTO, Universidad Nacional de La Pampa, Argentina [email protected] Patricia Figueiró SPINELLI, Museu de Astronomia e Ciências Afins (MAST), Brazil [email protected] Grazyna STASINSKA, Observatoire de Paris, France [email protected] Katrien Christine STEENBRUGGE, Instituto de Astronomia, Universidad Catolica del Norte & Department of Physics, University of Oxford, Chile [email protected] João E. STEINER, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas - USP, Brazil [email protected] Thaisa STORCHI-BERGMANN, Instituto de Fı́sica, Universidade Federal do Rio Grande do Sul, Brazil [email protected] Laura Andrea SUAD, Instituto Argentino de Radioastronomı́a (IAR)., Argentina [email protected] Edilberto SUAREZ TORRES, Universidad Distrital ”Francisco José de Caldas”, Facultad de Ingenierı́a, Colombia [email protected] Katalin TAKATS, Universidad Andres Bello, Chile [email protected] Gonzalo TANCREDI, Depto. Astronomia, Fac. Ciencias, Uruguay [email protected] Eduardo TELLES, Observatorio Nacional, Brazil [email protected] Ramachrisna TEXEIRA, IAG-USP, Brazil [email protected] Patricia B. TISSERA, Institute for Astronomy and Space Physics, Argentina [email protected] xxxviii Laura TORIBIO SAN CIPRIANO, Instituto de Astrofı́sica de Canarias, Spain [email protected] Carlos Alberto O. TORRES, Laboratório Nacional de Astrofı́sica (LNA/MCTI), Brazil [email protected] Andres David TORRES CAÑAS , National University of Colombia. Physics School. Sciences Faculty, Natural Sciences Museum of La Salle. A project of ITM. Astronomical Observatory, Colombia [email protected] Juanita TORRES ZAFRA, Instituto de Astrofı́sica de La Plata, Argentina [email protected] Sergio TORRES-FLORES, Universidad de La Serena, Chile [email protected] Silvia TORRES-PEIMBERT, UNIVERSIDAD NACIONAL AUTONOMA DE MEXICO, Mexico [email protected] Josué de Jesús TREJO-ALONSO, Universidad de Guanajuato, Mexico [email protected] Amy Alexandra TYNDALL, ESO, Chile / JBCA, UK, Chile [email protected] Fernanda URRUTIA, universidade de sao paulo, Brazil [email protected] Bruna VAJGEL, Observatorio do Valongo, Universidade Federal do Rio de Janeiro, Brazil [email protected] Natalia VALE ASARI, Universidade Federal de Santa Catarina, Brazil [email protected] Adriana VALIO, CRAAM, Universidade Presbiteriana Mackenzie, Brazil [email protected] David VALLS-GABAUD, Observatoire de Paris, France [email protected] Maria Eugenia VARELA, Instituto de Ciencias Astronomicas de la Tierra y del Espacio (ICATE), Argentina [email protected] Santiago VARGAS DOMÍNGUEZ, Universidad de los Andes, Colombia [email protected] Javier VASQUEZ, Instituto Argentino de Radioastronomı́a, Argentina, Argentina [email protected] Sebastian VELASCO, Universidad de los Andes, Colombia [email protected] Román Rodrigo VENA VALDARENAS, Instituto de Astronomı́a Teórica y Experimental, Argentina [email protected] Rafael Jonathan Camilo VERA, Universidad Nacional de Colombia, Colombia [email protected] Celia Anahi VERDUGO, Observatoire de Paris, France [email protected] xxxix Mariela Cristina VIEYTES, Universidad de Tres de Febrero, Instituto de Astronomı́a y Fı́sica del Espacio, Argentina [email protected] Carolina Susana VILLARREAL D’ANGELO, Instituto de Astronomı́a Teórica y Experimental (IATE), Argentina [email protected] Marcos Rincon VOELZKE, Universidade Cruzeiro do Sul, Brazil [email protected] Zhong WANG, Chinese Academy of Sciences South America Center for Astronomy (CASSACA), Chile [email protected] Ariel WERLE, Universidade Federal de Santa Catarina, Brazil [email protected] Othon Cabo WINTER, Universidade Estadual Paulista - UNESP, Brazil [email protected] Eduardo Luann WOJCIKIEWICZ, Universidade Federal de Santa Catarina, Brazil [email protected] Henrique Scemes XAVIER, Instituto de Fı́sica da Universidade de São Paulo (IFUSP), Brazil [email protected] Jincheng YU, Pontificia Universidad Católica de Chile, Chile [email protected] Alessandra ZANAZZI, INAF - Osservatorio Astrofisico di Arcetri, Italy [email protected] Luis A. ZAPATA, Centro de Radioastronomia y Astrofisica, UNAM, Mexico [email protected] Libardo ZERPA, Centro de Investigaciones de Astronomia ”Francisco José Duarte” (CIDA) y Universidad de Los Andes (ULA), Venezuela [email protected] Hans ZINNECKER, SOFIA Science Center, NASA-Ames, United States [email protected] Manuela ZOCCALI, Pontificia Universidad Catolica de Chile, Chile [email protected] xl Review & Invited Talks 1 Distribution and Origin of Hot Planets C. BeaugeB1 Close-in (or Hot) planets, usually defined as those having semimajor axes a < 0.1 AU (or orbital periods P < 10 days), are the easiest to detect, both with radial velocity (RV) surveys and transits. More than 300 members are currently known, and a much larger number of candidates has been proposed by the Kepler team. Since it is believed that these bodies cannot have been formed in-situ, they constitute an interesting population from which to derive information about orbital migration and dynamical evolution of planetary systems in general. In this talk we review some recent results on the dynamical characteristics of close-in planets, including the existence of both resonant and near-resonant configurations, planet multiplicity, eccentricity distribution and inclinations with respect to the stellar equator. We discuss how disk-induced migration, planet-planet scattering and tidal effects may help us explain several of these dynamical traits, although others are still poorly understood. Finally, we analyze the similarities and differences found in small (Earth to Neptune) and large (Jovian) size planets, and how these may reflect different evolutionary histories. B 1 [email protected] Instituto de Astronomia Teorica y Experimental, Observatorio Astronomico, Universidad Nacional de Cordoba, Argentina Planetary systems Review & Invited Talks Impact studies in Latin America Gonzalo TancrediB1 The research about impact process of extraterrestrial bodies onto the Earth is a new subject in only a few institutes in Latin America. A proof of that is the scarcity of recognized impact structures in the region. Nevertheless, we have among the most interesting features on Earth, like the crater strewn fields of Campo del Cielo (Chaco, Argentina) and Bajada del Diablo (Neuquén, Argentina); and the recently formed small crater of Carancas (Perú). These cases have questioned several ideas about the nature of the impacting objects: monolithic vs. agglomerate; as well as the survival of the objects in the passage through the atmosphere. These questions have important implications regarding the plans to deflect a threatening asteroid and the risk and consequences of small impactors. A few groups in the region have been involved in field research in those craters, as well as experimental and theoretical studies about impact processes and deflection mechanisms. We will highlight the most relevant results on this growing scientific field. B 1 [email protected] Depto. Astronomia, Fac. Ciencias, Montevideo, URUGUAY 4 Review & Invited Talks Teaching and outreach A New Chinese Astronomy Center in Chile Wang, Z.B1,2,3 ; Huang, J.-S.1,2,3 As part of a new initiative launched by the Chinese Academy of Sciences (CAS) to expand its collaboration with the rest of the world, a CAS South America Center for Astronomy (CASSACA, also known as China-Chile Joint Center for Astronomy) has recently been established in Santiago, Chile. I will introduce the central mission of this Center, and discuss the prospect of supporting collaborative research between Chinese astronomers and their Latin American colleagues. B 1 2 2 [email protected] Chinese Academy of Science’s South American Center for Astronomy National Astronomical Observatories, Chinese Academy of Sciences Harvard-Smithsonian Center for Astrophysics 5 Stars Review & Invited Talks Supergiants, Stellar Winds and Mass-loss Cidale, L.B1,2 The knowledge of the wind properties and the mass loss rate in massive stars is a milestone in the stellar evolution and the chemical composition of the interestellar medium. Our current view of stellar winds reveals they are often highly variable and inhomogeneous. We review here the wind structure of early-type stars (the wind clumping and the weak-wind problems) and the peculiar circumstellar environment around some short-lived phases of evolved massive stars (i.e.: LBVs and B[e] supergiants). Accurate mass loss rate estimates are crucial keys to discuss the importance of different triggering mechanisms in driving the wind. B 1 2 [email protected] Instituto de Astrofı́sica La Plata Facultad de Ciencias Astronómicas y Geofı́sicas, Universidad de La Plata 6 Review & Invited Talks ISM Abundance determinations in ionized nebulae and their sensitivity to temperature Rodriguez, M.B1 ; Manso-Sainz, R.2 Our main source of uncertainty in the determination of chemical abundances in H II regions and planetary nebulae arises from a discrepancy: the abundances implied by recombination lines are larger than those implied by collisionally excited lines. Most objects show a factor of 2 discrepancy, but some planetary nebulae display much higher discrepancies. I will discuss the possible explanations of this effect, focusing on the latest: I will describe what kind of deviations from a Maxwellian electron energy distribution are needed in order to reproduce the measured abundance discrepancies. I will explore the parallelisms between the three explanations of the discrepancy that are based on the sensitivity to temperature of collisionally excited lines, namely, deviations from a Maxwellian energy distribution, temperature fluctuations, and the presence of metal-rich inclusions. I will show some evidence that at least one of these mechanisms is acting in H II regions. B 1 2 [email protected] Instituto Nacional de Astrofisica, Optica y Electronica (INAOE) Instituto de Astrofisica de Canarias (IAC) 7 Stars Review & Invited Talks Solar Transient Activity: Magnetic Energy Release and Topology Mandrini, C. H.B1 The energy released during transient atmospheric events in the Sun is contained in current-carrying magnetic fields that have emerged after traversing the solar convective zone. Once the magnetic flux reaches the photosphere, it may be further stressed via motions in this lower atmospheric layer. Magnetic field reconnection is thought to be the mechanism through which the stored magnetic energy is transformed into kinetic energy of accelerated particles and mass flows, and radiative energy along the whole electromagnetic spectrum. Though this mechanism is efficient only at very small spatial scales, it may imply a large-scale restructuring of the magnetic field which is inferred from the combined analysis of observations, models of the coronal magnetic field, and computation of its topology. The consequences of energy release include events that range from nano-flares, still below our present observational spatial resolution, to powerful flares that may be accompanied by the ejection of large amounts of plasma and magnetic field in events called coronal mass ejections (CMEs). We will review key observational signatures of flares and CMEs on the Sun and discuss how the computation and analysis of the magnetic field topology, applied to the widest variety of observed magnetic configurations, can be used to identify the energy release locations and their physical characteristics. B 1 [email protected] Instituto de Astronomı́a y Fı́sica del Espacio, IAFE 8 Review & Invited Talks Planetary systems The SNC Meteorites Varela, M. E.B1 The SNC (Shergotty-Nakhla-Chassigny) group, are achondritic meteorites. Of all SNC meteorites recognized up to date, shergottites are the most abundant group. The petrographic study of Shergotty began several years ago when Tschermak, (1872) identified this rock as an extraterrestrial basalt. Oxygen isotopes in SNC meteorites indicate that these rocks are from a single planetary body (Clayton and Mayeda, 1983). Because the abundance patterns of rare gases trapped in glasses from shock melts (e.g., Pepin, 1985) turned out to be very similar to the Martian atmosphere (as analyzed by the Viking landers, Owen, 1976), the SNC meteorites are believed to originate from Mars (e.g. McSween, 1994). Possibly, they were ejected from the Martian surface either in a giant impact or in several impact events (Meyer 2006). Although there is a broad consensus for nakhlites and chassignites being -1.3Ga old, the age of the shergottites is a matter of ongoing debates. Different lines of evidences indicate that these rocks are young (180Ma and 330-475Ma), or very old (> 4Ga). However, the young age in shergottites could be the result of a resetting of these chronometers by either strong impacts or fluid percolation on these rocks (Bouvier et al., 2005-2009). Thus, it is important to check the presence of secondary processes, such as re-equilibration or pressure-induce metamorphism (El Goresy et al., 2013) that can produce major changes in compositions and obscure the primary information. A useful tool, that is used to reconstruct the condition prevailing during the formation of early phases or the secondary processes to which the rock was exposed, is the study of glass-bearing inclusions hosted by different mineral phases. I will discuss the identification of extreme compositional variations in many of these inclusions (Varela et al 2007-2013) that constrain the assumption that these objects are the result of closed-system crystallization. The question then arises whether these inclusions can be considered reliable samples of the fluid/melt that was originally trapped. B 1 [email protected] Instituto de Ciencias Astronómica de la Tierra y del Espacio (ICATE) 9 Instrumentation Review & Invited Talks New Opportunities with the Gemini Observatory M. BoccasB1 Gemini Observatory’s associate director for development Maxime Boccas will present an update of the facility and introduce some new opportunities for astronomers at Gemini. Gemini operates twin 8-m telescopes, one in Hawaii and the other in Chile. The departure of the UK from Gemini’s international partnership at the end of 2012 provided the chance to re-evaluate the services offered to Gemini users and opened new opportunities in two domains. First, Gemini will welcome discussions with groups wanting to bring their own instruments for campaigns. This visiting instrument program will complement the suite of workhorse instruments offered by the Observatory, and will allow scientific breakthroughs not possible with the regular suite of instruments. Second, the Gemini observatory will be offering cross-partnership large or long programs. From 2014 on, Gemini will be dedicating 20collaborative programs selected through a yearly call. Gemini is also looking at the possibility of offering some fraction of time in a fast turn-around mode, as well as ”eavesdropping” for queue observing. We remain very interested in having astronomers visit the telescopes. In addition to these two major initiatives, several new instruments have appeared in 2013: Flamingos-2 and the Gemini Multi-conjugate adaptive optics System (GeMS) are being offered for science, and the Gemini Planet Imager (GPI) has arrived on Cerro Pachon. B 1 [email protected] Gemini Observatory 10 Review & Invited Talks AGN Active Galactic Nuclei Arévalo, P.B1 Accreting supermassive black holes have had a large impact in the evolution of their host galaxies, and even inject significant energy into their host cluster of galaxies. Although the black hole’s influence in these large structures is evident, the central engine itself is remarkably difficult to observe. Their extremely compact nature makes it impossible to resolve the final source of fueling, the accretion disc, although interferometric observations have started to reveal important details of the material directly outside this region. In this talk I will review the techniques that have shed light into the structure and behavior of these central engines in the quest to find out how black hole grow. B 1 [email protected] Pontificia Universidad Católica, Chile 11 Star formation Review & Invited Talks Diversity of protoplanetary disks in stellar clusters: the case of the sigma Orionis cluster Hernández J.B1 ; Calvet N.2 ; Mauco K.2 ; Ballesteros J.4 ; Perez A.1 ; Briceño C.1 ; Hartmann L.2 ; Olguin L.3 ; Contreras M.4 ; Allen L.5 ; Espaillat C.6 The Orionis cluster is a natural laboratory to study stars and protoplanetary disks in the first stages of their evolution. This cluster is relatively near (Distance ⇠400 pc) and the extinction is low (AV < ⇠ 0.5 mag) and thus enable us to study young stars in a entire range of masses, from its most massive star (O9.5 type star) to the lowest mass objects, such as brown dwarfs and free-floating planets. Recently, we have obtained the largest and most homogeneous spectroscopic characterization to date of stars belong to this cluster. This information is a corner stone to derive stellar parameter. Of particular interest are stars that exhibit infrared excesses produced by protoplanetary disks. Since the Orionis cluster has an evolutionary stage in which mechanisms of disk dispersal have affected substantially its disk population, we observe large diversity of disks in this stellar cluster (e.g.,optically thick full disks, pre-transitional disks, transitional disks, homogeneusly depleted disks and debris disks). More than 100 stars bearing protoplanetary disks have been detected in the Orionis cluster with the disk census presented few years ago using IRAC and MIPS observations. In this contribution, we present an overview of the latest results of an ongoing study of the disk population in the Orionis cluster combining Hershel-PACS observation, IRS spectroscopic data for selected targets and theoretical models of disk evolution. In order to get a better understand of how disk evolves from optically thick full disks to debris disks, these results will be combined with similar studies that we are doing in more dispersed and older regions of the Orion OB1a and OB1b sub association. B 1 2 3 4 5 6 [email protected] Centro de Investigaciones de Astronomı́a, Mérida, Venezuela Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, US Depto. de Investigación en Fı́sica, Universidad de Sonora, Sonora, México Instituto de Astronomı́a, Universidad Nacional Autónoma de México, Ensenada, BC, México NOAO, US Harvard-Smithsonian Center for Astrophysics, US 12 Review & Invited Talks Stars White Dwarf Stars S. O. KeplerB1 White dwarfs are the evolutionary endpoint for nearly 95% of all stars born in our Galaxy, the final stages of evolution of all low- and intermediate mass stars, i.e., main sequence stars with masses below (8.5 ± 1.5) M , depending on metallicity of the progenitor, mass loss and core overshoot. Massive white dwarfs are intrinsically rare objects, tand produce a gap in the determination of the initial vs. final mass relation at the high mass end (e.g. Weidemann 2000 A&A, 363, 647; Kalirai et al. 2008, ApJ, 676, 594; Williams, Bolte & Koester 2009, ApJ, 693, 355). Main sequences stars with higher masses will explode as SNII (Smartt S. 2009 ARA&A, 47, 63), but the limit does depend on the metallicity of the progenitor. Massive white dwarfs are probably SNIa progenitors through accretion or merger. They are rare, being the final product of massive stars (less common) and have smaller radius (less luminous). Kepler et al. 2007 (MNRAS, 375, 1315), Kleinman et al. 2013 (ApJS, 204, 5) estimate only 1-2% white dwarfs have masses above 1 M . The final stages of evolution after helium burning are a race between core growth and loss of the H-rich envelope in a stellar wind. When the burning shell is exposed, the star rapidly cools and burning ceases, leaving a white dwarf. As they cool down, the magnetic field freezes in, ranging from a few kilogauss to a gigagauss. Peculiar type Ia SN 2006gz, SN 2007if, SN 2009dc, SN 2003fg suggest progenitors in the range 2.4 2.8 M , and Das U. & Mukhopadhyay B. (2012, Phys. Rev. D, 86, 042001) estimate that the Chandrasekhar limit increases to 2.3 2.6 M for extremely high magnetic field stars, but differential rotation induced by accretion could also increase it, according to Hachisu I. et al. 2012 (ApJ, 744, 69). Garcı́a-Berro et al. 2012, ApJ, 749, 25, for example, proposes double degenerate mergers are the progenitors of high-field magnetic white dwarfs. We propose magnetic fields enhance the line broadening in WDs, causing an overestimated surface gravity, and ultimately determine if these magnetic fields are likely developed through the star’s own surface convection zone, or inherited from massive Ap/Bp progenitors. We discovered around 20 000 spectroscopic white dwarfs with the Sloan Digital Sky Survey (SDSS), with a corresponding increase in relatively rare varieties of white dwarfs, including the massive ones (Kleinman et al. 2013, ApJS, 204, 5, Kepler et al. 2013, MNRAS, 439, 2934). The mass distributions of the hydrogen-rich (DA) measured from fitting the spectra with model atmospheres calculated using unidimensinal mixing lenght-theory (MLT) shows the average mass (as measured by the surface gravity) increases apparently below 13 000K for DAs (e.g. Bergeron et al. 1991, ApJ, 367, 253; Tremblay et al. 2011, ApJ, 730, 128; Kleinman et al. 2013). Only with the tridimensional (3D) convection calculations of Tremblay et al. 2011 (A&A, 531, L19) and 2013 (A&A, 552, 13; A&A, 557, 7; arXiv 1309.0886) the problem has finally been solved, but the effects of magnetic fields are not included yet in the mass determinations. Pulsating white dwarf stars are used to measure their interior and envelope properties through seismology, and together with the luminosity function of white dwarf stars in clusters and around the Sun are valuable tools for the study of high density physics, and the history of stellar formation. B 1 [email protected] Universidade Federal do Rio Grande do Sul, Brazil 13 Planetary systems Review & Invited Talks The evolution of protoplanetary disk Matthias R. SchreiberB1 The evolution of protoplanetary disks is essential for the star and planet formation process. While we have discovered several mechanisms that are likely to drive the evolution of disks, e.g. grain growth, photoevaporation, planet formation, or binarity, we still struggle to understand their relative importance for the global evolution of protoplantary disks and to relate them to observations. I will review recent progress based on large infrared surveys of star forming regions, highlight spectacular discoveries made with ALMA, discuss the possible detections of forming planets still embedded in their disks, and outline the future prospects of this rapidly advancing research field. B 1 [email protected] Universidad de Valparaiso, Chile 14 Review & Invited Talks Galaxies Galaxies at High Redshift Franz. E. BauerB1 Recent years have seen tremendous progress in finding and charactering star-forming galaxies at high redshifts across the electromagnetic spectrum, giving us a more complete picture of how galaxies evolve, both in terms of their stellar and gas content, as well as the growth of their central supermassive black holes. A wealth of studies now demonstrate that star formation peaked at roughly half the age of the Universe and drops precariously as we look back to very early times, and that their central monsters apparently growth with them. At the highest-redshifts, we are pushing the boundaries via deep surveys at optical, X-ray, radio wavelengths, and more recently using gamma-ray bursts. I will review some of our accomplishments and failures. Telescope have enabled Lyman break galaxies to be robustly identified, but the UV luminosity function and star formation rate density of this population at z = 6 8 seems to be much lower than at z = 2 4. High escape fractions and a large contribution from faint galaxies below our current detection limits would be required for star-forming galaxies to reionize the Universe. We have also found that these galaxies have blue rest-frame UV colours, which might indicate lower dust extinction at z > 5. There has been some spectroscopic confirmation of these Lyman break galaxies through Lyman-↵ emission, but the fraction of galaxies where we see this line drops at z > 7, perhaps due to the onset of the Gunn-Peterson effect (where the IGM is opaque to Lyman-↵). B 1 [email protected] Pontificia Universidad Católica de Chile 15 Galaxies Review & Invited Talks The star formation history of galaxies in the CALIFA survey Rosa González DelgadoB1 ; Roberto Cid Fernandes2 ; Enrique Pérez1 ; Ruben Garcı́a Benito1 ; André Amorim1,2 ; Clara Cortijo1 ; Rafael López Fernández1 ; Sebastian Sánchez1 The spatially resolved star formation history (SFH) of galaxies contains fundamental information to understand how the galaxies formed and evolve. We apply the fossil record method based on spectral synthesis techniques to recover the SFH resolved in space and time for more than 200 galaxies from the CALIFA survey, which is gathering Integral Field Spectroscopy over the optical range and up to radial distances of 3 half light radii (HLR) of local (z = 0.005–0.03) galaxies. This CALIFA sub-sample is well distributed in the colormagnitude diagram and contains a fair representation from the ellipticals through the bulge dominated to the pure disk galaxies. In terms of stellar mass, the galaxies are distributed between Log M (Msun)= 9 to 12 with a peak in galaxies like the MW and M31. We investigate the SFH of galaxies and their trends of the radial structure as a function of the galaxy stellar mass and morphology. We show how the different galactic spatial sub-components (”bulge” and ”disk”) grow their stellar mass over time. We find that star formation history of bulges is more fundamentally related to the stellar galaxy mass, and in contrast disks is related with the local stellar mass surface density. We also obtain the spatially averaged and integrated galaxy properties, and how they are related with the properties at 1HLR. B 1 2 [email protected] Instituto de Astrofı́sica de Andalucı́a Universidade Federal de Santa Catarina 16 Review & Invited Talks Instrumentation ESO: Present and Future Andreas KauferB1 ESO is an intergovernmental organization for astronomy founded in 1962 by five countries. It currently has 14 Member States in Europe with Brazil poised to join as soon as the Accession Agreement has been ratified. Together these countries represent approximately 30 percent of the world’s astronomers. ESO operates optical/infrared observatories on La Silla and Paranal in Chile, partners in the sub-millimeter radio observatories APEX and ALMA on Chajnantor and is about to start construction of the Extremely Large Telescope on Armazones. La Silla hosts various robotic telescopes and experiments as well as the NTT and the 3.6m telescope. The former had a key role in the discovery of the accelerating expansion of the Universe and the latter hosts the ultra-stable spectrograph HARPS which is responsible for the discovery of nearly two-thirds of all confirmed exoplanets with masses below that of Neptune. On Paranal the four 8.2m units of the Very Large Telescope, the Interferometer and the survey telescopes VISTA and VST together constitute an integrated system which supports 16 powerful facility instruments, including adaptive-optics-assisted imagers and integralfield spectrographs, with half a dozen more on the way and the Extremely Large Telescope with its suite of instruments to be added in about ten years time. Scientific highlights include the characterisation of the supermassive black hole in the Galactic Centre, the first image of an exoplanet, studies of gamma-ray bursts enabled by the Rapid Response Mode and milliarcsec imaging of evolved stars and active galactic nuclei. The single dish APEX antenna, equipped with spectrometers and wide-field cameras, contributes strongly to the study of high-redshift galaxies and of star- and planet-formation. Early Science results obtained with the ALMA interferometer already demonstrate its tremendous potential for observations of the cold Universe. The review will summarize the entire ESO program and consider the next steps. B 1 [email protected] ESO 17 Stellar systems Review & Invited Talks Galactic Dynamics: Origin, History, Present and Prospect Barbara PichardoB1 In this talk I will present a travel through the history and main contributions to astrophysical development of the galactic dynamics discipline, passing by the most successful predictions and models, finishing with an integral vision of what is known from the Milky Way structure from it dynamics and the prospects with the new large scale surveys to understand it in the next decades. B 1 [email protected] Instituto de Astronomı́a, Universidad Nacional Autónoma de México (UNAM) 18 Review & Invited Talks AGN Determining the distances of the structures surrounding super-massive black holes Steenbrugge, K. C.B1,2 The surroundings of super-massive black holes located in the centers of active galaxies is complex with many components, such as the accretion disk, the corona, broad line region, the reflection component, the torus and warm absorber, which is outflowing ionized plasma. The distance from the black hole, the size and geometry of most of these components is poorly constrained. To constrain some of these physical parameters we used the technique of time-resolved UV and X-ray spectroscopy. We obtained optical to gamma-ray spectra and lightcurves over 100 days for Mrk 509, one of the brightest AGN in the X-ray band. The most important conclusions are that the corona is consistent with an optically thick and relatively low temperature layer on top of the accretion disk, compto-ionizing the accretion disk photons. The reflection component, easily detected through the broad Fe K↵ line, is located between 40-1000 gravitational radii from the black hole. Two of the warm absorber components have a distance of ⇠10 pc and for the others the distance is larger than 70 pc, and all are thus located well outside the broad line region. From these distances we can constrain the importance of these outflows on galactic evolution through feedback and the recycling of metals in the galaxy. B 1 2 [email protected] Instituto de Astronomia, Universidad Catolica del Norte, Avenida Angamos 0610, Antofagasta, Chile Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK 19 Cosmology Review & Invited Talks Testing Fundamental Hypotheses in Cosmology J. S. AlcanizB1 Testing fundamental hypotheses in cosmology constitutes an important task for fundamental physics since any violation of them would be a clear evidence of new physics. In this talk, we review some of these hypotheses and discuss the possibility of testing the so-called cosmic distance duality relation (CDDR). We derive a new relation involving current measurements of the gas mass fraction of galaxy clusters from the SunyaevZeldovich effect fSZE and x-ray surface brightness fX ray observations, i.e., fSZE = ⌘fX ray , where ⌘ quan- tifies deviations from the CDDR. Since this latter expression is valid for the same object in a given galaxy cluster sample, its application to current data removes possible contaminations from different systematics error sources and redshift differences involved in luminosity and angular diameter distance measurements. We use the most recent fX ray and fSZE data to test the CDDR as an exact principle in Nature and discuss the results in the light of some possible physics mechanisms of CDDR violation. B 1 [email protected] Observatório Nacional/MCTI 20 Review & Invited Talks Cosmology Multiple-tracer surveys of the large-scale structure of the Universe L. Raul AbramoB1 New astrophysical surveys are starting to detect galaxies of many different types in massive numbers. At the same time, these surveys are also mapping with exquisite accuracy the different environments where these galaxies live. I will show that redshift surveys that map several different tracers of large-scale structure (e.g., galaxies of different luminosities, or halos of different masses) are a new leap forward for Cosmology. These surveys can even appear to overcome the fundamental statistical limitation known as cosmic variance. I will show how this is in fact possible, and how we can enhance constraints on cosmological parameters when a given survey has a sufficient number of tracers of large-scale structure of different biases. I will make the case for the multiple-tracer approach using the concrete example of J-PAS (the Javalambre PAU Astrophysical Survey), one of the most promising redshift surveys of the near future. B 1 [email protected] Physics Institute, University of Sao Paulo 21 Instrumentation Review & Invited Talks Mmtron de Graauw, T.B1 Millimetron is a 10-meter cooled space observatory that is optimized for the far-infrared and submm wavelength range. The facility has two operating modes: one can operate as a single-dish observatory or as an element of a space-earth VLBI system. It will have scientific capabilities that can address various key problems in astronomy and astrophysics such as the formation and evolution of stars and planetary systems, evolution of galaxies, quasars etc.. The telescope will be deployed in space and the panels of the primary mirror are to be adjustable to achieve an rms accuracy less than 10 micron. The telescope and instrument compartment will be cooled down to 4.5K by passive cooling and mechanical coolers. The instrument package is to include a set of heterodyne receivers operating in several bands between from 500 and 5000 GHz, a submm array camera/spectrometer and a mm array camera/spectrometer covering 50 micron to 3 mm. Millimetron is proposed as a Russian-led mission and is to include a wide international collaboration. Currently, the mission scheduled to be launched in 2020. B 1 [email protected] ALMA 22 Review & Invited Talks Instrumentation The SOFIA Airborne Infrared Observatory - first science highlights and future science potential Hans ZinneckerB1 SOFIA, short for Stratospheric Observatory for Infrared Astronomy, is a Boeing 747SP aircraft with a 2.7m telescope flying as high as 45000 ft in the stratosphere above 99 percent of the precipitable water vapor. SOFIA normally operates from its base in Palmdale, California, and a typical observing flight lasts for 10 hours before returning to base. SOFIA has started astronomical observations in Dec 2010 and has completed some 30 early science flights in 2011, delivering a number of exciting results and discoveries, both in mid-infrared imaging (5-40mu) and in far-infrared (THz) heterodyne high-resolution spectroscopy which were published in mid-2012 in special issues of ApJ Letters and A & A, respectively. Meanwhile, in July 2013, as part of Cycle 1, SOFIA has deployed to New Zealand for a total of 9 flights (all of them successful) and has observed key targets in the southern hemisphere at THz frequencies, including star forming regions in the Large and Small Magellanic Clouds. In this talk, I will present a few highlights of SOFIA early science and its future potential, when the full suite of 7 instruments will be implemented by the time of full operations in 2015. As Herschel ran out of cryogens in April 2013, SOFIA will be the premier FIR-astronomical facility for many years to come. Synergies with ALMA and CCAT must be explored. SOFIA is a major bilateral project between NASA and the German Space Agency (DLR), however as an international observatory it offers observing time to the whole astronomical community world-wide, not only to the US and German primary partners. B 1 [email protected] SOFIA Science Center at NASA-Ames, USA and DSI at Univ. of Stuttgart, Germany 23 Star formation Review & Invited Talks Star and planet formation in the era of the submillimeter observatories SMA/ALMA Luis ZapataB1 In this talk, I will present the recent advances and challenges on the star and planet formation studies in era of the submillimeter observatories: the Submillimeter Array (SMA) and the Atacama Large Millimeter/Submillimeter Array (ALMA). These observatories now provide angular resolutions similar to those obtained in the optical regimen allowing to study the obscured innermost parts of the circumstellar disks where the planet and star formation are taken place. When ALMA is finished, its sensivity and high angular resolution might reveal planets around close-by young stars just in the process of formation. This will open a new venue for the understanding on the origin of our own solar system. B 1 [email protected] Centro de Radioastronomı́a y Astrofisica (CRyA), UNAM 24 Short Talks 25 Planetary Systems PS -1 Multi-band characterization of hot jupiters using OPD data M. MoyanoB1 ; L. A. Almeida2,3 ; F. Jablonski3 If an exoplanet’s orbit is oriented along the line of sight, it is possible to observe periodic transits. The study of transiting extrasolar planets (TEPs) provides an unmatchable source of planetary properties and make possible for the first time to access to an accurate ensemble of parameters such as radii or semi-major axis. Multi-band observations of a TEP constrain much more the physical properties of the system. Parameters such as the inclination are independent of wavelength and can be determined much better if transits at different passbands are observed. In addition, these observations also serve as a first-order broad-band transmission spectrum, which can be used to search for the presence of strong absorbers. The measured planetary radius is wavelength-dependent and measurements of its changes are indication of possible spectral variations. I will summarize the analysis and results of a multi-band observing campaign to characterize the hot jupiters Wasp-44b, Wasp-5b, and Wasp-46b. These observations were carried out at the Observatorio do Pico dos Dias (OPD/LNA), in Brazil. This study includes the first transit follow-up characterization of the planet Wasp-46b. B 1 2 3 [email protected] Instituto de Astronomı́a, Universidad Católica del Norte Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas IAG/USP Instituto Nacional de Pesquisas Espaciais/MCTI 27 Planetary Systems Short Talks PS -1 Creep tides. A new model to study the tidal evolution of close-in satellites and exoplanets Ferraz-Mello, S.B1 We present a new reophysical theory of the dynamical tides of celestial bodies in which the body tends always to creep towards the equilibrium (inviscid) by the only action of the gravitational forces acting on it (selfgravitation and tidal potential) with a rate inversely proportional to its viscosity. The adopted creep law is Newtonian linear) and at every instant the stress is assumed proportional to the distance to the equilibrium. This leads to a non-homogeneous ordinary differential equation that determines the distortion due to the tidal perturbation. In this approach the dissipation is inversely proportional to ( + 1) ( is the tide frequency in units of a relaxation factor inversely proportional to the viscosity). In the inviscid limit, the dissipation is roughly proportional to the frequency (as in standard theories), but when the viscosity is high and the relaxation factor much smaller than the tide frequency the dissipation decreases almost linearly with the frequency. The theory is applied to several Solar System and extrasolar bodies and values of the relaxation factor are derived for these bodies. A numerical approach allowed us to overcome the cumbersome algebraic manipulations involved in applications to more complex problems and to introduce the perturbations by a third body. The results for the tidal terms of the physical libration of the Moon have been compared to the values determined from the Lunar Laser Ranging measurements. The comparison of the predictions of the theory to observations serves to validate the theory and also to indicate possible future improvements. B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas 28 Short Talks Planetary Systems PS -1 Stellar Occultations by Transneptunian and Centaurs Objects: results from more than 10 observed events Braga-Ribas, F.B1 ; Vieira-Martins, R.1 ; Assafin, M.2 ; Camargo, J. I. B.1 ; Sicardy, B.3 ; Ortiz, J. L.4 Transneptunian objects (TNOs) and Centaurs are small fossils of the Solar System orbiting beyond Saturn. Over 1200 of them have been found since 1992, and among them we find dwarf-planets such as Pluto, Makemake and Eris. Their origin, dynamical evolution and collisional history are linked to the formation of the Solar System. Having information about their size and mass distribution, surface and internal structure (albedo, shape and density) can help the understanding of the dynamical evolution of our system. We use the stellar occultation technique which consists in observing a star while the object transit in front of it. The precise duration of the event, observed from several different sites, allows to deduce their size and shape with kilometric accuracy. If the object has an atmosphere (as Pluto for example), the light of the star is attenuated during its ingress and egress behind the body, so we can determine its pressure down to the nanobar level, or put a limit to its presence. Our group has developed a long-term prediction process which consists of observing the sky path of selected objects, constructing an astrometric star catalogue used to predict these events. This work allowed us to detect several occultations and derive interesting results. For instance, we learned that Eris, known as the biggest TNO, has the same size as Pluto within the error bars, but a very high albedo, probably due to a condensed atmosphere. Makemake, the third biggest known TNO, has no global atmosphere and a high albedo. Quaoar has a diameter greater than 1100 km, a density of 2.0 ± 0.5 g cm3 , and a low albedo. Varuna and 2003 AZ84 , other big objects, are very elongated. These results, among others, will be detailed, and their impact to our knowledge about these far objects, will be discussed. By the time of this writing thirteen events were already observed by our group, involving nine different objects, in an international consortium between the Observatório Nacional / BR - Paris-Meudon Observatory / FR - Instituto de Astrofı́sica de Andalucı́a / ES. B 1 2 3 4 [email protected] Observatório Nacional / MCTI, Rio de Janeiro, Brazil Observatório do Valongo/UFRJ, Rio de Janeiro, Brazil Observatoire de Paris - Meudon / LESIA, Meudon, France Instituto de Astrofı́sica de Andalucı́a, CSIC, Spain 29 Planetary Systems Short Talks PS -1 Imaging polarimetry of the potentially planet-forming circumstellar disk HD 142527. The NaCo view Cánovas, H.B1,9 ; Ménard, F.2,6,9 ; Hales, A.3,4,9 ; Jordán, A.5,9 ; Schreiber, M. R.1,9 ; Casassus, S.6,9 ; Gledhill, T. M.7 ; Pinte, C.8 HD 142527 is a unique system in terms of planet formation. Its high accretion rate combined with its huge inner gap and short age make of it an ideal candidate for harboring forming planets. ALMA cycle-0 observations revealed gap crossing gas streams and showed that the millimeter-sized dust particles are distributed in a horse-shoe shape. Here I present our recent NIR imaging polarimetry results of HD 142527 obtained with NaCo/VLT. By means of polarimetry, we remove most of the stellar light, directly imaging the disk’s inner regions. Our observations allow us to constrain the dust properties (size, composition and porosity) on the surface of the the outer disk. We also detect two regions of the disk with low emission (”nulls”) both in polarized and unpolarized light. Intriguingly, one of these nulls is azimuthally coincident with the maximum of the horse-shoe shape detected by ALMA. We discuss the possible link between these two (different?) features. B 1 2 3 4 5 6 7 8 9 [email protected] Departamento de Fı́sica y Astronomı́a, Universidad de Valparaı́so, Valparaı́so, Chile UMI-FCA, CNRS / INSU France (UMI 3386) Atacama Large Millimeter/Submillimeter Array, Joint ALMA Observatory, Alonso de Córdova 3107, Vitacura 763-0355, Santiago - Chile National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, Virginia, 22903-2475, United States Instituto de Astrofı́sica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile Departamento de Astronomı́a, Universidad de Chile, Casilla 36-D, Santiago, Chile Science and Technology Research Institute, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK UJF-Grenoble 1 / CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble, F-38041, France Millenium Nucleus “Protoplanetary Disks in ALMA Early Science”, Universidad de Chile, Casilla 36-D,Santiago, Chile 30 Short Talks Planetary Systems PS -1 The Janus-Epimetheus Ring B1 Winter, O. C. ; Pinho, A.1 ; Sfair, R.1 ; Mourao, D. C.1 ; Foryta, D.2 ; Giuliatti Winter, S. M.1 The known planetary ring systems of Saturn, Jupiter, Uranus and Neptune present a wide range of peculiar cases. However, a different from all of them has been found sharing its trajectory with Janus and Epimetheus, co-orbital satellites of Saturn. In the present work we show that, behaving like a firefly, this ring can only be seen from time to time, when the Cassini spacecraft, the ring and the Sun are in a particular geometric configuration. Otherwise, it “remains in the dark”, not being visible by the spacecraft camera. Another interesting feature of the Janus-Epimetheus ring (J-E ring) is that all its particles are removed from the ring within the shortest lifetime ever found among the planetary rings. The large particles (> 8 micrometers) have a lifetime of at most a few years, being removed by collisions with one of the co-orbital moons, while the small particles (< 8 micrometers) show even shorter lifetimes (a few tens of days), being removed by encounters with the F ring. So, the J-E ring needs to be constantly replenished. Using Janus and Epimetheus as targets and considering the flux of micrometeorites that reaches the J-E ring region, we developed a detailed physical model that matches very well the data of the J-E ring extracted from Cassini images. We show that the existence of the J-E ring is due to the constant supply of material extracted from the co-orbital moons by collisions with micrometeorites, and the generated size distribution of particles selects the light scattering regime responsible for the “firefly” behaviour of this ring. B 1 2 [email protected] Grupo de Dinamica Orbital e Planetologia - UNESP - Guaratingueta - SP - Brazil Departamento de Fisica - UFPR - Curitiba - PR - Brazil 31 Planetary Systems Short Talks PS -2 Young Brown Dwarfs as Giant Exoplanet Analogs Faherty, J. K.B1,2,3 ; Rice, E.2,4 ; Cruz, K.2,5 Young brown dwarfs and directly-imaged exoplanets have enticingly similar photometric and spectroscopic characteristics, indicating that their cool, low gravity atmospheres should be studied in concert. We have identified, confirmed, and characterized several new young M and L type brown dwarfs (see Faherty et al. 2013) and compared them to directly-imaged planetarymass companions and exoplanets like 2MASS 1207b and HR8799b. Similarities between the peculiar shaped H band and location on near-IR color magnitude diagrams provide important clues about how to extract physical properties of planets from current brown dwarf observations. In this talk I will present newly found systems and describe our comparative browndwarf exoplanet studies. B 1 2 3 4 5 [email protected] Universidad de Chile American Museum of Natural History Carnegie Department of Terrestrial Magnetism College of Staten Island Hunter College 32 Short Talks Planetary Systems PS -2 Precise stellar occultation predictions for 39 selected TNOs/Centaurs Camargo, J. I. B.B1 ; Assafin, M.2 ; Vieira-Martins, R.1 ; Sicardy, B.3 ; Braga-Ribas, F.1 ; Desmars, J.1 ; Benedetti-Rossi, G.1 ; Dias-Oliveira, A.1,3 ; Andrei, A. H.1 ; da Silva Neto, D. N.4 Trans-Neptunian objects (TNOs) are Solar System bodies located in the range within 30 100 AU from the Sun. They are also relics, relatively unaltered, of the proto-planetary disk from which Solar System planets emerged. Therefore, these are key objects to help us better understand the history and evolution of the outer Solar System. Centaurs are a population of objects orbiting closer to the Sun than the TNOs and Neptune. They can be interpreted as small size representatives of the same primitive parent population of TNOs, filling up the gap of small TNOs that cannot be observed with current telescope facilities. Currently, about 200 Centaurs are known. One of the ways to study these bodies, TNOs and Centaurs, is given by the analysis of a light curve as obtained when they occult a star. Stellar occultations are the only ground-based way to derive their sizes with kilometric accuracy and detect putative atmospheres as tenous as few nanobars. These events, rare in many cases and that naturally encourage international collaborations, always require a huge observational and computational work to predict where and when on the Earth they can be observed. Different sets of observations are used to determine the positions of TNOs/Centaurs and of the stellar content around their paths on the sky. An initial accuracy of 000 .05 is obtained to all positions which must be then refined to 000 .02 as the possible event approaches. As a continuation of previous works, where predictions of stellar occultations by Pluto (plus Charon, Nix and Hydra) and 10 other large TNOs (Assafin et al. 2010, 2012) were made, we have just concluded the preparation of predictions for a set of 39 selected TNOs and Centaurs for the period 2012.5 to the end of 2014. The necessary observational data was acquired during 4 consecutive semesters, from 2011 to 2013, at La Silla with the ESO/MPG 2.2m telescope equipped with its Wide Field Imager (WFI). It is relevant to mention that these works have predicted almost all of the stellar occultations by TNOs observed so far, exception made for Pluto. Here, we present the whole process involved in determining the predictions as well as some important problems and possible solutions, from observations to ephemeris corrections. We also present some selected predictions and light curves along with expectations for the near future of this work. B 1 2 3 4 [email protected] Observatório Nacional / MCTI Observatório do Valongo / UFRJ Observatoire de Paris-Meudon - França Universidade Estadual da Zona Oeste / RJ 33 Planetary Systems Short Talks PS -2 Large Semimajor Axis Centaurs: where do they come from? Gomes, R. S.B1 ; Soares, J. S.1 ; Brasser, R.2 Centaurs are Solar System objects in unstable orbits whose perihelia are in the realm of the major planets. Some of these Centaurs have large semimajor axis (Laces) with their aphelia beyond 2000 AU. Small semimajor axis Centaurs are usually believed to originate in the scattered disk, but Laces would have as its most likely origin the Oort Cloud. We argue however that the Oort Cloud could not produce as many Laces as are estimated through the number of those already observed. In this way, we propose that a still undiscovered planetary mass solar companion could be enhancing the production of Laces thus accounting for the current number of observed Laces. B 1 2 [email protected] Observatório Nacional, Rio de Janeiro, Brasil Institute for Astronomy and Astrophysics, Academia Sinica, Taipei 106, Taiwan 34 Short Talks Planetary Systems PS -2 Atlas of the three body resonances in the Solar System Gallardo, T.B1 Three body resonances (TBRs) between a massless particle with an arbitrary orbit and two planets P1 and P2 in circular coplanar orbits occur when the critical angle = k0 0 + k1 1 + k2 2 (k0 + k1 + k2 )$0 being ki integers is oscillating over time. The approximate localization in semimajor axis of the TBRs taking arbitrary pairs of planets is very simple, specially if we ignore the secular motion of the perihelion and nodes of the perturbing planets. When these slow secular motions are taken into account each of the nominal three body resonances split in a family of resonances all them very near the nominal one. The challenge is to obtain the width, strength or whatever that give us the dynamical relevance of these TBRs. We propose an algorithm to numerically estimate the strength of arbitrary TBRs between two planets in circular coplanar orbits and a massless particle in an arbitrary orbit. This algorithm allowed us to obtain an atlas of the TBRs in the Solar System showing where are located and how strong are thousands of TBRs involving all the planets from 0 to 1000 au. Relevant results for the population of asteroids and transneptunian objects will be presented. B 1 [email protected] Facultad de Ciencias, Universidad de la República, Uruguay 35 Planetary Systems Short Talks PS -3 Detectability of Habitable Planets around Very Low-Mass Stars Martioli, E.B1 ; Martı́n, E. L.2 ; Cabrera, J.3 ; Solano, E.2 ; Tata, R.4 We present observations of 18 very low-mass stars with Kepler light curves available in the public archive, where we performed a search for transits and characterized the photometric variability to estimate the effects of stellar activity in the detectability of habitable planets around stars at the cool end of the stellar mass distribution. We obtained low-resolution red optical spectra and found the spectral types of these targets to lie in the range dM4.5–dM8.5, implying spectrophotometric distances from 17 pc to 80 pc. We find that the size of the planets detectable by Kepler around these small stars typically lie in the range 1 to 5 Earth radii within the habitable regions (P10 days). For 11 of these objects reliable photometric periods shorter than 7 days are derived, and are interpreted as rotational modulation of magnetic cool spots. For 3 objects we find possible photometric periods longer than 50 days that require confirmation. H-alpha emission measurements and flare rates are used as a proxies for chromospheric activity and transversal velocities are used as an indicator of dynamical ages. We discuss the relationship between age, magnetic activity and rotation in fully convective stars, and the detectability of planets around them. We show that Super-Earth planets with sizes around 2 Earth radii are detectable with Kepler around about half of the stars in our sample, independently from their level of chromospheric activity. B 1 2 3 4 [email protected] Laboratório Nacional de Astrofı́sica (LNA/MCTI) Centro de Astrobiologı́a (INTA-CSIC) Institute of Planetary Research, German Aerospace Center Instituto de Astrofı́sica de Canarias 36 Short Talks Planetary Systems PS -3 Tidal, thermal and magnetic evolution of terrestrial exoplanets in the habitable zone of dwarf stars P. Cuartas-RestrepoB1 ; M. Melita2 ; J. Zuluaga1 ; J. Hoyos3 ; M. Sucerquia1 The rotation and thermal evolution of a planet plays a main role in the planetary magnetic field evolution. The rotation period determines properties like the regime of the planetary dynamo and its intensity. This is crucial for a planet to keep its reservoir of volatile material like water, protected against the erosive action of the stellar wind and cosmic rays. Planets orbiting dwarf stars are tidally afected by their host, this detemines the final rotation period (resonance) or the tidal locking of the planet, especially during the very first Myr. At the same time this first period of the planet history is the most afected by the magnetic activity of the host star. We calculate the rotation and tidal evolution of planets and combine this with a thermal evolution model to know how this very first stages of the planetary evolution finish with an stable and protective planetary magnetic field or with an unprotected planet. B 1 2 3 [email protected] Instituto de Fı́sica - FCEN, Universidad de Antioquia, Medellı́n, Colombia Instituto de Astronomı́a y Fı́sica del Espacio - IAFE, Buenos Aires, Argentina Departamento de Ciencias Básicas, Universidad de Medellı́n, Medellı́n, Colombia 37 Planetary Systems Short Talks PS -3 Mapping the early distribution of volatiles in the Main Belt with the JPAS/J-PLUS photometric survey J. M. CarvanoB1 ; M. De Prá1 ; D. Lazzaro1 ; F. Roig1 ; A. Alvarez-Candal1 ; T. Mothé-Diniz2 The JPAS/J-PLUS is a joint Spanish-Brazilian project that aims to map an area of the sky of 8000 square degrees, in order to measure, with unprecedented accuracy, the redshifts of a large sample of extragalactic objects up magnitude 23. It involves the installation of two telescopes on the Javalambre Mountains, in Spain. The T250 telescope will have an aperture of 250cm and will be equipped with a camera with a 3 square degree field of view and will use a set of 56 filters (54 narrow band + 2 wide band) covering the 0.3-1.0 micron range, while the T80 telescope (presently on commissioning phase) will have a camera with 2 square degree field of view and will use a set of 12 narrow and intermediate band filters covering the same wavelength range. During its execution, the surveys will also observe a large number of minor Solar System bodies. For those objects, the differential of JPAS/J-PLUS with respect to other large photometric survey is the number and position of the filters used, which will allow a better identification of some taxonomic classes that are not well defined only with SDSS-like filter systems. In particular, the JPAS/J-PLUS data set will allow a robust identification of the 0.7 micron water alteration band that characterize the Ch class in Bus taxonomy. Thus, with JPAS/J-PLUS it will be possible to map the occurrence of water alteration in the present Solar System, which in turn will allow us to put further constraints of the presence of volatiles and of heating processes in the early Solar System. B 1 2 [email protected] Coordenadoria de Astronomia e Astrofı́sica, Observatório Nacional - MCTI Observatório do Valongo, UFRJ 38 Short Talks Planetary Systems PS -3 A dynamical mechanism to produce high-inclinations TNOs Brasil, P. I. O.B1,2 ; Gomes, R. S.2,3 ; Nesvorný, D.2 We discuss the dynamical formation of small Solar System objects beyond Neptune. The discovery of the first trans-Neptunian object (TNO) except for Pluto and Charon is relatively recent (1992QB1 ). Many unpredicted dynamical and physical features not predicted in past theoretical models and are now showing up. Among them, we note the existence of many high-inclined orbits with respect to the eclipitc plane (where all Solar System bodies supposedly have formed). The aim of this work is to show a dynamical pathway from the primordial planetesimal disk to high inclinations orbits in the trans-Neptunian region. The main mechanism requires that scattered planetesimals are captured into some exterior mean motion resonance (MMR) with Neptune and then be trapped into the Kozai resonance as well. After that, some planetesimals may access a resonance hibernating mode in which the planesimal is barely locked in resonance. We show that only a few percent of all scattered planetesimals would access the hibernating mode. But, once this mechanism is active, ⇠ 100% of the particles would escape both resonances while Neptune is in its final migration stage (after the LHB phase). Our results could explain at least a portion (up to 80%) of the classical hot population, defined by a2:3 < a < a1:2 , i > 5o , and q > 36au. Previous results indicate that this mechanism is the most likely to form the detached objects close to MMR with Neptune as, for example, 2004XR190 (Gomes, 2011, Icarus 215, 661). We have determined the most probable regions, in the orbital elements space (a, e, i), where detached objects would form close to 2:5 and 1:3 MMRs (Brasil, Gomes & Soares, 2013 - submitted to A&A). B 1 2 3 pedro [email protected] Instituto Nacional de Pesquisas Espaciais, Divisão de Mecânica Espacial e Controle - INPE/DMC Southwest Research Institute, Departments of Space Studies and Space Operations - SwRI/DSSSO Observatório Nacional, Grupo de Pesquisa em Astromomia - ON/GPA 39 40 Stars & Stellar Systems SSS -1 A study of the recent chemical evolution of the Large Magellanic Cloud Palma, T.B1,2 ; Clariá, J. J.1,2 ; Geisler, D.3 ; Ahumada, A. V.1,2 We present the results of a study of the Large Magellanic Cloud (LMC) chemical evolution during the last 2.2 Gyr. This study was based on Washington photometric observations of LMC’s star clusters carried out with the Cerro Tololo Inter-American Observatory (CTIO) 4 m telescope. As tracers of the LMC’s chemical enrichment, we used 83 star clusters projected both on the bar and in the inner and outer LMC disc, more than half of which have not been previously studied. We determine size, reddening, deprojected distance, age and metallicity of the observed star clusters. We show that the most metal-poor clusters are distributed throughout the entire disc while most metal-rich clusters are mainly located in the inner disc. We find that the youngest clusters tend to be located in the inner disc whereas intermediate-age clusters are mainly found at larger deprojected Galactocentric distances. These trends are maintained when the sample is complemented with clusters observed by other authors using the same technique. These results appear to strengthen the idea of the absence of a radial metallicity gradient in the LMC for metal-poor clusters. The resulting age-metallicity relationship appears to be unrelated to what LMC region is considered. B 1 2 3 [email protected] Observatorio Astronómico, Universidad Nacional de Córdoba, Argentina CONICET Departamento de Astronomı́a, Universidad de Concepción, Chile 41 Stars & Stellar Systems Short Talks SSS -1 Star clusters in an infalling galaxy Mora M. D.B1 ; Chanamé J.1 ; Puzia T.1 Star clusters are among the most common stellar systems in the universe. Their formation occurs as part of a hierarchical process where large interstellar regions fragment into giant molecular clouds and cloud cores (e.g. Elmegreen 2011). These fragments are highly sub-structured, containing dense clumps and filaments showing a typical fractal dimension (e.g. Scheepmaker et al. 2009a; Sanchez & Alfaro 2008) where cluster-cluster interactions occurs and may lead to star-cluster disruption or star-cluster merging (Kroupa 1998; Fellhauer & Kroupa 2005). In this work we present the discovery of several young star clusters and star cluster complexes in NGC 1427A, a dwarf irregular galaxy that is likely infalling toward the center of the Fornax galaxy cluster for the first time at supersonic speed (Chanamé et al. 2000). Its apparent morphological distortion and star clusters lining up within the bow-shock region make us to believe that this star formation activity is triggered by the passage through the hot intra cluster medium of the Fornax cluster. B 1 [email protected] Pontificia Universidad Católica Chile 42 Short Talks Stars & Stellar Systems SSS -1 Planetary nebulae near the Galactic centre: chemical abundances Cavichia, O.B1 ; Costa, R. D. D.1 ; Maciel, W. J.1 ; Molla, M.3 Planetary nebulae (PNe) are the offspring of stars within a large mass interval (0.8 8 M ). PNe constitute an important tool to study the chemical evolution of the Milky Way and other galaxies, probing the nucleosynthesis processes, abundance gradients and the chemical enrichment of the interstellar medium. However, the presently available chemical composition studies are strongly biased, since they were focused on brighter objects, predominantly located in Galactic regions of low interstellar reddening. In this work, we report physical parameters and abundances derived for a sample of high extinction PNe located in the Galactic bulge, near the Galactic centre, based on low dispersion spectroscopy secured at the SOAR telescope using the Goodman spectrograph. The new data allow us to extend our database including older, weaker objects that are at the faint end of the planetary nebula luminosity function (PNLF). The results show that the abundances of our sample are similar to those from other regions of the bulge. Nevertheless, the average abundances of the galactic bulge do not follow the observed trend of the radial abundance gradient in the disk. We propose a chemical evolution model for the Galactic bulge to explain the observed data, adopting a scenario where the bulge is formed in a single collapse timescale of 2 Gyr, which is longer than other chemical evolution models predict. There is no need to invoke a second infall episode, as recently suggested by other authors to explain the observed bulge metallicity distribution. B 1 2 [email protected] Universidade de São Paulo Dept. of Basic Research - CIEMAT 43 Stars & Stellar Systems Short Talks SSS -1 New axion bounds from the white dwarf luminosity function Melendez, B. E.B1,2 ; Miller Bertolami, M. M.1,2,3 It has been shown that the shape of the luminosity function of white dwarfs (WDLF) can be a powerful tool in order to check the possible existence of DFSZ-axions, a proposed but not yet detected type of weakly interacting particle. In this research we show that the feedback of the axion emission into the neutrino emission cannot be neglected at high luminosities (MBol  8), and that the axion emission need to be incorporated in a self-consistent way into the evolution of the white dwarfs when dealing with axion masses larger than ma cos2 5meV. We have performed a 2 -test in order to have a quantitative measure of the agreement between the theoretical WDLF -computed under assumptions of different axion masses- on the one hand and the observed WDLF on the other. Our results indicate that axion masses larger than ma cos2 10meV can be rejected at more than a 99.9% confidence level and that the existence or non-existence of axions with masses ma cos2  5meV cannot be concluded at any significant confidence level with the current knowledge of the WDLF. Our results also confirm the disagreement between the observed WDLF and the cooling speed by asteroseismological tools on G117-B15A. B 1 2 3 [email protected] Facultad de Ciencias Astronómicas y Geofı́sicas de La Plata, La Plata, Argentina Instituto de Astrofı́sica de La Plata (IALP), UNLP-CONICET, La Plata, Argentina Max-Planck-Institut fur Astrophysick, Garching, Germany 44 Short Talks Stars & Stellar Systems SSS -2 Asteroseismology of massive pulsating DA white dwarf stars with fully evolutionary models A. D. RomeroB1 ; S. O. Kepler1 ; A. H. Córsico2 ; L. G. Althaus2 ; L. Fraga3 In this work we performed the first asteroseismological study for 42 massive DA white dwarf stars, or ZZ Ceti, based on detailed and fully evolutionary models representative of these stars. Our DA white dwarf models, cover a wide range of stellar masses, effective temperatures, and envelope thicknesses, are the result of fully evolutionary computations that take into account the complete history of the progenitor stars from the ZAMS. In addition, these models are characterized by a detailed and consistent chemical inner profile for the core and the envelope, which is crucial in white dwarf asteroseismology. Our sample comprise all the ZZ Ceti stars with spectroscopic stellar masses between 0.72 and 1.05M know to date. The asteroseismological analysis of a set of 42 stars gives the possibility to study the ensemble properties of the massive pulsating white dwarf stars with carbon oxygen cores, in particular the thickness of the hydrogen envelope and the stellar mass. B [email protected] Departamento de Astronomia, Universidade Federal do Rio Grande do Sul, Av. Bento Goncalves 9500 Porto Alegre 91501-970, RS, Brazil 2 Facultad de Ciencias Astronómicas y Geofı́sicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, (1900) La Plata, Argentina, Instituto de Astrofı́sica La Plata, CONICET-UNLP, Argentina 3 Southern Observatory for Astrophysical Research, Casilla 603, La Serena, Chile, Laboratório Nacional de Astrofı́sica – LNA/MCTI, R. Estados Unidos, 154, Itajubá, MG, CEP: 37504-364, Brazil 1 45 Stars & Stellar Systems Short Talks SSS -2 MLS110213:022733+130617: A new eclipsing polar above the period gap Silva, K. M. G.B1 ; Rodrigues, C. V.1 ; Oliveira, A. S.2 ; Almeida, L. A.1 ; Cieslinski, D.1 ; Costa, J. E. R.1 Polars are magnetic cataclysmic variables (CVs): short period binaries in which a low-mass main-sequence star transfers matter to a magnetic white dwarf via an accretion column. A stand-off shock is formed near the white-dwarf surface, followed by a hot post-shock region that cools down by cyclotron radiation mainly in optical and infrared ranges. Over a 135 polars and polar candidates were identified so far: ⇠ 26% have periods over the period gap ( P > 3h) and only 6 of these systems are eclipsing. We have obtained photometry and polarimetry (OPD) and spectroscopy (SOAR) data of MLS110213: 022733+130617 which is one of the polar candidates identified and monitored by the Catalina Sky Survey (CSS). After analyzed all the available data (OPD,SOAR,CSS) covering the last 7 years, we confirm the system as a new eclipsing polar. The long term observations obtained by CSS shows the system in two distinct brightness state, 1.5 mag apart. This kind of variation in polars are explained as variations in the mass rate accretion. A deep eclipse is observed with a decrease of 3 (1.5) mag in high (low) brightness state, indicating that system has a high inclination. From the mid-eclipse of the photometric data we estimated an orbital period of 3.787 hours which is in the above the period gap with only three other systems showing longer periods. In the high state of brightness, the light curve outside the eclipse is almost flat, while in the low state a strong modulation is observed, with a phase maximum 0.175. The polarimetric data is from high state of brightness. The system presents circular polarization varying in the range -3 to 15% in R-band, with a phase maximum 0.175, consistent with low state maximum, which confirms that this component is mainly due to cyclotron emission from the accretion column. The polarization does not have a standstill at zero, and there are phases when the signal changes, indicating a region always visible, but observed from the backside in some fases. A spectrum in the energy range 4500-7000 Å was obtained in the phase interval 0.7-0.88 which shows a flat continuum and strong emission-lines. There’s no clear evidence of the secondary star presence, however it shows the typical characteristic high ionized optically thick regions: i) Inverse Balmer series decrement (H↵ < H < H ) and ii) intense HeII 4686 are present. B 1 2 [email protected] Instituto Nacional de Pesquisas Espaciais Universidade do Vale do Paraı́ba 46 Short Talks Stars & Stellar Systems SSS -2 Symbiotic stars in X-rays and UV Luna, G. J. M.B1 ; Sokoloski, J. L.2 ; Mukai, K.3 ; Nelson, T.4 ; Nuñez, N. E.5 Until recently, symbiotic binary systems in which a white dwarf accretes from a red giant were thought to be mainly a soft X-ray population. I will describe the detection with the Swift/XRT of 14 white dwarf symbiotics that were not previously known to be X-ray sources. The 14 new X-ray detections were the result of a survey of more than 50 symbiotic stars using Swift fill-in programs during three years. Their X-ray spectra are consistent with thermal emission and fall naturally into three distinct groups. The first group contains those sources with a single, highly absorbed hard component, which we identify as probably coming from an accretion-disk boundary layer. The second group is composed of those sources with a single, soft Xray spectral component, which likely arises in a region where low-velocity shocks produce X-ray emission, i.e. a colliding-wind region. The third group consists of those sources with both hard and soft X-ray spectral components. Simultaneous Swift/UVOT data allowed us to find that unlike in the optical, where rapid, stochastic brightness variations from the accretion disk typically are not seen, detectable UV flickering is a common property of symbiotic stars. Supporting our physical interpretation of the two X-ray spectral components, the UV photometry shows that symbiotic stars with harder X-ray emission tend to have stronger UV flickering, which is usually associated with accretion through a disk. B 1 2 3 4 5 [email protected] Instituto de Astronomia y Fı́sica del Espacio, CONICET Columbia University NASA/GSFC & USRA University of Minnesota Instituto de Ciencias Astronómicas, de la Tierra y del Espacio 47 Stars & Stellar Systems Short Talks SSS -2 Time-lapse and flickering mapping of accretion discs: measuring the disc viscosity parameter Raymundo BaptistaB1 Flickering is the intrinsic brightness fluctuation of 0.01-1 mag on timescales of seconds to dozens of minutes that is seen in light curves of T Tau stars, mass-exchanging binaries and active galactic nuclei. It is considered a basic signature of accretion, and may be used to probe the anomalous viscosity that powers accretion discs. Maximum-entropy eclipse mapping techniques are key to the study of flickering and accretion disc viscosity in mass-exchanging binaries. By measuring the (viscous) timescale with which the disc responds to changes in mass input rate, one might infer the average disc viscosity parameter ↵ (time-lapse mapping). Moreover, by combining a large ensemble of lightcurves one can separately measure the low- and highfrequency flickering amplitude as a function of binary phase and derive maps of their surface brightness distributions from their eclipse shapes (flickering mapping). Flickering mapping of quiescent dwarf novae reveal that low-frequency flickering is associated to turbulence in the mass-transfer process, whereas high-frequency flickering arises in the accretion disc. Interestingly, if the disc-related flickering is caused by magneto-hydrodynamic turbulence in the disc’s atmosphere, its relative amplitude yields a direct measure of the ↵-viscosity parameter. The three dwarf novae mapped with this technique so far show high viscosity discs in quiescence (↵ ' 0.1 0.2). This is at odds with the thermal-viscous disc instability model to explain dwarf nova outbursts, which predicts that their discs switch between a cool, low-viscosity regime (↵ ⇠ 10 outburst. B 1 2 ) in quiescence to a hot, high-viscosity regime (↵ ⇠ 10 [email protected] Universidade Federal de Santa Catarina, Brazil 48 1 ) in Short Talks Stars & Stellar Systems SSS -3 Two rings but no fellowship: LoTr 1 and its relation to planetary nebulae possessing Barium central stars Tyndall, A. A.B1,2 ; Jones, D.2 ; Boffin, H. M. J.2 ; Miszalski, B.3,4 ; Faedi, F.5 ; Lloyd, M.1 ; Lopez, J. A.6 ; Martell, S.7 ; Pollacco, D.5 ; Santander Garcia, M.8 LoTr 1 is a planetary nebula thought to contain an intermediate-period binary central star system. The system shows the signature of a K-type, rapidly rotating giant, and most likely constitutes an accretion-induced post-mass transfer system similar to other PNe such as LoTr 5, WeBo 1 and A70. Such systems represent rare opportunities to further the investigation into the formation of Barium stars and intermediate period post-AGB systems – a formation process still far from being understood. Here, we present the first detailed analyses of both the central star system and the surrounding nebula of LoTr 1 using a combination of spectra obtained with VLT-FORS2, AAT-UCLES and NTT-EMMI, as well as SuperWASP photometry.We confirm the binary nature of the central star of LoTr 1 that consists of a K1 III giant and a hot white dwarf. The cool giant does not present any sign of s-process enhancement but is shown to have a rotation period of 6.4 days, which is a possible sign of mass accretion. Both LoTr 1 and A 70 also present broad double-peaked H↵ emission lines, whose origin is still unclear. The nebula of LoTr 1 consists in two slightly elongated shells, with ages of 17 000 and 35 000 years, respectively, and with different orientations. As such, LoTr 1 present a very different nebular morphology than A70 and WeBo 1, which may be an indication of difference in the mass transfer episodes. B 1 2 3 4 5 6 7 8 [email protected] Jodrell Bank Centre for Astrophysics, UK European Southern Observatory South African Astronomical Observatory South African Large Telescope University of Warwick, UK Instituto de Astronomia, Universidad Nacional Autonoma de Mexico Australian Astronomical Observatory Observatorio Astronómico National, Madrid 49 Stars & Stellar Systems Short Talks SSS -3 Search for Southern Galactic Be star candidates B. E. SabogalB1 ; A. Garcı́a-Varela2 ; R. E. Mennickent2 We present the result of a search for Galactic Be star candidates within the miscellaneous ASAS-2 Catalogue of Variable Stars. This search, performed using statistical, photometrical and morphological criteria, leads us to find 691 new southern Be star candidates. A comparison of photometric properties of these stars with those of Be star candidates in the Magellanic Clouds suggests that outbursting stars are more scarce in our Galaxy than in the Magellanic Clouds. We do not find stars showing clear high and low states similar to those detected in the Magellanic Clouds. Stars with periodic or quasi-periodic variations are more abundant than outbursting stars. The amplitudes of outbursts observed in our selected stars seem to confirm that the processes of mass ejection are less energetic in the higher metallicity environment of the Galaxy. B 1 2 [email protected] Universidad de los Andes, Departamento de Fı́sica, Cra. 1E No. 18A-10, Edificio Ip, A.A. 4976, Bogotá, Colombia Universidad de Concepción, Departamento de Astronomı́a, Casilla 160-C, Concepción, Chile 50 Short Talks Stars & Stellar Systems SSS -3 Viscous Disks in Be Stars B1 Rimulo, L. R. ; Carciofi, A. C.1 ; Mota, B. C.1 ; Haubois, X.2 ; Rivinius, T.3 The fast-spinning Be stars offer a testbed for developing and testing astrophysical theories in their limit. For the star proper, rapid rotation allows for studying the effects of rotation on the stellar evolution and structure. Recent interferometric studies of the photosphere, for instance, allowed for measuring the gravity darkening coefficient and the results present a challenge for current models. Be star phenomenology is strongly associated with their circumstellar disks. On one hand, the disk acts as a sink of angular momentum, and this fact couples the disk with the evolution of the central object. On the other hand, the disk reprocesses starlight, thereby modifying the emerging spectrum. In the past decade our understanding of these disks saw a major leap forward; with the very high angular resolution that can be achieved with modern interferometers we can now resolve the disk up to the immediate vicinity of the star, as well as determining the disk kinematical properties. Coupled with advancements in the physical modeling of these systems, these observations allowed for establishing the viscous decretion disk model as the most viable scenario for disk formation and evolution. In this model, material that is ejected with Keplerian or super-Keplerian speeds at the base of the star and diffuses outwards by means of viscous forces. More recently, models became available for the temporal evolution of these disks when subject to variable feeding rates. In this contribution we will discuss how these dynamical disk models can be used for constraining fundamental disk parameters, such as the alpha viscosity parameter, and we will report on an ongoing effort to model light curves of a large number of stars. B 1 2 3 [email protected] Universidade de São Paulo, Brazil Sydney Institute for Astronomy, Australia ESO, Chile 51 Stars & Stellar Systems Short Talks SSS -3 The Be star Achernar and its circumstellar environement Faes, D. M.B1,2 ; Carciofi, A. C.1 ; Domiciano de Souza, A.2 The circumstellar disks ejected by many rapidly rotating B stars (so-called Be stars) offer the rare opportunity to study the structure and dynamics of gaseous disks at high spectral as well as angular resolution. Recent works, largely based on optical long baseline interferometry, showed that Achernar (↵ Eridani, HD10144), the brightest (V = 0.46 mag) and nearest (distance of 42.5 pc) Be star is a key target to a deeper understanding of the physics of Be stars, because it displays most of features that characterizes the Be phenomenon: (i) Strong rotational rate; (ii) Residual disk; (iii) Episodic mass ejections; (iv) Quasi-cyclic disk formation/dissipation; (v) Polar wind; and (vi) Binarity. Here we present preliminary results for the recent history of Achernar. We use a large set of observational data, such as AMBER spectro-interferometry and PIONIER interferometry (VLTI/ESO), broad-band optical polarimetry (OPD/LNA) and multi-instruments spectroscopy. The radiative transfer code HDUST is used to analyze and interpret the observational dataset, aiming at obtaining a realistic physical model of the circumstellar environment (disk and/or wind) in interaction with the stellar photosphere. In particular, we analyse a preliminary inconsistency between Achernar’s 2009 AMBER and 2011 PIONIER interferometric data can be solved by the existence of a residual disk at the time of the first observations; this residual disk is compared with the disk at the active phase of 2003 and, after seven years of quiescense, the present active phase (2013). Lastly, a few words are given about the quasi-cyclic disk formation/dissipation and the binarity of the system. B 1 2 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Univ. of São Paulo Observatoire de la Côte d’Azur, Univ. de Nice-Sophia Antipolis 52 Short Talks Stars & Stellar Systems SSS -4 A kinematic study of the Lupus star-forming region Galli, P. A. B.B1 ; Bertout, C.2 ; Teixeira, R.1 ; Ducourant, C.3 To reliably determine the main physical parameters (mass and age) of young stellar objects a precise determination of the distance to individual stars is required. While the average distance to nearby star-forming regions (< 300 pc) is often known, the distances to individual stars are usually unknown. Most pre-main sequence stars were neither observed by the Hipparcos satellite due to their magnitude nor have any trigonometric parallax measured from the ground due to their distance. In this context, we investigate the kinematic properties of the Lupus association of young stars with the primary objective of deriving individual parallaxes for each group member. We identify those stars in the Lupus star-forming region that define the co-moving association of young stars using our new and improved convergent point search method that allows us to derive the precise position of the convergent point of a moving group and perform a membership analysis. We used published proper motion catalogs and searched the literature for radial velocities, which are needed to compute individual parallaxes via convergent point method. Our strategy also made it possible to distinguish Lupus stars from the adjacent Upper Centaurus Lupus (UCL) subgroup of the Scorpius-Centaurus association. Doing so, we derive individual parallaxes for 109 pre-main sequence stars and discuss the properties of the various Lupus subgroups and pre-main sequence subclasses. B 1 2 3 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo Institut d’Astrophysique de Paris Laboratoire d’Astrophysique de Bordeaux 53 Stars & Stellar Systems Short Talks SSS -4 A new library of theoretical stellar spectra for stellar population applications Coelho, P.B1 Libraries of stellar spectra are one of the main ingredients of stellar population synthesis models. Theoretical libraries have been increasingly used in recent years to overcome limitations of empirical libraries, in particular to explore parameter space (in temperatures, metalicities and abundance patterns) not well covered by empirical libraries. In this talk, a new theoretical stellar library is presented. It consists of high and low-resolution spectra which cover the parameter space required to the modelling of stellar populations between 30 Myr and 14 Gyr, metalicities Z between 0.0017 and 0.0048, at both solar-scaled and ↵-enhanced compositions. The characteristics of the library as well as comparisons to observations will be presented. B 1 [email protected] Universidade Cruzeiro do Sul 54 Short Talks Stars & Stellar Systems SSS -4 Improvement and analysis of the MILES library for stellar population modelling Milone, A.B1 ; Sansom, A.2 ; Vazdekis, A.3,4 ; Sánchez-Blázquez, P.5 ; Allende Prieto, C.3,4 ; Falcón Barroso, J.3,4 The main limitation of current semi-empirical SSP models is the use of spectra from solar neighbourhood stars, whose individual element abundances are not adequately considered. Typically only iron is taken as a metallicity tracer, but the spectral energy distributions of stars and stellar systems considerably depend on abundances of other metals (e.g. CNO group and ↵ elements). With the goal of assembling a new generation of SSP models with variable ↵-enhancement assuming Mg as a proxy, we obtained magnesium abundances with a precision of ⇠0.1 dex for nearly 80% of MILES stellar library (Mid-resolution Isaac Newton Telescope Library of Empirical Spectra). The [↵/Fe] abundance ratio is known as a good temporal scale indicator for the star formation since the ↵ and iron-group elements have distinct nucleosynthetic origins with different time scales (respectively type II and type Ia supernovae). The higher this ratio is, the shorter the time scale for stellar formation. The MILES library is being expanded by around 20% by including stars with known parameters and Mg abundances. The transformation of their photospheric parameters to the MILES homogeneous system was carried out, but the calibration of [Mg/Fe] is still in progress. In parallel, C, N and O abundances are also being compiled from published works for the library’s stars because these elements play an important role on the blue spectral region. The main motivation is to improve the distribution of stars over the parameter space (Tef f , log g, [Fe/H], [X/Fe]). We have also done careful comparisons of the theoretical stellar predictions of the Lick System line-strength indices against the MILES data. These comparisons reveal that the behaviour of Fe-sensitive line indices is generally well reproduced by the theoretical models, while other indices tend to show either some systematic offsets from the predicted relations or large scatter about them. We have thus been analysing this set of compiled empirical data to test synthetic models for stellar spectra used in population modelling. B 1 2 3 4 5 [email protected] Instituto Nacional de Pesquisas Espaciais (Brazil) University of Central Lancashire (UK) Instituto de Astrofı́sica de Canarias (Spain) Universidad de La Laguna (Spain) Universidad Autónoma de Madrid (Spain) 55 Stars & Stellar Systems Short Talks SSS -4 Estimating metallicities with isochrone fits done by global optimization to photometric data of open clusters Monteiro, H.B1 ; Oliveira, A. F.1 ; Dias, W. S.1 ; Caetano, T. C.1,2 The metallicity is a critical parameter that affects the correct determination fundamental characteristics stellar cluster and has important implications in Galactic and Stellar evolution research. Fewer than 10% of the 2174 currently catalog open clusters have their metallicity determined in the literature. In this work we present a method for estimating the metallicity of open clusters via non-subjective isochrone fitting using the cross-entropy global optimization algorithm applied to UBV photometric data. The free parameters distance, reddening, age, and metallicity simultaneously determined by the fitting method. The fitting procedure uses weights for the observational data based on the estimation of membership likelihood for each star, which considers the observational magnitude limit, the density profile of stars as a function of radius from the center of the cluster, and the density of stars in multi-dimensional magnitude space. We present results of [Fe/H] for nine well-studied open clusters based on 15 distinct UBV data sets. The [Fe/H] values obtained in the ten cases for which spectroscopic determinations were available in the literature agree, indicating that our method provides a good alternative to determining [Fe/H] by using an objective isochrone fitting. Our results show that the typical precision is about 0.1 dex. B 1 2 [email protected] IFQ, UNIFEI IAG, USP 56 Short Talks Stars & Stellar Systems SSS -4 Modeling photometric and spectroscopic data of HS 2231+2441: an HW Vir type system with a brown dwarf companion Almeida, L. A.B1,2 ; Daminelli, A.1 ; Rodrigues, C. V.2 ; Cieslinski, D.2 Stellar evolution is one of the most firmly established theories in modern Astrophysics. Precise values of fundamental parameters such as masses and radii of stars are crucial to test this theory to the level better than a few percent. As eclipsing binary systems provide a straightforward method for measuring these parameters, they play an important role in present observational efforts and theoretical developments. HW Vir type systems are an interesting class of eclipsing binaries with only a few known cases. These systems consist of a B subdwarf (sdB) plus a M dwarf (dM) in a compact orbit (Porb ⇠ 0.1 days). In this study we present an analysis of BVRC IC photometry and phase-resolved optical spectroscopy of the HW Vir type system HS 2231+2441. From the spectroscopic data analysis, we derived the radial velocity semi-amplitude, K1 = 38.7 ± 0.8 km/s of the sdB star. Modeling simultaneously the photometric and spectroscopic data with the Wilson-Devinney code, we obtained the geometrical and physical parameters of HS 2231+2441. With orbital period Porb ⇠ 2.65 h, inclination i = 80.9 ± 0.6 and mass ratio q = M2 /M1 = 0.177 ± 0.06, the components of the system have, M1 = 0.163 ± 0.06 M , M2 = 0.030 ± 0.006 M , R1 = 0.131 ± 0.005 R and R2 = 0.070 ± 0.005 R . We discuss these results in the context of HW Vir systems and their evolution. B 1 2 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas IAG/USP Instituto Nacional de Pesquisas Espaciais/MCTI 57 Stars & Stellar Systems Short Talks SSS -5 a observations of three globular clusters: NGC 104 NGC 6205 NGC 7099 Paunzen, E.1,2 ; Illiev, I. K.2 ; Pintado, O. I.B3 Globular clusters are main astrophysical laboratories to test and modify evolutionary models. Thought to be rather homogeneous in their local elemental distribution of members, new results suggest a wide variety of chemical peculiarities. The preselection of apparent peculiar stars for a detailed spectroscopic analysis is very important for globular cluster fields. Most regions are very dense and the target stars are, normally, very faint. Photometry could be one way out of the dilemma since it is very efficient. Up to now, only observations in the Johnson U BV (RI) and Strömgren uvby systems are able The tool of a photometry is employed in order to detect chemically peculiar Population II stars. This three filter narrow band system measures the flux distribution in the region from 4900 to 5600Å in order to find any peculiarities around 5200Å. The first a observations for 3 globular clusters: NGC 104, NGC 6205 and NGC 7099, give very promising results, which will serve as a solid basis for follow-up observations including photometric as well as spectroscopic studies. B 1 2 3 [email protected] Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic Rozhen National Astronomical Observatory, Institute of Astronomy of the Bulgarian Academy of Sciences, Smolyan, Bulgaria Instituto Superior de Correlación Geológica, Tucumán, Argentina 58 Short Talks Stars & Stellar Systems SSS -5 Dynamical Properties of Blue Straggler Stars in Galactic Globular Clusters: NGC3201, Omega Cen and NGC6218 Simunovic, M.B1,2 ; Puzia, T. H.1 Blue Straggler Stars (BSSs) have been shown to be promising indicators of the properties of their globular clusters. Their internal dynamics could help constraint their formation mechanisms, which are likely related to strong dynamical events occurring in the past, and therefore allowing for a direct test on the dynamical state of their parent globular clusters. We present the first dynamical study of BSSs in three Galactic globular clusters, NGC 3201, NGC 5139 (!Cen), and NGC 6218, based on medium-resolution spectroscopy (R ⇡ 10000) obtained with the Inamori-Magellan Areal Camera & Spectrograph (IMACS) mounted at the 6.5 meter Baade Magellan telescope. Our BSS candidate selection technique uses HST/ACS and ESO/WFI photometric data out to > 4.5 rc . We use radial velocity measurements to discard non-members and achieve a success rate of ⇠ 93%, which yields a sample of 116 confirmed BSSs. Using the penalized pixel fitting method (pPXF) we measure the v sin(i) values of the sample BSSs and find a bimodal v sin(i) distribution function in each globular cluster. About 90% of the BSS population in NGC 3201 and NGC 6218 exhibit values in the range 10 50 km s 1 , while ⇠ 80% of the BSSs in !Cen show v sin(i) values between 20 and 70 km s BSSs in NGC 3201 and NGC 6218 which show v sin(i) > 50 km s 1 1 . We find that the are all found in the central cluster regions, inside a projected 2 rc , of their parent clusters. We find a similar result in !Cen for BSSs with v sin(i) > 70 km s 1 which are all, except for two, concentrated inside 2 rc . In all globular clusters we find rapidly rotating BSSs that have relatively high differential radial velocities which likely put them on hyperbolic orbits, suggestive of strong dynamical interactions in the past. Based on stellar spin down and dynamical crossing timescales we estimate that all the observed rapidly rotating BSSs are likely to form in their central cluster regions no longer than ⇠ 300 Myr ago and may be subsequently ejected from their host globular clusters. Using dereddened V I colors of our photometric selection we show that blue BSSs in !Cen with (V I)0 < ⇠ 0.25 mag show a significantly increased v sin(i) dispersion compared with their red counterparts and all other BSSs in our sample, therefore strongly implying that fast rotating BSSs are preferentially bluer, i.e. more massive. This may indicate that this particular blue BSS population in !Cen was formed in an unique formation event and/or through an unique mechanism. B 1 2 [email protected] Instituto de Astrofisica, Pontificia Universidad Catolica de Chile Astronomisches Rechen-Institut, Heidelberg University 59 Stars & Stellar Systems Short Talks SSS -5 Metallicity effects on globular clusters: size and colour Sippel, A. C.B1,2 ; Hurley, J. R.2 While it has been known for a long time that the sizes of globular clusters within our galaxy correlate to their galactocentric distances, more recently it has also been found that blue, metal-poor clusters are on average larger than red, metal-rich clusters in nearby galaxies. This has generated a debate on the origin of these size differences. Using direct N-body simulations of globular clusters with different metallicities, we can distinguish between structural and apparent (i.e. mass versus light) differences. We find that metallicity does not affect the cluster structure, while metallicity alone can produces apparent size differences as observed. In addition, we can trace the evolution of colour with time, which enables us to follow the evolution of a dynamically evolved single stellar population. B 1 2 [email protected] ESO Santiago, Chile Centre for Astrophysics and Supercomputing, Swinburne University, Melbourne Australia 60 Short Talks Stars & Stellar Systems SSS -5 R-Process Abundances in Metal-Poor Galactic Halo Stars Siqueira-Mello, C.B1 ; Barbuy, B.1 ; Spite, M.2 ; Spite, F.2 The origin of the elements is a fundamental field in modern astrophysics, and the problem of the heavy elements has been gaining attention in recent decades. The site of the r-process production is not yet fully identified: the most likely sites are high-entropy neutrino-driven winds of neutron-rich matter in core-collapse supernova, but alternative sites have been suggested, as the merging of two neutron stars or the merging of a neutron star and a black hole. The origin of the lightest trans-Fe elements gallium through cadmium adds another difficulty to this picture, since it has been attributed in varying degrees to several processes. Observed abundances are the best clues to bring some light to this multiplicity of possible mechanisms, and the extremely metal-poor (EMP) Galactic halo stars have a special role in this problem. In this contribution we describe the results obtained with the EMP r-II star CS31082-001 in the frame of the ESO Large Programme ”First Stars”. Most of the heavy elements are present in the ultraviolet (UV), and for some of them only this spectral region has measurable lines. Using HST/STIS observations we provide abundances for those elements, making this star the most complete r-II object studied, with a total of 37 detections of neutron-capture elements. The analysis of the isotopic abundances is another approach to the problem. Example of that are the isotopic fraction measurements of barium in the well studied metal-poor halo subgiant star HD 140283, which indicates a 100% contribution by the s-process in recent literature, in contradiction with the Truran’s theory since the metallicity of HD 140283 ([Fe/H]=-2.50±0.20) indicates presumably the absence of s-process contribution.We present the solution of this twenty years long-standing problem with a genuine detection of europium in HD 140283, in agreement with the prevision of a strong r- process contribution for the origin of the heavy elements, showing that it is necessary to be careful with results obtained from isotopic analysis. The study of r-I stars is a third interesting approach to the heavy elements problem. At least twice as common as their extreme counterparts, the r-II stars, in this contribution we present the results obtained from a sample of this class of stars, showing the place they have to help us solving this problem. Conclusions and perspectives will be also presented. B 1 2 [email protected] IAG, Universidade de Sao Paulo GEPI, Observatoire de Paris 61 Stars & Stellar Systems Short Talks SSS -6 Primera identificación astrométrica y espectrofotométrica de miembros de Bochum 7 Corti, M. A.B1,2 ; Orellana, R. B.1,3 ; Bosch, G. L.1,3 Una asociación OB es un grupo de estrellas jóvenes (edad  50 ⇥ 106 años) con tipos espectrales O y B, de baja densidad, originado en una gran nube molecular. La importancia de su estudio radica en la interacción entre la componente estelar y las varias fases gaseosas del medio interestelar, ya sea por creación de cáscaras de HI o fenómenos globales como pueden ser el enriquecimiento de la galaxia por explosiones de supernovas. Se les adjudica también a estas estrellas de alta temperatura y luminosidad, ser buenas trazadoras de los brazos espirales de la galaxia. Este trabajo tiene como objetivo continuar y profundizar el conocimiento de la composición estelar de la asociación OB conocida como Bochum 7 (Moffat & Vogt, 1975, A&AS, 20, 85; Lundstrom & Stenholm, 1984, A&AS, 58, 136; Sung et al. 1999, JKAS, 32, 109; Corti et al. 2007, A&A, 467, 137). La misma se encuentra en una zona de relativamente baja extinción en el tercer cuadrante del plano galáctico, a una distancia de entre 4 y 6 kpc. En el caso de grupos estelares ubicados a distancias superiores al kiloparsec, la determinación de miembros se vuelve extremadamente compleja, necesitando aplicar varias técnicas con el fin de obtener resultados confiables. En este trabajo, mostraremos cuan potente es investigar a los miembros de una asociación estelar empleando para ello técnicas astrométricas y astrofı́sicas, simultáneamente. La búsqueda astrométrica se realiza utilizando los datos del catálogo UCAC4 y empleando el método de Orellana et al. (2010, A&A, 521, A39) para separar los miembros de la asociación de las estrellas de campo. Luego, se prosigue efectuando un análisis al grupo astrométrico, empleando datos fotométricos y espectroscópicos propios y de bases de datos, obteniendo con ello el listado final de miembros de Bochum 7. Del estudio de las caracterı́sticas fı́sicas de cada uno de sus miembros, finalmente resulta posible conocer las componentes del movimiento propio medio, edad, distancia, velocidad radial media, etc., de la asociación OB Bochum 7. B 1 2 3 [email protected] Facultad de Ciencias Astronómicas y Geofı́sicas, Universidad Nacional de La Plata, Argentina Instituto Argentino de Radioastronomı́a (CCT-La Plata, CONICET), Argentina Instituto de Astrofı́sica de La Plata (CCT-La Plata, CONICET), Argentina. 62 Short Talks Stars & Stellar Systems SSS -6 A photometric study of M67: anchoring measurements for the determination of astrophysical parameters of bright stars Dalle Mese, G.B1 ; Lopez-Cruz O.1 ; Schuster, W.2 ; Chavarria, C.2 ; Garcia, G2 We present the photometric analysis of the stars in M67 open cluster. We have performed uvby-Hbeta Stromgren observations using the OAN-SPM 84 cm telescope + CCD and 1.5 m + Danish Spectrophotometer. We have compared our photometric measurements with CHORIZOS (Maiz-Apellaniz, J. 2004) in order to generate stellar physical parameters and the age of the cluster is modeled with the Dartmouth Stellar Evolution Database (Dotter et al., 2008). This is the first result of a comprehensive photometric program carried out in SPM for the generation of a set of secondary standards for the Stromgren system B 1 2 [email protected] Instituto Nacional de Astrofisica, Optica y Electronica Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, sede Ensenada 63 Stars & Stellar Systems Short Talks SSS -6 The GALEX Nearby Young-Star Survey B1 Rodriguez, David R. ; Zuckerman, B.2 ; Kastner, Joel H.3 ; Bessell, M. S.4 ; Faherty, Jacqueline K.1,5,6 ; Murphy, Simon J.7 ; Vican, Laura2 Over the last few decades, many 10-100 Myr-old stars have been identified in moving groups located closer than 100 parsecs to Earth. For direct imaging searches of extrasolar planets these stars represent the best targets and they will be continuously observed during the coming decades as new imaging systems and larger telescopes are commissioned. Recent work has shown that near-IR surveys, like 2MASS, combined with ultraviolet data from GALEX can be used to identify additional members in these moving groups. In particular, this methodology is well suited to searching for low-mass stars, which are generally lacking in moving group member statistics. Initial searches for young stars relied on optical identification (such as with Tycho and Hipparcos) and X-ray detection with ROSAT. The release of the all-sky WISE catalog has opened up a new frontier in the search for nearby, young, low-mass stars. We have carried out an all-sky cross correlation between the GALEX, WISE, and 2MASS databases and identified many candidate young, low-mass stars on the basis of their ultraviolet and near-IR colors as well as kinematic information. Early spectroscopic results confirm the youthful nature of our candidates. This suggests that our technique is capable of identifying the many low-mass stars that remain to be found among the nearby young moving groups. B 1 2 3 4 5 6 7 [email protected] Universidad de Chile University of California, Los Angeles Rochester Institute of Technology Australian National University American Museum of Natural History Carnegie Department of Terrestrial Magnetism Astronomisches Rechen-Institut, University of Heidelberg 64 Short Talks Stars & Stellar Systems SSS -6 The Gaia-ESO Survey: detailed abundances for thousands of FGK-type stars Smiljanic, RodolfoB1 The Gaia-ESO Survey (GES) is an ambitious public spectroscopic survey that is obtaining medium- and highresolution spectra of more than 105 stars with the FLAMES multi-fiber facility at the VLT. Giraffe mediumresolution spectra will be obtained for ⇠ 105 stars and high-resolution UVES spectra will be obtained for about 5 000 stars. The targets have been selected to cover all major components of the Galaxy (the halo, the thick and thin disks, and the bulge) and a significant sample of open clusters (⇠100) covering different ages, masses, and distances. The ambitious ultimate goal is to provide detailed distribution functions of kinematics and element abundances for stars in all Galactic components, giving a detailed view of the formation and evolution history of the Galaxy. In this talk, I will introduce the Survey and its goals, with emphasis on the sample of more than 5 000 FGK-type stars that is being observed in the solar neighbourhood and in open clusters. I will discuss how the spectra are being analysed and which data products will be made available to the community through annual public releases. Finally, I will also present some examples of early science results obtained with Survey data. B 1 [email protected] Nicolaus Copernicus Astronomical Center, Torun, Poland 65 Stars & Stellar Systems Short Talks SSS -6 The WFCAM Variable Star Catalog and New Variability index Ferreira Lopes, C. E.B1 ; Dekany, I.2 ; Catelan, C.2 ; Angeloni, R.2 ; De Medeiros, J. R.1 WFCAM is the wide-field near-infrared camera of the 3.8m United Kingdom Infrared Telescope (UKIRT), designed to be capable of carrying out ambitious large-scale survey programs such as the UKIRT Infrared Deep Sky Surveys that show photometric data in at least 8 bands (Y,Z,J,H,K,H2,nBr,nbj). This data is showing a ”treasures data” to analyse varibility source in infrared. In this way, we present the catalog with 245 identified variable stars shown its characteristics from a data miner’s point of view. We found a total of 49 stars that were already known from previous studies: in particular, 28 sources are included in the NSVS catalog and, among them, 3 are also GCVS objects (i.e., AM Tau, EH Lyn, UV Vir – an Algol-type eclipsing binary, a contact binary, and a RRab Lyrae, respectively). In the other side, the tremendous development in astronomical instrumentation have been giving rise to several synoptic surveys of increasing scale of data thus requiring that there was an improvement of the tools of data analysis. So, we present a set of new variability indices that shown be three times more efficient than Stetson index. Moreover, these variability indices represents a new look at the time series data from view point from signal correlation among the subset of data. B carlos [email protected] DFTE, Universidade Federal do Rio Grande do Norte, Natal, RN, 59072-970 Brazil 2 Departamento de Astronomı́a y Astrofı́sica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile 1 66 Short Talks Stars & Stellar Systems VVV-1 The VVV Survey D. MinnitiB1 ; VVV Science Team The Vista Variables in the Via Lactea Survey (VVV) is a public near-IR variability survey scanning the Milky Way bulge and an adjacent section of the disk. The main goal of the VVV Survey is to map the 3D structure of the Galactic bulge and decide among different models of bulge formation. The survey will take 193 nights of observations with the ESO 4-m VISTA telescope between 2010 and 2016, covering a billion point sources across an area of 540 deg2 . The final product will be a deep near-IR atlas in the YZJHKs passbands (0.9-2.5 µm), and a catalogue of more than a million variable point sources. The Survey has already produced a number of scientific results and discoveries that will be presented in this talk. B 1 [email protected] P. Universidad Catolica de Chile 67 Stars & Stellar Systems Short Talks VVV-1 Variable stars in the VVV globular clusters Alonso-Garcı́a, J.B1,2 ; Dékány, I.1,2 ; Catelan, M.1,2 ; Contreras, R.1,2 ; Minniti, D.1,2,3 The VVV survey is observing the central regions of our Galaxy in the near-infrared, where the extinction is highly diminished, in several epochs. Numerous inner Galactic globular clusters fall inside the area covered by the VVV survey. Most of these clusters, especially the faintest ones, have been poorly studied due to the presence of severe extinction and high stellar densities in the field. We will present the first results of a search for variable stars we are conducting in these clusters. Our main aim is to obtain a better determination of the physical parameters of these globular clusters using the information provided by their variables. B 1 2 3 [email protected] Instituto de Astrofı́sica, Facultad de Fı́sica, Pontificia Universidad Católica de Chile, Santiago, Chile The Milky Way Millennium Nucleus, Santiago, Chile Vatican Observatory, Vatican City State, Italy 68 Short Talks Stars & Stellar Systems VVV-1 Searches for variability in the Milky Way bulge with the VVV Survey R. K. SaitoB1 ; D. Minniti2,3,4 ; F. Gran2 ; D. Iglesias2 ; G. Muro2 ; I. Dekany2,3 The Vista Variables in the Via Lactea (VVV) is an ESO public near-IR variability survey scanning the Milky Way bulge and southern Galactic disk. VVV is producing a ZYJHKs catalogue of about a billion sources over an area of 562 square degrees and upon completion will deliver Ks-band light-curves for a few million variable sources with 80-100 data-point covering many years. Data taken during 2010-2012 covered the whole VVV bulge area in the five passbands, plus up to 30-40 Ks-band epochs with a large baseline. This data set allow us to search for variability in the Galactic bulge using different strategies. In this talk we will summarize the first results from this search, from the study of tiny variations due to planetary transits, until the discovery of hundreds of long period variables, and the detection of microlensing events and explosive Galactic Nova eruptions. B 1 2 3 4 [email protected] Departamento de Fisica, Universidade Federal de Sergipe Instituto de Astrofisica, Pontificia Universidad Catolica de Chile The Milky Way Millennium Nucleus Vatican Observatory 69 Stars & Stellar Systems Short Talks VVV-1 The general catalog of VISTA variables in the Via Lactea Istvan DekanyB1 ; Joyce Pullen; Dante Minniti; Marcio Catelan The VISTA Variables in the Via Lactea (VVV) ESO Public Survey is providing deep, long-baseline timeseries photometry in the near-infrared for hundreds of millions of objects in the bulge and the southern disk. The scientific potential of these data is manifold, and its global exploration requires homogeneous and high-level data products. In my talk, I will expound on the details of a massive computational effort to produce a general variability database and a catalog of periodic and transient variables in the bulge, using photometry provided by the VISTA Data Flow System. The goal of this project is to duly provide science-ready data products in the form of a simple on-line database which may serve as the basis for various specific studies from stellar pulsation to microlensing, conducted by the VVV community. I will discuss the main steps of the procedure, the characteristics and possible uses of the database, the current status of the project, and will conclude by highlighting selected results. B 1 [email protected] Instituto de Astrofisica, Pontificia Universidad Catolica de Chile 70 Short Talks Stars & Stellar Systems SSS -7 A new insight to the O Vz stars within the framework of the GOSS Survey Arias, J. I.B1 ; Maı́z Apellániz, J.2 ; Barbá, R. H.1 ; Walborn, N. R.3 ; Sota, A.2 ; Morrell, N. I.4 ; Alfaro, E.2 ; Gamen, R. C.5 Based on high-S/N observations from both hemispheres, the Galactic O-Star Spectroscopic Survey (GOSSS) is the largest collection of O-star optical spectra ever assembled. Because of the quality, quantity, and homogeneity of the data, this survey has produced several systemic developments and revisions, some of them unexpected, for the massive hot stars. Beside having improved the definition of the spectral-classification system, GOSSS is revealing numerous objects and categories of special interest, also allowing their statistical study. The present work constitutes a further example. It is focused on the Galactic members of the Vz luminosity class, in which He II 4686 absorption is stronger than any other He II or He I lines. This characteristic has been hypothesized to be a signature of the extreme youth of the objects, as the stellar winds responsible for the emission filling of the former line would be less developed than even at class V. We investigate systematically the Galactic O Vz stars, finding a number of curious effects regarding their distribution as a function of spectral type. The definition of what it means to be an O Vz star, along with the astrophysical significance of this category, is also rediscussed. B 1 2 3 4 5 [email protected] Universidad de La Serena, Chile Instituto de Astrofı́sica de Andalucı́a, España Space Telescope Science Institute, USA Las Campanas Observatory, Chile Universidad Nacional de La Plata, Argentina 71 Stars & Stellar Systems Short Talks SSS -7 OWN Survey: results after seven years of high-resolution spectroscopic monitoring of Southern O and WN stars Barba, R. H.B1 ; Gamen, R.2 ; Arias, J.1 ; Morrell, N. I.3 ; Walborn, N.4 ; Maiz Apellaniz, J.5 ; Alfaro, E.5 ; Sota, A.5 The high-resolution spectroscopic monitoring survey of O and WN stars (OWN Survey) has completed seven years of continuous campaigning, using observational facilities of Chile and Argentina. The sample was selected corresponds to those stars for which there is no indication of multiplicity in the Galactic O-star Catalog (Maiz Apellaniz et al. 2004) and the VII Catalogue of Galactic WR stars (van der Hucht 2000). We have collected over 4000 spectra of about 200 O and WN stars which has allowed us to discover 126 stars showing radial variations greater than 10 km/s. From these stars: 101 new systems, being 53 single-lined spectroscopic binaries, 40 double-lined spectroscopic binaries, and 8 multiple-lined binaries. The new orbital periods spanning from 1.5 to 2200 days. In this work, we present the main result of ”OWN Survey”: the determination of orbits for over forty O-type spectroscopic binary systems. This result is unprecedented in the context of massive binary stars, since we almost doubling the number of systems with known orbits. We analyse the distribution of orbital elements, mass function, mass ratio, spectral types, etc. B 1 2 3 4 5 [email protected] Universidad de La Serena Instituto de Astrofisica La Plata - CONICET Las Campanas Observatory Space Telescope Science Institute Instituto de Astrofisica de Andalucia - CSIC 72 Short Talks Stars & Stellar Systems SSS -7 Overview of Stellar Interferometry and its contribution to the study of massive stars Kanaan, S.B1 ; Meilland, A.2 ; Millour, F.2 ; Cure, M.1 ; Chesneau, O.2 ; Borges, M.3 ; Cidale, L.4 ; Arcos, C.1 This talk is an overview of stellar interferometry applied to Be and B[e] phenomena. Hot Active stars are an important source of UV photons that are ionizing the circumstellar and interstellar environment up to a few hundred of parsecs. Thus, they are playing an important role in the heating of the gas in the arms of galaxies as well as the formation of radiative shocks in the interstellar medium. These stars are very bright and over luminous compared to B “normal” stars due to the presence of their circumstellar envelope. Thus, in young clusters, with many Be stars, the luminosity function may seem to contain too massive stars, leading to an artificially top-heavy Initial Mass Function (IMF). The lack of angular resolution in observations limited the study of these objects and their modelling was based only on fitting the SED or line profiles. To discriminate between the various physical processes describing the mass loss and the distribution of matter in the circumstellar medium, the geometry and the kinematics of these envelopes have to be fully constrained. This cannot be done by a single telescope and long-baseline interferometry is the only available technique to reach the spatial resolution necessary to resolve most of the envelopes. The VLTI instruments AMBER and MIDI and the upcoming instruments such as MATISSE and GRAVITY are perfectly adapted to the study of these gaseous and dusty environments as their flux is generally dominated by circumstellar emission beyond 1 µm. Using interferometry with high resolution spectra allow us to use the differential visibility and differential phase. In fact disks in rotation or in expansion have the same spectroscopic profile which make it impossible to descriminate between these two scenarios. On the other hand these scenarios have there own signature in the differential visibility and phase. Performing many interferometric observations, with different baselines lengths and position angle, will allow us to reconstruct images with softwares such as MIRA. The advantage of the image reconstruction lies in the fact that it is independent from any model. Moreover using image reconstruction could reveal the flattening of the envelope, asymmetries in the disk such as spiral arm, clumpiness or binarity. B 1 2 3 4 [email protected] Universidad de Valparaiso, departamento de fisica y astronomı́a Laboratoire Lagrange, Universite de Nice Sophia-Antipolis, CNRS, Observatoire de la Cote d’Azur Observatorio Nacional, Rio de Janeiro Instituto de Astrofısica de La Plata, CCT-La Plata, CONICET & Facultad de Ciencias Astronomicas y Geofisicas, UNLP 73 Stars & Stellar Systems Short Talks SSS -7 Integral Field Unit spectroscopy of supernova host galaxies B1,2 Lluı́s Galbany ; Vallery Stanishev1 ; Ana Mourão1 ; Myriam Rodrigues3 ; Hector Flores4 ; CALIFA Collaboration We used optical IFU spectroscopy of nearby SN host galaxies (0.005 < z < 0.03), obtained by the CALIFA Survey and from previous observations, in order to look for correlations between the SN type and the environmental parameters at the location of the explosion. After subtracting the stellar continuum emission, we produced spatially resolved maps of several ionized gas emission lines and stellar population parameters. We found differences in the galactocentric distances distributions in a sequence from Ibc to Ia, being type II in the middle of those. After selecting the nearest HII region we found core collapse SNe tending to explode closer than SNe Ia. This can be explained by differences in ages and masses among the parent stellar populations of the progenitors of different SN types. In addition, we also found slightly differences in the local elemental abundances of type Ibc and type Ia compared to type II SNe. Once distances are normalized to the effective radius, the metallicity gradient seems to be universal, and differences between the value at the SN position and that obtained from the gradient can be established. We finally compared the values measured at the galaxy core, SN position, and co-adding all the galaxy emission, finding significant differences among them, especially for SNe Ia, which tend to explode in metal-rich environments. B 1 2 3 4 [email protected] CENTRA - Centro Multidisciplinar de Astrofı́sica, Instituto Superior Técnico, Av. Rovisco Pais 1, 1049-001 Lisbon, Portugal Departamento de Astronomı́a, Universidad de Chile, Casilla 36-D, Santiago, Chile European Southern Observatory, Alonso de Cordova 3107 Casilla 19001 - Vitacura -Santiago, Chile GEPI, Observatoire de Paris, UMR 8111, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France 74 Short Talks Stars & Stellar Systems SSS -7 Subluminous type Ia supernovae Gonzalez-Gaitan, S.B1 We present a thorough photometric and spectroscopic study of a large sample of subluminous type Ia supernovae (SNe Ia) comparing them to the normal type Ia population. Subluminous SNe Ia are characterized by strong Ti II and enhanced Si II lines, they are fainter, redder and have fast evolving light-curves. Due to their outlying differences they have been left out of cosmological studies but they are key to understand SNIa progenitors. We show that subluminous SNe Ia can be clearly identified via spectroscopic but also purely photometric techniques of current and upcoming surveys, and we present some of their key features that enable us to characterize their progenitor systems. B 1 [email protected] Departamento de Astronomia, Universidad de Chile 75 Stars & Stellar Systems Short Talks SSS -8 Supernova remnants colliding with molecular clouds: From high- to low-energy interactions Montmerle, T.B1 It is now well established that a class of gamma-ray sources in the galactic plane, especially in the TeV range as seen by HESS and other Cerenkov telescopes, and in the GeV range by the Fermi and AGILE satellites, is associated with intermediate-age supernova remnants interacting with molecular clouds in massive starforming regions. After a brief general introduction linking high-energy gamma-rays and cosmic rays, I will focus on a few such gamma-ray sources (W28, W44, and W51) and the challenging conclusions that can be drawn from them. I will then describe our recent work on related submm measurements and implications of enhanced ionizing effects in molecular clouds due to locally accelerated low-energy cosmic rays. B 1 [email protected] Institut d’Astrophysique de Paris, France 76 Short Talks Stars & Stellar Systems SSS -8 A new class of type Ia Supernovae Pignata G.B1 ; Taubemberger S.2 ; Kromer, M.2 ; Pakmor R.3 I will present evidences for a new class of type Ia SNe which have low luminosity, red colors and absence of a secondary maximum typical of sub-luminous type Ia SNe but display a slow rice to maximum and also a slow post-maximum decline which place them completely out of standard light curve width-luminosity relation of SNe Ia. This study starts from the observational campaign on SN2010lp carried out by the Millennium Center for Supernova Science (MCSS), but subsequently include other peculiar SNe Ia from the literature which display similar photometric and spectroscopic properties. SN2010lp is the first ever observed type Ia SN showing oxygen emission line on its nebular spectrum. The [0I] features has a complex profile with a broad base and two narrow emission peaks superimposed which suggests that oxygen is distributed in a non-spherical region close to centre of the ejecta. The latter pointed to a violent merger of two white dwarf (Pakmor et al. 2012,2013) as the most promising scenario for this SN. Base on this explosion model we generate, through a complete radiative transfer simulations, light curve and spectra at the photospheric phase which match quite well the observed light curve and spectra of SN2010lp reinforcing the hypothesis this SN and probably the other peculiar SNe Ia we consider in this study come for this progenitor channel. B 1 2 3 [email protected] Universidad Andrés Bello Max-Planck-Institut für Astrophysik Heidelberger Institut für Theoretische Studien 77 Stars & Stellar Systems Short Talks SSS -8 Recurrent solar coronal jets induced by magnetic emergence Y. Guo1,2 ; P. Démoulin3 ; B. Schmieder3 ; M. D. Ding1,2 ; S. Vargas Domı́nguezB4 ; Y. Liu5 Jets of plasma are frequently observed in the solar corona. A self-similar recurrent behavior is observed in a fraction of them. These jets are thought to be a consequence of magnetic reconnection, however, the physics involved is not fully understood. Therefore, we study some jet observations with unprecedented temporal and spatial resolutions with data from the Solar Dynamics Observatory (SDO). We derive the magnetic flux evolution, the photospheric velocity field, and the vertical electric current evolution. The magnetic configuration before the jets is derived by the nonlinear force-free field (NLFFF) extrapolation. Three EUV jets recurred in about one hour on 2010 September 17 in the following magnetic polarity of active region 11106. We derive that the jets are above a small magnetic bipole which is continuously driven by photospheric diverging flows. The interaction drove the build up of electric currents that we indeed observed as elongated patterns at the photospheric level. For the first time, the high temporal cadence of HMI allows to follow the evolution of such small currents. In the jet region, we found that the integrated absolute current peaks repetitively in phase with the 171 Å flux evolution. The photospheric current pattern of the jets is found associated to the quasi-separatrix layers deduced from the magnetic extrapolation. From previous theoretical results, the observed diverging flows are expected to build continuously such currents. We conclude that magnetic reconnection occurs periodically, in the current layer created between the emerging bipole and the large scale active region field. It induced the observed recurrent coronal jets and the decrease of the vertical electric current magnitude. B 1 2 3 4 5 [email protected] School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, China LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France Departamento de Fı́sica, Universidad de Los Andes, A.A. 4976, Bogotá, Colombia W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA 78 Short Talks Stars & Stellar Systems SSS -8 Mass extinctions, galactic orbits in the solar neighborhood and the Sun: a connection? Gustavo F. Porto de MelloB1 ; Wilton S. Dias2 ; Jacques Lépine3 ; Diego Lorenzo-Oliveira1 ; Rodrigo Kazu Siqueira4 The orbits of the stars in the disk of the Galaxy, and their passages through the Galactic spiral arms, are a rarely mentioned factor of biosphere stability which might be important for long-term planetary climate evolution, with a possible bearing on mass extinctions. The Sun lies very near the co-rotation radius, where stars revolve around the Galaxy in the same period as the density wave perturbations of the spiral arms. Conventional wisdom generally considers that this status makes for few passages through the spiral arms. Controversy still surrounds whether time spent inside or around spiral arms is dangerous to biospheres and conducive to mass extinctions. Possible threats include giant molecular clouds disturbing the Oort comet cloud and provoking heavy bombardment; a higher exposure to cosmic rays near star forming regions triggering increased cloudiness in Earth’s atmosphere and ice ages; and the destruction of Earth’s ozone layer posed by supernova explosions. We present detailed calculations of the history of spiral arm passages for all 212 solar-type stars nearer than 20 parsecs, including the total time spent inside the spiral arms in the last 500 Myr, when the spiral arm position can be traced with good accuracy. We found that there is a large diversity of stellar orbits in the solar neighborhood, and the time fraction spent inside spiral arms can vary from a few percent to nearly half the time. The Sun, despite its proximity to the galactic co-rotation radius, has exceptionally low eccentricity and a low vertical velocity component, and therefore spends 30% of its lifetime crossing the spiral arms, more than most nearby stars. We discuss the possible implications of this fact to the long-term habitability of the Earth, and possible correlations of the Sun’s passage through the spiral arms with the five great mass extinctions of the Earth’s biosphere from the Late Ordovician to the Cretaceous-Tertiary. B 1 2 3 4 [email protected] Observatório do Valongo, Universidade Federal do Rio de Janeiro Instituto de Ciências Exatas, Universidade Federal de Itajubá Instituto Astronômico, Geofı́sico e de Ciências Atmosféricas, Universidade de São Paulo Instituto Carlos Chagas Filho de Biofı́sica, Universidade Federal do Rio de Janeiro 79 Stars & Stellar Systems Short Talks VVV-2 Reddening-Free Indices in the VISTA Filter System Catelan, M.B1 ; Leyton, P. Accurate interstellar extinction values represent one of the most important items in every astronomer’s wish list. Unfortunately, extinction is notoriously difficult to measure, and thus represents a serious challenge in the era of high-precision astronomy. In this sense, reddening-free indices can be of considerable astrophysical importance, as they allow analysis of several problems without the need for accurate foreground reddening values. In this paper, we describe our efforts towards generalizing the reddening-free indices in the VISTA filter system that were first defined in Catelan et al. (2011), by evaluating their dependence on spectral type and luminosity class. B 1 [email protected] Pontificia Universidad Catolica de Chile, Instituto de Astrofisica 80 Short Talks Stars & Stellar Systems VVV-2 Near-Infrared Photometric Parameters of Galactic Globular Clusters From the VVV Survey Cohen, R. E.B1 ; Mauro, F.1 ; Moni Bidin, C.1 ; Geisler, D.1 ; Villanova, S.1 We present results from near-infrared photometry of Galactic globular clusters located towards the Galactic bulge from the Vista Variables in the Via Lactea (VVV) survey. In light of updated spectroscopic abundance information, correlations between photometric parameters and cluster metallicities are examined and compared to predictions from evolutionary models, with the large survey area permitting statistical field star decontamination. These data are supplemented with additional high spatial resolution optical and infrared photometry, facilitating not only photometric analyses over a broad color baseline, but also new constraints on the reddening and reddening law in the direction of these clusters as well as their structural parameters. B 1 [email protected] Universidad de Concepcion 81 Stars & Stellar Systems Short Talks VVV-2 Study of Young Stellar Clusters in the Nebular Complex NGC6357 with VVV Lima, E. F.B1 ; Bica E.1 ; Bonatto C.1 ; Saito R. K.2 NGC 6357 is a very active star-forming complex seen in the optical as an extensive H II region located in the Sagittarius spiral arm. We are studying several star clusters in NGC 6357 doing a matching of the 2MASS and VVV data. The 2MASS data were used for the brightest objects (Ks < 11 mag), while VVV was used for the fainter objects. To disentangle field and cluster stars we employed the statistical decontamination algorithm described in Bonatto & Bica 2010. Our analysis has provided a preliminary view of the Colour Magnitude Diagrams (CMD) and density structure of these objects, and also basic information about the behavior of the interstellar medium in the complex. B 1 2 [email protected] Universidade Federal do Rio Grande do Sul - Brazil Universidade Federal de Sergipe - Brazil 82 Short Talks Stars & Stellar Systems VVV-2 Proper motions and brown dwarfs in the VVV survey B1 Beamı́n, J. C. ; Minniti, D.1,2,3 ; Gromadzki, M.4 ; Kurtev, R.4 ; Ivanov, V. D.5 ; Lucas, P.6 ; Saito, R. K.7 ; Borissova, J.4 The Vista Variables in the Vı́a Láctea (VVV) survey is a deep multi wavelength, multi-epoch, Near infrared survey of the Galactic inner disk and bulge covering 560deg2 in the sky. We started a search for High Proper Motions -HPM ( PM>0.1 ”/yr) objects in the VVV database, using the Ks band observations from 2010 until 2012. We have found and recovered hundreds of HPM objects. Our studies are complementary to other HPM surveys, especially considering we target very crowded and heavily extincted regions, also our survey is particularly sensitive to detect low mass stars, ultra cool dwarfs because of the use of deep near-IR data. The higher spatial resolution and multi-epoch data, help us to reveal HPM objects that were hidden by confusion with background sources in previous observations. As an example of the success of this approach we present the first brown dwarf discovered in the VVV survey, an unusually blue L dwarf at 17.5 pc of the Sun (Beamı́n et al. 2013 submitted). VVV data also allows us to calculate parallaxes of nearby objects up to ⇠20-30 pc. B [email protected] Instituto de Astrofı́sica, Facultad de Fı́sica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile 2 The Milky Way Millennium Nucleus, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile 3 Vatican Observatory, Vatican City State V-00120, Italy 4 Departamento de Fı́sica y Astronomı́a, Facultad de Ciencias, Universidad de Valparaı́so, Ave. Gran Bretaña 1111, Playa Ancha,Valparaı́so Chile 5 European Southern Observatory, Ave. Alonso de Cordoba 3107, Casilla 19001, Santiago, Chile 6 Centre for Astrophysics Research, Science and Technology Research Inst., University of Hertfordshire, Hatfield AL10 9AB, UK 7 Universidade Federal de Sergipe, Departamento de Fı́sica, Av. Marechal Rondon s/n, 49100-000, São Cristóvão, SE, Brazil 1 83 Stars & Stellar Systems Short Talks VVV-2 Weather on Other Worlds: Brown Dwarf variability and VVV B1 Kurtev, R. ; Metchev, S.2 ; Heinze, A.2 ; Gromadzki, M.1 ; Ivanov, V. D.3 ; Minniti, D.4 ; Beamin, J. C.4 ; Borissova, J.1 L/T transition brown dwarfs present large-amplitude variability on rotational timescales. Photometric monitoring from warm Spitzer reveals that the L3 dwarf DENIS-P J1058.7-1548 varies sinusoidally in brightness with a period of ⇠4.25 hr and an amplitude of ⇠0.4% (peak-to-valley) in the 3.6µm band, confirming the reality of a 4.3±0.3hr periodicity detected in J-band photometry from the SOAR telescope. The J-band variations are a factor of 2.2±0.3 larger in amplitude than those at 3.6µm, while 4.5µm Spitzer observations yield a 4.5/3.6µm amplitude ratio of only 0.23±0.15, consistent with zero 4.5µm variability. This wide range in amplitudes indicates rotationally modulated variability due to magnetic phenomena and/or inhomogeneous cloud cover. However, inhomogeneous cloud cover alone can explain all our observations, and our data align with theory in requiring that the regions with the thickest clouds also have the lowest effective temperature. DENIS-P J1058.7-1548 is only the first of nearly two dozen low-amplitude variables discovered and analyzed by the Weather on Other Worlds project. Here we present also variability results for another two of our targets based on SPARTAN/SOAR and SOFI/NTT NIR observations as well as long term variability from the VVV survey for some additional VVV targets. B 1 2 3 4 [email protected] Departamento de Fisica y Astronomia, Universidad de Valparaiso Department of Physics and Astronomy, Stony Brook Univesity European Southern Observatory Departamento de Astronomia, Pontificia Universidad catolica de Chile 84 Star Formation SF -1 Observational diagnostics of young stellar objects in NGC 2264 Silvia AlencarB1 ; Jerome Bouvier2 ; John Stauffer3 ; CSI2264 Team We present the results of a multiwavelength observational campaign of the young (⇠ 3 Myr) open cluster NGC 2264. The cluster was observed simultaneously for about a month with the CoRoT, MOST and Spitzer satellites in December 2011 and January 2012. We also obtained 3.5 days of Chandra observations at the same epoch, together with 20 epochs of FLAMES (VLT-ESO) multi-object spectrocopy and U band photometry with Megacam at CFHT. We have identified several classes of objects with optical light curves that are dominated by either by cold spots, extinction by circumstellar material or variable accretion events. We show that we can characterize, with both photometric and spectroscopic data, the different physical processes taking place at the stellar surface and its circumstellar environment of young low mass systems. B 1 2 3 [email protected] DF-ICEx, UFMG, Brazil IPAG, Grenoble, France Caltech, USA 85 Star Formation Short Talks SF -1 The SONYC survey: Towards a complete census of brown dwarfs in star forming regions Kora MuzicB1 ; Aleks Scholz2 ; Ray Jayawardhana3 ; Vincent C. Geers4 ; P. Dawson4 ; T. P. Ray4 ; M. Tamura5 Deep surveys of star forming regions are the backbone of observational studies on the origin of stars and planets: On one side, they provide large and homogeneous object samples required to study disks, accretion, and multiplicity. On the other side, such surveys determine the shape and the low-mass limit of the Initial Mass Function (IMF), which are fundamental constraints on star formation theory. SONYC, short for “Substellar Objects in Nearby Young Clusters”, is an ongoing project to provide a census of the substellar population in nearby star forming regions. We have conducted deep optical and nearinfrared photometry, combined with proper motions, and followed by extensive spectroscopic follow-up campaigns with Subaru and VLT, in which we have obtained more than 700 spectra of candidate objects in NGC1333, ⇢ Ophiuchi, Chamaeleon-I, Upper Sco, and Lupus-3. We have identified and characterized more than 60 new substellar objects, among them a handful of objects with masses close to, or below the Deuterium burning limit. Thanks to the SONYC survey and the efforts of other groups, the substellar IMF is now well characterized down to ⇠ 5 10MJ , and we find that the ratio of the number of stars with respect to brown dwarfs lies between 2 ad 6. Another important piece of information for the star formation theories is that, down to ⇠ 5MJ , the free-floating objects with planetary masses are 20-50 times less numerous than stars, so that their total contribution to the mass budget of the clusters can be neglected. In this contribution we will present the status of the SONYC survey, discuss its main results, and focus on the latest findings in NGC1333, Lupus-3 and Upper-Sco. B 1 2 3 4 5 [email protected] European Southern Observatory (ESO), Chile School of Physics & Astronomy, St. Andrews University, United Kingdom Department of Astronomy & Astrophysics, University of Toronto, Canada School of Cosmic Physics, Dublin Institute for Advanced Studies, Ireland National Astronomical Observatory of Japan, Tokyo, Japan 86 Short Talks Star Formation SF -1 Millimeter and Far-IR observations of the IRDC G341.24-0.27 Vasquez, J.B1,2 ; Cappa, C.1,2 ; Romero, G.2 ; Rubio, M.3 Infrared Dark Clouds (IRDCs) are the cold T < 25 K) and dense (> 105 cm and a mass of 10⇥ 2 5 3 ) regions, with a scale of 1 - 10 pc M . Cores within the IRDCs may be in different phases, from a quiescent to an active one. Quiescent cores represent the earliest protostellar (starless) core phase without infrared signatures of star formation, commonly observed at far IR wavelengths, while active cores have extended and enhanced 4.5µm emission. In this work, we analyze CO(2-1), 13CO(2-1), and CO(2-1) lines, and mid- and far-infrared data towards the EGOS (Extended Green Objects) G341.23-0.27 and G341.22-0.26(a), projected onto the IRDC G341.240.27. B 1 2 3 [email protected] Instituto Argentino de Radioastronomı́a, CONICET, Argentina Facultad de Ciencias Astronómicas y Geofı́sicas de La Plata, Argentina Departamento de Astronoı́mia, Universidad de Chile 87 Star Formation Short Talks SF -1 A X-ray view of young star population in CMa R1 Santos-Silva, T.B1 ; Gregorio-Hetem, J.1 ; Montmerle, T.2 In previous works we studied the star formation scenario in the molecular cloud Canis Major R1 (CMa R1), derived from the existence of young stellar population groups near the Be stars Z CMa and GU CMa. Using data from the ROSAT X-ray satellite, having a field-of-view of ⇠ 1o in diameter, Gregorio-Hetem et al. (2009) discovered in this region young stellar objects mainly grouped in two clusters of different ages, with others located in between. In order to investigate the nature of these objects and to test a possible scenario of sequential star formation in this region, four fields (each 30 arcmin diameter, with some overlap) have been observed with the XMM-Newton satellite, with a sensitivity about 10 times better than ROSAT. The XMM-Newton data are currently under analysis. Preliminary results indicate the presence of about 324 sources, most of them apparently having one or more near-infrared counterparts showing typical colors of young stars. The youth of the X-ray sources was also confirmed by X-ray hardness ratio diagrams (XHRD), in different energy bands, giving an estimate of their Lx/Lbol ratios. In the present work we show the results of the study based on the spectra of about 150 sources found in four XMM fields. We checked that the X-ray spectra (0.3 to 10 keV) of young objects is different from that observed in field stars and extragalactic objects. Some of the candidates also have light curve showing flares that are typical of T Tauri stars, which confirms the young nature of these X-ray sources. B 1 2 [email protected] Instituto de Astronomia Geofı́sica e Ciências Atmosféricas, Departamento de Astronomia Institut d’Astrophysique de Paris 88 Short Talks Star Formation ISM -1 The role of reconnection diffusion in the gravitational collapse of turbulent cloud cores Leão, M. R. M.1 ; de Gouveia Dal Pino, E. M.2 ; Santos-Lima, R.B2 ; Lazarian, A.3 For a molecular cloud clump to form stars some transport of magnetic flux is required from the denser, inner regions to the outer regions of the cloud, otherwise this can prevent the collapse. Fast magnetic reconnection which takes place in the presence of turbulence can induce a process of reconnection diffusion (RD). Extending earlier numerical studies of reconnection diffusion in cylindrical clouds, we consider more realistic clouds with spherical gravitational potentials and also account for the effects of the gas self-gravity. We demonstrate that within our setup RD is efficient. We have also identified the conditions under which RD becomes strong enough to make an initially subcritical cloud clump supercritical and induce its collapse. Our results indicate that the formation of a supercritical core is regulated by a complex interplay between gravity, self-gravity, the magnetic field strength and nearly transonic and trans-Alfvénic turbulence, confirming that RD is able to remove magnetic flux from collapsing clumps, but only a few of them become nearly critical or supercritical, sub-Alfvénic cores, which is consistent with the observations. Besides, we have found that the supercritical cores built up in our simulations develop a predominantly helical magnetic field geometry which is also consistent with observations. Finally, we have evaluated the effective values of the turbulent reconnection diffusion coefficient and found that they are much larger than the numerical diffusion, especially for initially trans-Alfvénic clouds, ensuring that the detected magnetic flux removal is due to to the action of the RD rather than to numerical diffusivity. B 1 2 3 [email protected] Instituto de Matemática, Estatı́stica e Computação Cientı́fica, UNICAMP Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, USP University of Wisconsin 89 Star Formation Short Talks SF -2 The SACY view of the Sco-Cen complex B1 Claudio H. F. Melo ; Carlos A. O. Torres2 ; Germano R. Quast2 ; Ramiro de la Reza3 ; Juarez B. de Carvalho2 SACY is a program to search for associations containing young stars in the solar neighborhood. For that we observed spectroscopically and photometrically TYCHO stars that were detected in the ROSAT survey. We have detected some previously unknown young nearby associations as we published somewhere. Nevertheless most of the young detected stars belong to the Sco-Cen complex, and this enables a new view of this complex. To better accomplish this we add to our catalog some stars attributed to one of the associations of the complex, mainly for the ones that have few members in the SACY sample. We have a new view of the kinematical, spatial, age and Li distribution definitions of LCC, US, UCL, Lupus, rho Oph extension, CrA extension associations and we can also compare them with other associations that are considered in some way connected with the complex (as TWA, epsilon Cha, beta Pic and the Cha I/II associations). We show a new view of the young solar environment from 5 to 15 Myr. B 1 2 3 [email protected] ESO Laboratório Nacional de Astrofı́sica (LNA/MCTI) Observatório Nacional (ON/MCTI) 90 Short Talks Star Formation SF -2 The Role of Local Environment in Stellar Cluster Formation Carlos G. Román-ZúñigaB1 We will present the results of a comparative analysis of the properties of galactic embedded clusters in various active star forming complexes of the galaxy: B59, W3/W3(OH), W75N/S, Rosette and Sh 2-252. By combining deep, near-IR observations with archive point source catalogs from Spitzer and Chandra Space Telescopes, we compare the young stellar clusters forming in these regions, in terms of their development in the context of influence from massive star formation, the structure of the molecular cloud in which they form -analyzed from dust-extinction maps and, when available, dust-emission maps from Herschel Space Telescope. It appears that local triggering by massive clusters could be less important than cloud structure in determining the formation of secondary and tertiary generations. Clusters form in dense molecular clumps and evolve rapidly, with class II and class III sources spreading away from prenatal gas in a times comparable to disk-dissipation timescales, while class 0/I sources continue to trace the aggregation of material as the cloud and form with decreasing efficiency as the available gas is exhausted. B 1 [email protected] Instituto de Astronomı́a, Universidad Nacional Autónoma de México 91 Star Formation Short Talks SF -2 Deuteration and fragmentation in massive star-forming regions Rodón, J. A.B1 ; Beuther, H.2 ; Zhang, Q.3 ; Schilke, P.4 In the last decade, we have started to spatially resolve the small gas and dust condensations in high-mass star-forming regions that will eventually become a massive star or system, finally being able to describe how those regions fragment. Recent works, for example Palau et al. 2013, show that there is no correlation between the fragmentation of a region and its physical properties. But what about its chemistry? According to Fontani et al. 2011, an interesting chemical property to investigate is the deuteration fraction, since it can be used as a chemical clock. In this contribution we show the fragmentation properties and deuteration factors obtained for a group of massive star-forming regions with SMA, PdBI, and IRAM-30m observations, and discuss what the relationship between them tells us. B 1 2 3 4 [email protected] European Southern Observatory Max-Planck Institut für Astronomie Harvard-Smithsonian Center for Astrophysics Universität zu Köln 92 Short Talks Star Formation SF -2 Formation Models of Cometary Ices in Protoplanetary Disks Chaparro, G.B1 ; Kamp, I.1 I set out to constrain the chemical conditions in the early Solar System by analyzing chemical evolution models of protoplanetary disks and comparing them to our current knowledge of Solar System bodies, such as comets. For this I require a 2D radiative disk model in vertical hydrostatic equilibrium to set the conditions in which the chemistry evolves. Given that the planet (and comet) forming region of disks coincides with the cosmic-ray dominated midplane of disks, I focus on understanding the role of cosmic ray-induced photoprocesses, treating them in a way that is consistent with the local dust and gas opacity. I find that gas opacity in gas-rich regions of the disk midplane is a major contributor to the total opacity. Gas species formed in this region that drift vertically to optically thin zones may be used to probe the midplane chemical activity. I find that cometary ice species are formed in timescales shorter than the lifetime of the disk, thus showing that steady-state chemical models underpredict those abundances. I propose that regions located at r > 10 AU are ideal for the formation of ice mantles that match observed cometary abundances and ice-to-dust mass ratios. I discuss the possibility of trapping ice species formed in early stages of the disk evolution, thus forming a stratified ice mantle. The growth of an ice mantle contributes to increase significantly the size of dust grains. Such a modification in the dust size distribution will impact the midplane temperature and the efficiency of dust coagulation. B 1 [email protected] Kapteyn Astronomical Institute 93 94 ISM ISM -1 A new catatalogue of H I supershell candidates in the outer part of the Milky Way Suad, L. A.B1 ; Caiafa, C. F.1,2 ; Arnal, E. M.1,3 ; Cichowolski, S.4 The interstellar medium, when viewed in the neutral hydrogen (H I) line emission, reveals a complex structure that is evidenced by the presence of inhomogeneities like shells, supershells, arcs, cavities and loops. In particular H I supershells are minima in the galactic H I emission distribution surrounded completely, or partially, by ”walls” of enhanced H I emission. Supershells are believed to be created, most likely, by the action of the powerful stellar winds of massive stars and their subsequent explosion as supernova. Nevertheless, other mechanisms like gamma-ray bursts or high velocity cloud infall have been proposed for those shells whose kinetic energy is about 1053 54 erg. In this work we present a new catalogue of H I supershell candidates in the outer part of the Galaxy. Several catalogues of shells and/or supershells have been made using either a visual inspection (Heiles 1979, 1984; McClure-Griffiths et. al 2002) or automatic algorithms (Ehlerová & Palous 2005, 2013; Daigle et al. 2007). In this new catalogue we have used a combination of both visual and automatic identification procedures. One of the main features of our algorithm has to do with the fact that it is able to recognize structures even when they are not completely surrounded by walls of H I emission. In this respect it is quite different from the automatic detection algorithms used up to now by other researchers. We used the LeidenArgentine-Bonn survey (Kalberla et al. 2005). The catalogue covers most of the second and third galactic quadrants, except for a region 30 wide centered at 180 (90 < l < 165 and 195 < l < 270 ; 50 < b < 50 ). We have considered as supershell candidates those structures satisfying the following criteria: I) a linear diameter larger than 200 pc, II) an angular diameter larger than 2 , and III) a velocity extent of at least 6.5k s 1 . A total of 575 supershells have been catalogued. Only 55% of them are completely surrounded by ”walls” of enhanced H I emission. In this work we also analyze the main statistical parameters of the supershell candidates. From the OB associations and open clusters catalogues we have looked for correlations between these objects and the supershells. Finally, we have compared our catalogue with the ones made by other authors. B 1 2 3 4 [email protected] Instituto Argentino de Radioastronomı́a (IAR), CC 5, 1894, Villa Elisa, Argentina Facultad de Ingenierı́a, Universidad de Buenos Aires, C.A.B.A., Argentina Facultad de Ciencias Astronómicas y Geofı́sicas, Universidad Nacional de La Plata, La Plata, Argentina Instituto de Astronomı́a y Fı́sica del Espacio (IAFE), Cuidad Universitaria, C.A.B.A, Argentina 95 ISM Short Talks ISM -1 Photostability of Organic Molecules in Circumstellar Environment Monfredini, T.B1 ; Wolff, W.1 ; Mendoza, E. F.1 ; Lago, A. F.2 ; Rocco, M. L. M.1 ; Boechat-Roberty, H. M.1 From observational data of interstellar medium we have two clear spectroscopy features in the VIS and UV wavelength ranges: the unidentified diffuse interstellar bands (DIBs) and the bump at 217.5 nm. Neutral and ionic Polycyclic Aromatic Hydrocarbons (PAHs), which consist of fused benzene rings, such as naphthalene, anthracene and pyrene, have been found in several astrophysical environments, ranging from planetary nebulae to active galactic nuclei. Toluene (C6 H5 CH3 ), or methyl-benzene molecule, is a basic unit for the methylated PAHs. Their precursor molecules such as benzene (C6 H6 ), diacetylene (C4 H2 ), triacetylene (C6 H2 ), methylacetylene (CH3 C2 H) and methyl-diacetylene (CH3 C4 H) were detected in protoplanetary nebulae CRL 618 (Cernicharo et al. 2001a) and in SMP LMC 11 in the Large Magellanic Cloud (Bernard-Salas et al. 2008). Interaction of UV and X-ray photons from the hot central star ionizes and dissociates molecules present in its circumstellar material. Ionic species and free radicals, produced by these processes, can lead to the formation of new organic molecules. In this work we present the study of the photoionization and photodissociation processes of the toluene molecule in gas phase using synchrotron radiation at soft X-ray spectral regions and time of flight mass spectrometry. Mass spectra of ionic fragments were recorded at energies around C1s resonance (285 eV). The production of ions from the toluene were quantified, indicating that C6 H5 CH3 is more efficiently fragmented by soft X-ray than by UV radiation, where 30% of the ionized molecule survive to UV dissociation while only about 3% resist to X-rays. Partial ion yields of H+ and small + hydrocarbons such as C2 H+ , C3 H+ 2 and C3 H3 are determined. Absolute photoionization and dissociative photoionization cross sections have also been determined. From these values the ionization rate, destruction rate and half-life of methyl benzene molecule were also obtained for the X-ray photon fluxes in CRL 618. For example, this molecule survives about 2 ⇥ 103 years at a distance of 595 AU from the central star. B 1 2 [email protected] Universidade Federal do Rio de Janeiro Universidade Federal do ABC 96 Short Talks ISM ISM -1 Gas, dust and star formation in the infrared dust bubble S 24 Cappa, C. E.B1,2 ; Vasquez, J.1,2 ; Firpo, V.3 ; Duronea, N. U.4 ; Romero, G. A.2 ; Rubio, M.4 We analyze the interstellar medium in which the infrared dust bubble S 24 is evolving. Based on observations of the 12 CO(2-1), 12 CO(3-2), 13 CO(2-1), and 13 CO(3-2) lines, and continuum at 870 µm obtained with the Atacama Pathfinder Experiment (APEX) located in the north of Chile, and Herschel images at 70, 160, 250, 350 y 500 µm, we identified a gas and dust shell that surrounds the bubble showing active star formation. We estimate the main physical parameters of the gas and dust and compare our results with other dust bubbles in our Galaxy. B 1 2 3 4 [email protected] Facultad de Cs. Astronómicas y Geofı́sicas, UNLP, Argentina Instituto Argentino de Radioastronomı́a, CONICET, Argentina Universidad de La Serena, Chile Universidad de Chile, Chile 97 ISM Short Talks ISM -2 The deceleration of nebular shells in evolved planetary nebulae Margarita PereyraB1 ; Michael G. Richer1 ; José Alberto López1 We have selected a group of 100 evolved planetary nebulae (PNe) and study their kinematics based upon spatially-resolved, long-slit, echelle spectroscopy. The data have been drawn from the San Pedro Mártir Kinematic Catalogue of PNe (López et al. 2012). The aim is to characterize in detail the global kinematics of PNe at advanced stages of evolution with the largest sample of homogenous data used to date for this purpose. The results reveal two groups that share kinematics, morphology, and photo-ionization characteristics of the nebular shell and central star luminosities at the different late stages under study.The typical flow velocities we measure are usually larger than seen in earlier evolutionary stages, with the largest velocities occurring in objects with very weak or absent [N II] 6584 line emission, by all indications the least evolved objects in our sample. The most evolved objects expand more slowly. This apparent deceleration during the final stage of PNe evolution is predicted by hydrodynamical models, but other explanations are also possible. These results provide a template for comparison with the predictions of theoretical models. B 1 [email protected] Instituto de Astronomı́a de la UNAM 98 Short Talks ISM ISM -2 The Carbon Content in Galactic Ring Nebulae: CNO Nucleosynthesis in Massive Stars A. Mesa-DelgadoB1 ; J. Garcı́a-Rojas2 ; C. Esteban2 ; F. Bresolin3 ; C. Morisset4 Ring nebulae are interstellar bubbles of ionized gas that have swept-up the surrounding interstellar medium (ISM) after mass loss episodes experienced by their progenitors. As such, they are valuable probes of the chemical enrichment of the ISM by massive stars. In the last 50 years, the study of their chemical composition has been based on the analysis of optical data, which have mainly informed us about elements such as He, N, O, and Ne. Carbon abundances, however, have been historically difficult to obtain. In this talk, we will present the first determinations of C abundances based on the faint recombination line CII 4267 Å from the analysis of the two brightest and nearest Galactic ring nebulae (NGC6888 and NGC7635). These crucial results represent the first contraints on C abundances, providing long-awaited information on the action of the CNO cycle that controls the nucleosynthesis processes in massive stars, and on the role of these in the origin of carbon in the Universe. B 1 2 3 4 [email protected] Pontificia Universidad Católica de Chile Instituto de Astrofı́sica de Canarias Institute for Astronomy, University of Hawaii Instituto de Astronomı́a, Universidad Nacional Autonoma de México 99 ISM Short Talks ISM -2 Ionization Correction Factors in Planetary Nebulae Delgado Inglada, G.B1 ; Morisset, C.1 ; Stasinska, G.2 Element abundances in planetary nebulae (PNe) have been longly used as tracers of metallicity and also as probes for stellar nucleosynthesis. In general, not all the ions present in the nebulae are observed, and thus, we need to use ionization correction factors (ICFs) to account for their contribution. Much work has been done on improving ICFs, but the correction scheme suggested by Kingsburgh & Barlow (1994), based on around ten unpublished models, is still the most adopted one in the literature. Moreover, it is known that some of these ICFs do not correct properly for unobserved ions (such as for Ne or S). We compute an extensive grid of ⇠15000 photoionization models using the c10.00 version of Cloudy code (Ferland et al. 1998) in order to re-analyze this issue. The models cover a wide range of Tef f , L⇤ , Rin , and nH , and incoporate blackbodies and Rauch atmospheres as ionizing sources. We calculate constant and nonconstant density models as well as radiation- and matter-bounded models. Using this grid of models, we explore new ICFs for PNe, and, what is more important, we quantify the uncertainties associated with the ICFs. We also use a large sample of PNe from the literature with observational data to test our ICFs. I will present here some of our results and I will compare them with those obtained from previous ICFs. B 1 2 [email protected] Institute of Astronomy, UNAM (Mexico) Paris-Meudon Observatory (France) 100 Short Talks ISM ISM -2 Carbon and Oxygen Abundances from Recombination Lines in Low Metallicity HII Regions Esteban, C.B1,2 ; Garcı́a-Rojas, J.1,2 ; Carigi, L.3 ; Mesa-Delgado, A.4 We present results on the analysis of deep echelle spectrophometry obtained with large aperture telescopes of several interesting low-metallicity HII regions where CII and OII recombination lines have been detected. Firstly, we discuss recent results about the shape of the Galactic C and C/O radial gradients at and beyond the photometric radius of the Milky Way. Secondly, we present results on several giant extragalactic HII regions and HII galaxies. The data permit to study the behavior of the abundance discrepancy factor the difference between abundance determinations based on recombination and collisionally excited lines ratios and C enrichment in the low-metallicity regime. B 1 2 3 4 [email protected] Instituto de Astrofı́sica de Canarias Departamento de Astrofı́sica, Universidad de La Laguna Instituto de Astronomı́a, Universidad Nacional Autónoma de México Departamento de Astronomı́a y Astrofı́sica, Pontificia Universidad Católica de Chile 101 and the C/O ISM Short Talks ISM -2 The internal density structure of Giant HII Regions H. O. CastañedaB1 ; H. E. Caicedo Ortiz2 ; J. Perez Oregón1 By measuring the local density of the ionized gas we study the internal structure of Giant HII Regions in the galaxies NGC 6822 and M 33. The data shows the existence of density gradients in localized areas of these objects. The result should to be taken into account in the calculation of the chemical abundances of gaseous nebula. We discuss the different models for the distribution of the radial density of the objects. B 1 2 [email protected] Departamento de Fisica, Escuela Superior de Fı́sica y Matemáticas. Instituto Politénico Nacional, Mexico Grupo de Ingenierı́a y Tecnologı́as Cuántica, Corporación Universitaria Autónoma del Cauca, Popayán, Colombia 102 Galaxies GAL -1 The abundance of galaxies and dark matter halos in the ⇤CDM Universe Abadi, M. G.B1 The ⇤CDM cosmological model is the current paradigm for structure formation in the Universe. A longstanding puzzle of this model concerns the striking difference between the shape of the galaxy stellar mass function and the cold dark matter halo mass function on dwarf galaxy scales. Dwarf galaxies are much less numerous than halos massive enough to host them, suggesting a complex non-linear relation between the mass of a galaxy and that of its surrounding halo. This is usually reconciled by appealing to baryonic processes that drastically reduce the efficiency of galaxy formation in low-mass halos. Recent models require that virtually no dwarf galaxies form in halos with virial mass below 1010 M . We use rotation curves of dwarf galaxies compiled from the literature to explore whether their total enclosed mass is consistent with these constraints. We find that almost one-half of the dwarfs in our sample, are at odds with this restriction: they live in haloes with masses substantially below 101 0M . This result presents a challenge to the cosmological model ⇤CDM. We use a cosmological simulation of the formation of the Local Group of Galaxies to identify a mechanism that enables the removal of baryons from low-mass halos without appealing to feedback or reionization. This mechanism may help to explain the scarcity of dwarf galaxies compared with the numerous low-mass halos expected in ⇤CDM and the large diversity of star formation histories and morphologies characteristic of faint galaxies. B 1 [email protected] Observatorio Astrónomico, Universidad Nacional de Córdoba and IATE, CONICET-UNC 103 Galaxies Short Talks GAL -1 The Formation of dSph galaxies Fellhauer, M.B1 ; Assmann, P.1,2 ; Wilkinson, M. I.3 Dwarf spheroidal (dSph) galaxies are considered the basic building blocks of the galaxy formation process in the ⇤CDM (Lambda Cold Dark Matter) hierarchical cosmological model. These galaxies are believed to be the most dark matter (DM) dominated systems known, have the lowest stellar content, and are poor in gas. Many theories attempt to explain the formation of dSph galaxies resorting to the fact that these galaxies are mainly found orbiting large galaxies or invoking other mechanisms of interactions. Here we show the full set of simulation as an extension of our fiducial model, where we study the formation of classical dSph galaxies in isolation by dissolving star clusters within the DM halo of the dwarf galaxy. In our parameter survey we adopt cored and cusped DM halo profiles and consider different numbers of dissolving star clusters. We investigate the dependency of observable quantities with different masses and scale-lengths of the DM halo and different star formation efficiencies (SFE). We find that our proposed scenario explains many features of the classical dSph galaxies of the Milky Way, like their morphology and their dynamics. We see trends how the surface brightness and the scale-length of the luminous component vary with the parameters of our simulations. We also identify how irregularities in their shape, i.e. clumpiness and ellipticity vary in our simulations. In velocity space, we identify the parameters leading to flat velocity dispersions curves. We recognize kinematically cold substructures in velocity space, named fossil remnants and stemming from our unique initial conditions, which alter the expected results. These streaming motions are considered as a key feature for future observation with high resolution to validate our scenario. B 1 2 3 [email protected] Departamento de Astronomia, Universidad de Concepcion, Chile Departamento de Astronomia, Universidad de Chile, Chile Department of Physics & Astronomy, University of Leicester, UK 104 Short Talks Galaxies GAL -1 Constraining Galaxy Evolution with Scaling Relations de la Rosa, I. G.B1,2 ; Ferreras, I.3 ; Dominguez, H.4 ; Lopes, P. A. A.2 The non-linear scaling relation involving surface brightness and magnitude for Early Type Galaxies (ETGs) shows a prominent turnover at MB ⇡ - 20.5. In a previous stellar population study, using SDSS spectra, we have sustained the idea of the turnover as a fundamental feature of the scaling relations, separating ETGs with different star formation histories. An ongoing study is presented in which similar scaling relations are constructed for ETGs in clusters with redshifts ranging from 0.2 to 0.9. Data are taken from the deep HST observations of the CLASH Survey, including 25 clusters measured in 16 broad bands from NUV to NIR. The variation of the turnover position with redshift, which shows a mixed sensitivity to cosmic expansion, surface-brightness-dimming and galaxy evolution, is used as a consistency test for cosmic and galaxy evolution. B 1 2 3 4 [email protected] Instituto de Astrofisica de Canarias, Spain Observatorio do Valongo, Brasil University College London, UK Centro de Astrobiologia, Spain 105 Galaxies Short Talks GAL -1 How do Brightest Cluster and Group galaxies grow? Observations vs Models Oliva-Altamirano, P.B1,2 ; Brough, S.2 ; Lidman, C.2 ; Couch, W.2 ; Taylor, E.3 Brightest Cluster Galaxies (BCGs) represent the most luminous systems known at present epochs. The extent to which such extreme galaxies have acquired their particular properties from their privileged location at the centres of clusters and/or their high density environment is of key astrophysical interest. Unfortunately, the assembly history and evolution of these giant galaxies is still poorly understood. We have analyse the growth of BCGs in the last 3.5 billion years using a large sample (1220 BCGs/BGG) from the Galaxy and Mass Assembly Survey (GAMA), and compared our results with the Semi-Analytic Models (SAMs) of De Lucia & Blaizot (2007) and Tonini et al. (2012). By comparing like-to-like clusters we find no significant growth between redshift 0 and 0.3, whereas SAMs predict that BCGs have acquired 30% of their stellar mass over this period of cosmic time. We also examine the position of the BCGs with respect to their Dark Matter Halo and find that around 14% of the BCGs are not lying at the centre of the dark matter halo potential well and this could be an indicator of recent cluster mergers. In a further analysis, we found that around 40% of the BCGs harbor on-going star formation, with rates in a range 0-4 M per year, in agreement with the new recipes used in Tonini et al. (2012). While BCGs might not be completely dormant, the fraction of their mass being converted into new stars is still very low. B 1 2 3 [email protected] Swinburne university of Technology Australian Astronomical Observatory (AAO) University of Melbourne 106 Short Talks Galaxies GAL -1 Quenching Star Formation Now and Then: Downsizing of the Mass Flux Density in the Green Valley Gonçalves, T. S.B1 ; Menéndez-Delmestre, K.1 ; Nogueira-Cavalcante, J. P.1 ; Martin, D. C.2 ; Lopes, P. A. A.1 The bimodality in galaxy properties has been observed at low and high redshift, with a clear distinction between star-forming galaxies in the blue cloud and passively evolving objects in the red sequence. The absence of galaxies with intermediate properties indicates that the quenching of star formation and subsequent transition between populations must happen rapidly. By using very deep spectroscopy with the DEIMOS instrument at the Keck telescope we are able to infer the star formation histories of so-called “green valley” galaxies at intermediate redshifts (z ⇠ 0.8), when the universe was half its current age. We measure the stellar mass flux density of green valley galaxies transiting from the blue cloud to the red sequence and find that this transition happens more rapidly in the past and that at z ⇠ 0.8 this process happens more rapidly for more massive galaxies. This suggests a top-down scenario in which the massive end of the red sequence forms first, representing another aspect of downsizing, with the mass flux density moving towards smaller galaxies in recent times. It remains an open question, however, which physical mechanisms are responsible for quenching star formation and how they may be more efficient at z ⇠ 0.8 than at lower redshifts. To tackle this we have recently initiated a project to detect the presence of bars at low and high redshift, and correlate their strength with the quenching timescales. This will allow us to infer the influence of secular evolution in galaxies at different epochs. B 1 2 [email protected] Observatório do Valongo, Universidade Federal do Rio de Janeiro California Institute of Technology 107 Galaxies Short Talks GAL -2 Evolution models for spiral and irregular galaxies M. MolláB1 ; O. Cavichia; R. D. D. Costa We will summarize our grid of chemical and spectro-photometrical models applied to spiral and irregular galaxies. They have been calculated consistently by applying to the chemical evolution code from Molla & Diaz (2005), updated with the most recent inputs (Mollá & Dı́az 2013). We will analyze the impact of the new assumptions related with the infall rate law, the IMF and stellar yields, and new prescriptions to form molecular clouds. Furthermore we will show the spectro-photometric information obtained when the evolutionary synthesis models from POPSTAR (Mollá et al 2009, Martı́n-Manjon 2010, Garcı́a-Vargas et al. 2013) are applied to the resulting star formation and enrichment histories of this type of galaxies. B 1 [email protected] CIEMAT (Spain) and Universidade de Sao Paulo (Brazil) 108 Short Talks Galaxies GAL -2 Galaxy And Mass Assembly (GAMA): The connection between metals, specific SFR and H I gas in galaxies: the Z-SSFR relation Lara-Lopez, M. A.B1 ; Hopkins, A. M.1 ; GAMA team We study the interplay between gas phase metallicity (Z), specific star formation rate (SSFR) and neutral hydrogen gas (HI) for galaxies of different stellar masses. Our study uses spectroscopic data from Galaxy and Mass Assembly (GAMA) and Sloan Digital Sky Survey (SDSS) star-forming galaxies, as well as HI detection from the Arecibo Legacy Fast Arecibo L-band Feed Array (ALFALFA) and Galex Arecibo SDSS Survey (GASS) public catalogues. We present a model based on the Z-SSFR relation that shows that at a given stellar mass, depending on the amount of gas, galaxies will follow opposite behaviours. Low-mass galaxies with a large amount of gas will show high SSFR and low metallicities, while low-mass galaxies with small amounts of gas will show lower SSFR and high metallicities. In contrast, massive galaxies with a large amount of gas will show moderate SSFR and high metallicities, while massive galaxies with small amounts of gas will show low SSFR and low metallicities. Using ALFALFA and GASS counterparts, we find that the amount of gas is related to those drastic differences in Z and SSFR for galaxies of a similar stellar mass. The results of this study were publish recently in a ”letter to the editor” (Lara-Lopez, M. A. et al. 2013, MNRAS, 433, L35) B 1 [email protected] Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia 109 Galaxies Short Talks GAL -2 Evolution of the Mass-Metallicity relations in passive and star-forming galaxies from SPH-cosmological simulations A. D. RomeoB1 ; J. Sommer-Larsen2 ; N. R. Napolitano3 ; V. Antonuccio-Delogu1 We present results from SPH-cosmological simulations, including self-consistent modelling of SN feedback and chemical evolution, of galaxies belonging to two clusters and twelve groups. We reproduce the mass– metallicity (ZM) relation of galaxies classified in two samples according to their star-forming activity, as parametrized by their sSFR, across a redshift range up to z = 2. The overall ZM relation for the composite population evolves according to a redshift-dependent quadratic functional form that is consistent with other empirical estimates, provided that the highest mass bin of the BCGs is excluded. Its slope shows irrelevant evolution in the passive sample, being steeper in groups than in clusters. However, the sub-sample of high-mass passive galaxies only is characterized by a steep increase of the slope with redshift, from which it can be inferred that the bulk of the slope evolution of the ZM relation is driven by the more massive passive objects. The scatter of the passive sample is dominated by low-mass galaxies at all redshifts and keeps constant over cosmic times. The mean metallicity is highest in cluster cores and lowest in normal groups, following the same environmental sequence as that previously found in the Red Sequence building. The ZM relation for the star-forming sample reveals an increasing scatter with redshift, indicating that it is still being built at early epochs. The star-forming galaxies make up a tight sequence in the SFR-M⇤ plane at high redshift, whose scatter increases with time alongside with the consolidation of the passive sequence. We also confirm the anti-correlation between sSFR and stellar mass, pointing at a key role of the former in determining the galaxy downsizing, as the most significant means of diagnostics of the star formation efficiency. Likewise, an anti-correlation between sSFR and metallicity can be established for the star-forming galaxies, while on the contrary more active galaxies in terms of simple SFR are also metal-richer. Finally the [O/Fe] abundance ratio is presented too: we report a strong increasing evolution with redshift at given mass, especially at z > 1. The expected increasing trend with mass is recovered when only considering the more massive galaxies. We discuss these results in terms of the mechanisms driving the evolution within the high- and lowmass regimes at different epochs: mergers, feedback-driven outflows and the intrinsic variation of the star formation efficiency. B 1 2 3 [email protected] INAF-OA Catania, Italia Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Danmark INAF-OA Capodimonte, Napoli, Italia 110 Short Talks Galaxies GAL -2 The formation of stellar haloes of massive Spirals in hierarchical scenario Patricia B. TisseraB1,2 ; Timothy C. Beers4 ; Daniela Carollo5 ; Cecilia Scannapieco3 We investigate the chemical and kinematic properties of the diffuse stellar haloes of six simulated Milky Way-like galaxies from the Aquarius Project. Binding energy criteria are adopted to defined two dynamically distinct stellar populations: the diffuse inner and outer haloes, which comprise different stellar subpopulations with particular chemical and kinematic characteristics. Our simulated inner- and outer-halo stellar populations have received contributions from debris stars (formed in sub-galactic systems while they were outside the virial radius of the main progenitor galaxies) and endo-debris stars (those formed in gasrich sub-galactic systems inside the dark matter haloes). The inner haloes possess an additional contribution from disc-heated stars in the range 3 30%, with a mean of ⇠ 20% . Disc-heated stars can exhibit signatures of kinematical support, in particular among the youngest ones. Endo-debris plus disc-heated stars define the so-called insitu stellar populations. In both the inner- and outer-halo stellar populations, we detect contributions from stars with moderate to low [alpha/Fe] ratios, mainly associated with the endo-debris or disc-heated sub-populations. The observed abundance gradients in the inner-halo regions are influenced by both the level of chemical enrichment and the relative contributions from each stellar sub-population. Steeper abundance gradients in the inner-halo regions are related to contributions from the disc-heated and endo-debris stars, which tend to be found at lower binding energies than debris stars. In the case of the outer-halo regions, although [Fe/H] gradients are relatively mild, the steeper profiles arise primarily due to contributions from stars formed in more massive satellites, which sink farther into the main halo system, and tend to have higher levels of chemical enrichment and lower energies. Our results show how the abundances of the stars in the stellar haloes vary with radius up to the virial radius and how the characteristics of the metallicity distributions can be linked to the history of assembly within in hierarchical clustering scenario B 1 2 3 4 5 [email protected] Consejo Nacional de Investigaciones Cientı́ficas y Técnicas, CONICET, Argentina Instituto de Astronomı́a y Fı́sica del Espacio, Casilla de Correos 67, Suc. 28, 1428, Buenos Aires, Argentina Max-Planck Institute for Astrophysics, Karl-Schwarzchild Str. 1, D85748, Garching, Germany National Optical Astronomy Observatory, Tucson, 85719, USA Macquarie University, Dept. Physics & Astronomy, Sydney, 2109 NSW, Australia 111 Galaxies Short Talks GAL -2 The effects of dark matter halo on the mass loss process in dwarf galaxies: results from 3D hydrodynamical simulations Lanfranchi, G. A.B1 ; Ruiz, L. O.1 ; Falceta-Goncalves, D.2 ; Caproni, A.1 Theoretical ⇤ CDM cosmological models predict a much larger number of low mass dark matter haloes than has been observed in the Local Group of galaxies. One possible explanation is the increased difficulty of detecting these haloes if most of the visible matter is lost at early evolutionary phases through galactic winds. In this work we study the current models of triggering galactic winds in dwarf spheroidal galaxies (dSph) from supernovae, and study, based on 3D hydrodynamic numerical simulations, the correlation of the mass loss rates and important physical parameters as the dark matter halo mass and the star formation rate. We find that the existence of winds is ubiquitous, independent on the gravitational potential, as would be expected. This because our simulations revealed that the Rayleigh-Taylor Instability (RTI) may play a major role on pushing matter out of these systems, even for very massive haloes. However, as already reported in previous works we have found a correlation between the mass loss rate and both the halo mass and the rate of supernovae. Besides, the epoch in which most of the baryon galactic matter is removed from the galaxy varies depends on those quantities. This result, combined to the importance of the RTI in each model, may change our understanding about the chemical evolution of dwarf galaxies, as well as in the heavy element contamination of the intergalactic medium at high redshifts. B 1 2 [email protected] NAT - Universidade Cruzeiro do Sul, SP-Brasil EACH/USP, SP-Brasil 112 Short Talks Galaxies GAL -3 TP-AGB stars and population synthesis models Gustavo BruzualB1 Using updated evolutionary tracks for TP-AGB stars from the Padova Group we explore by means of Montecarlo Simulations to what extent the Luminosity Functions and color distributions of TP-AGB stars in the LMC and SMC observed by the SAGE collaboration can be reproduced with these tracks. We compute as well the gas and dust production rate by TP-AGB stars in these galaxies, and derive the amount of gas and dust expelled by these stars during the past few Gyr. Detailed comparison with observations allow us to quantify the uncertainties introduced in population synthesis models by the use of these evolutionary tracks. We show that current models provide a better description of nature than previous versions. B 1 [email protected] CRyA, UNAM, Campus Morelia, Mexico 113 Galaxies Short Talks GAL -3 Spectral Synthesis of Star-forming Galaxies in the Near-Infrared Martins, L. P.B1 ; Rodrı́guez-Ardila, A.2 ; Diniz, S.1,3 ; Riffel, R.3 ; de Souza, R.4 The near-infrared spectral region is becoming a very useful wavelength range to detect and quantify the stellar population of galaxies. Models are developing to predict the contribution of TP-AGB stars, that should dominate the NIR spectra of populations 0.3 to 2 Gyr old. When present in a given stellar population, these stars leave unique signatures that can be used to detect them unambiguously. However, these models have to be tested in a homogeneous database of star-forming galaxies, to check if the results are consistent with what is found from different wavelength ranges. In this work we performed stellar population synthesis on the nuclear and extended regions of 23 star-forming galaxies to understand how the star-formation tracers in the near-infrared can be used in practice. The stellar population synthesis shows that for the galaxies with strong emission in the NIR, there is an important fraction of young/intermediate population contributing to the spectra, which is probably the ionization source in these galaxies. Galaxies that had no emission lines measured in the NIR were found to have older average ages and less contribution of young populations. Although the stellar population synthesis method proved to be very effective to find the young ionizing population in these galaxies, no clear correlation between these results and the NIR spectral indexes were found. Thus, we believe that, in practice, the use of this indexes is still very limited due to observational limitations. B 1 2 3 4 [email protected] NAT - Universidade Cruzeiro do Sul Laboratório Nacional de Astrofı́sica Universidade Federal do Rio Grande do Sul Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas - USP 114 Short Talks Galaxies GAL -3 A new class of galaxies (?): ultra-compact dwarfs Mieske, S.B1 I propose to give a review on ultra-compact dwarf galaxies (UCDs), a new class of stellar systems defining the interface between star clusters and dwarf galaxies. UCDs are believed to be either the most massive star clusters in the universe, tidally truncated galaxies, or, both. After a brief overall summary, I will focus in particular on two aspects. 1. The specific frequencies of UCDs - a recently introduced quantity that allows to test whether the luminosity distribution of UCDs follows the bright tail of the globular cluster luminosity function. Can all UCDs be explained as bright star clusters? 2. The elevated dynamical M/L ratios of UCDs. Are they due to highly clustered dark matter, a variation of the IMF, or maybe, due to massive central black holes that would be fossil relicts of UCD progenitor galaxies? B 1 [email protected] ESO Chile 115 Galaxies Short Talks GAL -3 Andromeda’s interplay with its dwarf companions Gonçalves, D. R.B1 ; Carneiro, C. M.1 ; Magrini, L.2 ; Teodorescu, A. M.3,4 Dwarf galaxies are the most numerous galactic systems in the Universe, mostly found in galaxy groups. Dwarfs in the Local Group (LG) are excellent laboratories in which to study galaxy evolution. Among the bright resolved stars in the LG dwarf galaxies, the strong emission line feature in the spectrum of planetary nebulae (PNe) allow us to study the late evolutionary stages of stars with low and intermediate masses, as well as the star formation history and the chemical evolution of the galaxy, within the age range of 1-10 Gyr. In a series of previous studies we have investigated the chemical properties of the emission-line populations of LG dwarf galaxies, observing HII regions and PNe in galaxies presently forming stars, such as dwarf Irregulars (dirrs) and of PNe in quiescent galaxies, such as dwarf spheroidals (dSphs). The major aims of our studies can be summarised as follows. i) Deriving the chemical composition of dwarf galaxies from PNe (and HII regions, whenever possible), and setting constraints to galaxy formation and evolution, and giving us the unique opportunity to determine the chemical composition of the ISM in different epochs, as at present and at the time of the formation of the PN progenitors. ii) Studying the stellar nucleosynthesis of low- and intermediate-mass stars in different conditions, and in different metallicity environments. iii) Deriving, in a homogeneous way, the metallicity traced, e.g., by the oxygen abundance, in both dIrrs and dSphs, allowing to derive the mass-metallicity relationship for all dwarf galaxies. Ultimately, fully disentangle the possible differences in this relation, claimed in the past, for star-forming and non starforming galaxies. In this framework, here we present GMOS spectroscopic observations of the PN population in the dwarf galaxy NGC 205, the brightest early-type dwarf satellite of the Andromeda galaxy (M 31). Among the low surface brightness galaxies in the LG, this is of particular importance due to its interesting star formation history, and also to several indications of a tidal encounter with its massive companion (M 31), being the galaxy located at the shortest projected distance of the three more massive dwarf companions of Andromeda. In this contribution, we discuss –in terms of the three main aspects above– the new observations of a sample of 37 candidate PNe, 24 of them resulted to be true PNe, one is a symbiotic system, and the remaining ones are stars. B 1 2 3 4 [email protected] Observatório do Valongo - Universidade Federal do Rio de Janeiro, Brazil INAF - Osservatorio Astrofisico di Arcetri, Florence, Italy Consiglio Nazionale delle Ricerche, Pisa, Italy Institute for Astronomy, University of Hawaii, USA 116 Short Talks Galaxies GAL -3 Assessment of the SFH retrieved from synthetic u’g’r’i’z’ photometry of galaxies Mejı́a, A. J.B1 ; Magris, G.1 In recent decades the photometric data exceeds enormously the spectroscopic data. The Sloan Digital Sky Survey (SDSS), for instance, puts to disposition of the astronomical community high quality photometric data, covering a sky area considerably large and reaching depths without precedents. This work aims to assess the physical parameters retrieved from a photometric sample of synthetic galaxies using the DINBAS algorithm. In order to achieve this objetive this steps were followed: (1) the construction of a library of synthetic galaxies with observational properties similars to that of the galaxies observed by the SDSS; (2) the assessment of the SFH retrieved from the photometry by comparing with the already known input SFH; (3) the comparison between the SFH retrieved from the spectroscopy and that retrieved from the photometry using DINBAS. It was found that mass and age were degenerated when the SFH was retrieved from the u’g’r’i’z’ photometry employing DINBAS. In all the cases, the spectroscopy was more accurate than photometry, with uncertainties within ⇠ 20% and ⇠ 70%, respectively. B 1 [email protected] Centro de Investigaciones de Astronomı́a 117 Galaxies Short Talks GAL -4 First spatially-resolved observations of ionized gas in submillimeter-selected high-redshift starbursts Menéndez-Delmestre, K.B1 ; Blain, A. W.2 ; Swinbank, M.3 ; Smail, I.3 ; Ivison, R. J. 4 ; Chapman, S. C.5 ; Gonçalves, T. S.1 We present the first spatially-resolved observations of the H-alpha emission in z ⇠ 2 submillimeter-selected galaxies (SMGs) using the Keck OH-Suppressing Infrared Imaging Spectrograph (OSIRIS) with Laser Guide Star Adaptive Optics (LGS-AO). The kpc-scale spatially-resolved view into these complex systems – up to ten times that achieved with previous seeing-limited studies – allows us to explicitly distinguish between compact AGN-dominated regions of broad H-alpha emission (FWHM > 1000 km/s) from more extended regions exhibiting narrow H-alpha emission (FWHM < 500 km/s) and thus likely dominated by star formation activity. We observe that the distribution of star formation in these objects is characterized by multiple Halphabright kpc-scaled clumps, each presenting high star-formation rate surface densities, with values similar to that of local extreme sources, such as circumnuclear starbursts and luminous infrared galaxies. However, in contrast to these local environments, SMGs appear to be undergoing such intense activity on significantly larger spatial scales as revealed by extended H-alpha emission over 4-16 kpc. The estimated clump masses and specific star-formation rates set SMGs off the main-sequence of star-forming objects at z ⇠ 2. The Halpha kinematics reveal no evidence of ordered global motion as would be found in a disk, but rather large velocity offsets (⇠few x 100 km/s) between the distinct clumps. Assuming that the broad H-alpha emission identifies a super-massive black hole likely at the dynamical center of system, we interpret both the velocity offsets between the observed clumps and their asymmetric distribution around the broad H-alpha region as an indication that these are not likely to reside in a regular potential well structure. Although a clumpy disk structure has been suggested in other populations of star-forming galaxies at similar redshifts, the merger interpretation is likely the most accurate scenario for the SMGs in our sample. However, the final test of whether an underlying disk structure is present will come from detailed studies of the cold molecular gas at the high spatial resolutions possible with ALMA. B 1 2 3 4 5 [email protected] Valongo Observatory of the Federal University of Rio de Janeiro, Brazil University of Leicester, UK Institute for Computational Cosmology, Durham University, UK University of Edinburgh/Royal Observatory Institute of Astronomy, Cambridge, UK 118 Short Talks Galaxies GAL -4 Comparing galaxy populations in compact and loose groups of galaxies Martinez, H. J.B1 ; Coenda, V.1 ; Muriel, H.1 We compare the properties of galaxies in compact groups, loose groups, and the field to deepen our understanding of the physical mechanisms acting upon galaxy evolution in different environments. We select samples of galaxies in compact groups identified by McConnachie et al. (2009), and in loose groups taken from Zandivarez & Martı́nez (2011). We compare properties of the galaxy populations in these different environments: absolute magnitude, colour, size, surface brightness, stellar mass, and concentration and morphological information from the Galaxy Zoo. We also study the fraction of red and early-type galaxies, the luminosity function, the colour-luminosity, and luminosity-size relations. Particularly, we analyse the fraction of the group’s total luminosity contained in the brightest group galaxy (BCG) and the difference in luminosity between the BCG and the second ranked galaxy. We find that the population of galaxies in compact groups differ from that of loose groups and the field. The fraction of red and early-type galaxies is larger in compact groups. Galaxies in compact groups are, on average, systematically smaller in size, more concentrated, and have higher surface brightnesses than galaxies in the field and in loose groups. At a fixed absolute magnitude, or fixed surface brightness, galaxies in compact groups are smaller in size. In addition, BCGs in compact groups are systematically more concentrated and have larger surface brightness than their counterparts in both, high and low mass loose groups. Our results show that BCGs in compact groups are, on average, brighter, more massive, larger, redder and more frequently classified as elliptical. We find that, in compact groups, the BCG contains a larger fraction of the system’s total luminosity and differ more in absolute magnitude with the second ranked galaxy. The physical mechanisms that transform galaxies into earlier types could be more effective within compact groups, owing to the typically high densities and small velocity dispersions of these environments, which could explain the large fraction of red and early-type galaxies we found in compact groups. Galaxies inhabiting compact groups have undergone a major transformation compared to galaxies that inhabit loose groups. B 1 [email protected] Instituto de Astronomia Teorica y Experimental, CONICET-Universidad Nacional de Cordoba, Argentina 119 Galaxies Short Talks GAL -4 CALIFA: The local extragalactic universe unveiled (survey status) Rosales-Ortega, F. F.B1 ; Sánchez, S. F.2 ; CALIFA team The Calar Alto Legacy Integral Field Area Survey (CALIFA) is observing a statistically well-defined sample of ⇠600 galaxies in the local universe using the PMAS/PPAK IFU, mounted on the Calar Alto 3.5 m telescope. CALIFA has just published its first Data Release (DR1), prodivindg freely to the community fully reduced and quality control tested datacubes of 100 objects in two spectral resolutions. This data will allow scientists to produce maps for the different properties of galaxies, such as velocity, stellar ages or chemical composition, to mention just a few. We present the current survey status and the last scientific outcomes from the collaboration. B 1 2 [email protected] Instituto Nacional de Astrofı́sica, Óptica y Electrónica, Mexico Instituto de Astrofı́sica de Andalucı́a 120 Short Talks Galaxies GAL -4 Fireworks at the center of the Milky Way João E. SteinerB1 ; Roberto B. Menezes1 ; Daniel Amorim de Oliveira1 The central parsec of the Milky Way is a very special region of our Galaxy; it contains the supermassive black hole associated with Sgr A* as well as a significant number of early-type stars and a complex structure of streamers of neutral and ionized gas, within two parsec from the centre, representing a unique laboratory. We report the identification of a high velocity compact nebular filament 2.2 arcsec south of Sgr A*. The structure extends over ⇠1 arcsec and presents a strong velocity gradient of ⇠200 km s 1 arcsec 1 . The peak of maximum emission, seen in [Fe III] and He I lines, is located at d↵ = +0.20±0.06 arcsec and d = 2.20±0.06 arcsec with respect to Sgr A*. This position is near the star IRS 33N. The velocity at the emission peak is Vr = -267 km s 1 . The filament has a position angle of PA = 115o ± 10o , similar to that of the Bar and of the Eastern Arm at that position. The peak position is located 0.7 arcsec north of the binary X-ray and radio transient CXOGX J174540.0-290031, a low-mass X-ray binary (LMXB) with an orbital period of 7.9 h. The [Fe III] line emission is strong in the filament and its vicinity. These lines are probably produced by shock heating but we cannot exclude some X-ray photoionization from the LMXB. Although we cannot rule out the idea of a compact nebular jet, we interpret this filament as a possible shock between the Northern and the Eastern Arm or between the Northern Arm and the mini-spiral ‘Bar’. B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas - USP 121 Galaxies Short Talks GAL -4 Mapping dust-obscured light in CALIFA galaxies Vale Asari, N.B1, 2 ; Wild, V.3 ; Kennicutt, R.2 ; Cid Fernandes, R.1 The Calar Alto Legacy Integral Field Area (CALIFA) survey is the first and largest survey of its kind, aiming to obtain optical datacubes for 600 nearby (z ⇠ 0.01) galaxies. Over 300 objects have already been observed. The spatial and spectral resolutions in CALIFA, combined with its sample size, offer unprecedented good quality data to study spatially resolved dust properties. This work focus on how dust is mapped by the ionized gas. By carefully removing the underlying stellar population, we measure the emission-line Balmer decrement (H↵/H ) in different regions in galaxies, separating HII complexes from diffuse emission. Preliminary results show that the effective dust attenuation measured on an integrated spectrum is underestimated with respect to the effective attenuation on HII regions. This implies that star formation indicators based on optical and UV data should be used with care and may need to be corrected by differential dust attenuation. B 1 2 3 [email protected] Departamento de Fisica, UFSC, Brazil Institute of Astronomy, University of Cambridge, UK School of Physics and Astronomy, University of St Andrews, UK 122 Short Talks Galaxies VVV-1 The wide view of the Bulge from the VVV survey B1 Oscar A. Gonzalez ; Dante Minniti2,7 ; Philip Lucas3 ; Marina Rejkuba1 ; Manuela Zoccali2,7 ; Elena Valenti1 ; Roberto Saito2,4,7,9 ; Jim Emerson5 ; Ignacio Toledo6 ; Maren Hempel2,7 The first year of observations of the Galactic bulge in the Vista Variables in the Via lacteal (VVV) ESO Public Survey, with the VISTA telescope, have yielded a deep, near-infrared, multi-colour (Z,Y,J,H,Ks) photometric coverage of over 320 square degrees. Results based on this impressive dataset are presented, showing the global properties of the bulge in order to investigate its place in the general context of galaxy bulges. Extinction has been mapped using the magnitude and colour of the red clump, revealing a large amount small-scale structure. This extinction map has been used to de-redden the VVV stellar photometry to study the complicated bulge morphology from the absolute magnitude of the red clump and to derive photometric metallicities from the color of red giant branch stars. These results provide unique constrains for modern Galaxy formation models.. B 1 2 3 4 5 6 7 9 [email protected] ESO Departamento Astronomia y Astrofisica, Pontificia Universidad Catolica de Chile Center for Astrophysics Research, University of Hertfordshire Departamento de Fisica y Astronomia, Universidad de Valparaiso School of Mathematical Sciences, Queen Mary University of London ALMA OSF The Milky Way Milennium Nucleus Universidade Federal de Sergipe, Departamento de Fı́sica 123 Galaxies Short Talks GAL -5 The role of the corotation resonance in the secular evolution of disks of spiral galaxies Jacques R. D. LepineB1 ; S. Scarano Jr.2 ; D. A. Barros1 ; T. C. Junqueira1 ; W. S. Dias3 ; S. Andrievsky4 The corotation resonance plays an important role in the evolution of the disks of spiral galaxies, and in particular, of our Galaxy. Its effect on the chemical abundance gradients is even a tool to estimate the age of the present spiral arm structure, which we find to be long-lived, contrary to a recent common belief. The metallicity gradients usually decrease in the inner regions and become flat or rising at larger radii. In several galaxies, including the Milky Way, one observes not only a change in the slope of the abundance gradient, but also an abrupt step in metallicity at corotation. This step is because the corotation resonance separates the disk of a galaxy in two regions (inside corotation and outside corotation) which are isolated one from the other, so that the two sides evolve in an independent way. The barrier between the two regions is the result of the flow of gas in opposite directions on the two sides and by the ring-shaped void of gas observed at corotation. We investigated a sample of galaxies, which have a known corotation radius, and for which there are measurements of abundance gradients of Oxygen available in the literature. A very good correlation is found between corotation radii and the radii at which there is a break in the slope of the gradients. Besides this, an independent effect of corotation is a minimum of star formation associated with the minimum velocity at which the interstellar gas feeds the spiral arms (seen as potential wells and star-formation machines). Still another effect is the scattering of stars by the resonance, which causes their migration to different galactic radii. B 1 2 3 4 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo, São Paulo, SP, Brazil Universidade Federal de Sergipe - Departamento de Fı́sica DFI/CCET, São Cristovão, SE, Brazil Instituto de Fı́sica e Quı́mica, Universidade Federal de Itajubá, Itajubá MG, Brazil Department of Astronomy and Astronomical Observatory, Odessa National University, Odessa, Ukraine 124 Short Talks Galaxies GAL -5 Bar and spiral arms dynamics in numerical simulations Ivânio PuerariB1 ; Irapuan Rodrigues de Oliveira Filho2 We present the results of SPH simulations with multi-million particles models. The models were constructed with an exponential disk, Spitzer’s isothermal sheet in the vertical direction and a NFW halo. In models having a bulge, a spherical Hernquist profile was used. The models were evolved for approximately 5 Gyears using Gadget 2. We present 1D and 2D Fourier analysis to quantify bar characteristics as length, strength, and pattern speeds. Fourier 2D analysis is also applied to show the effects of the swing amplification mechanism. Indeed, the density waves begin to be amplified as tightly wound leading spirals and unwound to open leading structures. Afterwards, the waves wound into trailing patterns, reach their maximum amplitude and finally, fade away as tightly wound trailing spirals. The timescale for each wave packet is of the order of some 108 years. B 1 2 [email protected] INAOE, Mexico Universidade do Vale do Paraı́ba, Brazil 125 Galaxies Short Talks GAL -5 Pitch Angle Restrictions in Normal Spiral Galaxies Based on Ordered and Chaotic Orbital Behavior Perez-Viilegas, A.B1 ; Pichardo, B.2 We built a family of non-axisymmetric potential models for normal non-barred or weakly-barred spiral galaxies as defined in the simplest classification of galaxies: the Hubble sequence. For this purpose a threedimensional self-gravitating model for spiral arms PERLAS is superimposed to the galactic axisymmetric potentials. We analyze the stellar dynamics varying only the pitch angle of the spiral arms. Self-consistency is indirectly tested through periodic orbital analysis, and through density response studies for each morphological type. In a first limit, based on ordered behavior, periodic orbits studies show that for pitch angles up to approximately 15 deg, 18 deg, and 20 deg for Sa, Sb and Sc galaxies, respectively, the density response supports the spiral arms potential, a requisite for the existence of a long-lasting large-scale spiral structure. Beyond those limits, the density response tends to ”avoid” the potential imposed by maintaining lower pitch angles in the density response; in that case the spiral arms may be explained as transient features rather than long-lasting large-scale structures. In a second limit, from a phase space orbital study based on chaotic behavior, we found that for pitch angles larger than ⇠ 30 deg, ⇠ 40 deg and ⇠ 50 deg for Sa, Sb, and Sc galaxies, respectively, chaotic orbits dominate all phase space prograde region that surrounds the periodic orbits sculpting the spiral arms and even destroying them. This result seems to be in good agreement with observations of pitch angles in typical isolated normal spiral galaxies. B 1 2 [email protected] Centro de Radioastronomia y Astrofisica, UNAM Instituto de Astronomı́a, UNAM 126 Short Talks Galaxies GAL -5 Probing the assembly of galaxy groups with intragroup light Eigenthaler, P.B1 Compact groups of galaxies are an environment where the evolution of galaxies occurs under extreme conditions due to the high spatial volume density of member galaxies and their low relative velocities implying that galaxy interactions should be frequent and efficient. N-Body simulations predict that compact groups should collapse in a small fraction of the Hubble time to a single elliptical, but retaining the extended Xray halo, forming so called fossil galaxy groups. Considering that fossil groups are the remnants of mergers in compact groups, the merger history of the progenitor group is expected to be imprinted in todays fossil groups. In recent years, a diffuse component of optical intragroup light (IGL) was detected in Hickson compact groups. A correlation between the structural properties of the IGL and indicators of dynamical evolution in compact groups like crossing time and the fraction of early-type galaxies has been found. Therefore, the IGL can be taken as a new tool to investigate the evolutionary stage and interaction history of compact groups. If fossil galaxy groups are indeed merged compact groups that assembled early in the universe, the observed correlations suggest a prominent and relaxed IGL component in fossil groups. No IGL has been detected so far in fossil groups. Once detected in these systems, its structure and kinematics will be a powerful diagnostic to study the evolutionary history of fossil groups. If fossil galaxy groups formed early, then stars dispersed within the IGL should have had enough time to form a relaxed and virialised IGL component tracing the dark matter halo of the host group. On the other hand, if the assembly of the central elliptical in fossils just happened recently, then a highly structured IGL would be expected because of the large relaxation timescales of such structures. Addressing these topics, I will highlight ongoing plans to detect the diffuse IGL component in fossil groups and present a kinematical study of the intragroup light in Hickson Compact Group 90 based on a Multi-Slit-Imaging-Spectroscopy (MSIS) technique. In this approach, planetary nebulae dispersed in the IGL are used as kinematical tracers via their characteristic [OIII] 5007Å line. The kinematic data will allow us to better understand the nature and origin of the IGL in compact groups and reveal its overall dynamical stage, virialised or unrelaxed. It is the first time that this technique is applied to the group environment. B [email protected] Instituto de Astrofı́sica, Facultad de Fı́sica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile 1 127 Galaxies Short Talks GAL -5 Backsplash Galaxies Muriel, H.1 ; Coenda V.B1 We explore the properties of galaxies on the outskirts of clusters and their dependence on recent dynamical history. Our aim is to know the real impact that the cluster core has on the evolution of galaxies. We analyze the photometric and spectroscopic properties of more than 1000 galaxies on the outskirts of 90 clusters (1 < r/rvir < 2) in the redshift range 0.05 < z < 0.10. Using the radial velocity of galaxies we selected high and low velocity subsamples. According to theoretical predictions, a significant fraction of the first subsample should be backsplash galaxies (BS), that is, objects that have already orbited near the cluster center. A significant proportion of the sample of galaxies of high relative velocity (HV) seems to be composed of in-falling objects. Our results show that, BS galaxies are on average redder, less luminous and smaller than HV. At fixed stellar mass, we found that late-type galaxies in the BS sample are systematically older and have formed fewer stars during the last 3 Gyrs than galaxies in the HV sample. This is consistent with models that assume that the central regions of clusters are effective in quenching the star formation by means of processes like ram pressure stripping or strangulation. At fixed stellar mass, BS galaxies tend to have higher surface brightness and smaller size than HV galaxies. These results may be related to dynamical processes which determine that galaxies that have orbited the central regions of clusters are more likely to suffer tidal effects, such as the loss of part of their mass as well as a re-distribution of matter towards more compact configurations. Finally, we found a higher fraction of ET galaxies in the BS sample, supporting the idea that the central region of clusters of galaxies can contribute to the transformation of morphological types towards earlier types. B 1 [email protected] IATE-OAC, Córdoba, Argentina 128 Short Talks Galaxies GAL -6 BUDHIES: a Blind Ultra Deep HI Environmental Survey Yara L. JafféB1 ; Bianca M. Poggianti; M. A. Verheijen; Jacqueline H. van Gorkom I will present recent results from the Blind Ultra Deep HI Environmental Survey (BUDHIES), that has detected over 150 galaxies at z ⇠ 0.2 with the Westerbork Synthesis Radio Telescope. Our multi-wavelength study is the first where optical properties and HI content are combined at a redshift where evolutionary effects begin to show. I will discuss the link between the environment, HI content, morphology, stellar mass and star formation in galaxies at z ⇠ 0.2, and the importance of different physical mechanisms in the transformation of galaxies. B 1 [email protected] Universidad de Concepcion 129 Galaxies Short Talks GAL -6 Emission line imaging survey of the Abell 901/902 supercluster Ana Chies-SantosB1 ; Bruno Rodriguez del Pino1 ; Alfonso Aragón-Salamanca1 ; Steven Bamford1 ; Meghan Grey1 It is widely debated whether galaxy evolution is more prone to internal or external effects. Trends to passive and/or more spheroidal populations in dense environments are widely observed and star-formation rate and stellar age and AGN fraction all correlate with measurements of the local galaxy density. However, in the hierarchical framework of galaxy formation the galaxies in the densest peaks start forming stars and assembling mass earlier making stellar mass one of the key determinants of galaxy properties. Nonetheless environmental effects are still very important and could be separated from the effect of internal galaxy properties. The Abell 901(a,b)/902 multiple cluster system at z ⇠ 0.165 is a unique laboratory for galaxy evolution. Besides three main clusters it includes a few related groups. The field comprises a very broad range of galaxy environments and masses at a single redshift. Therefore by observing this single region one is able to study galaxy evolution decoupling environmental and stellar mass effects from redshift-related ones. We are currently undertaking a survey of the region with the OSIRIS tunable filter imager on the GRANTECAN. We have targeted the H↵ and [NII] 6584 lines Together, these will provide the urgently needed star formation rate and AGN diagnostics for a full census of such properties in this field. In this talk I will present the first results of the survey on the high density regions A901a and A902 probing AGN and star formation. B 1 Ana.Chies [email protected] University of Nottingham, UK 130 Short Talks Galaxies GAL -6 The Next Generation Virgo Cluster Survey - Infrared (NGVS-IR) Thomas H. PuziaB1 ; Roberto Munoz1 ; Ariane Lancçon2 ; NGVS collaboration I will present a progress report of the most advanced near-UV/optical/near-IR photometric survey of the Virgo galaxy cluster that in the optical covers a total area of 104 square degrees from its core to its virial radius. The near-IR follow-up program (NGVS-IR) currently covers 20 square degrees around M87 and M49 and is being continuously expanded. After an overview of some technical aspects, I will discuss several primary science topics of the NGVS+NGVS-IR survey, in particular focussing on stellar population diagnostics in galaxies and star clusters. Combining near-UV, optical and near-IR data, we build the uiK color-color diagram of the pilot survey area. This displays significantly clearer substructure in the object distribution than the gzK diagram – the NGVS+NGVS-IR-equivalent of the classic BzK diagram, which is widely used in cosmological surveys. Most remarkably, the uiK diagram allows for a very clean color-based selection of globular clusters in Virgo. B 1 2 [email protected] Institute of Astrophysics, Pontificia Universidad Catolica de Chile University of Strasbourg 131 Galaxies Short Talks GAL -6 The UV GRB host galaxy luminosity function Schulze, S.B1 It is now well established that the progenitors of long gamma-ray bursts (GRBs) are collapsing massive stars. Hence, GRB-selected galaxy studies offer a new means to map the star formation in the Universe and the fundamental routes to the formation and the build-up of high-redshift galaxies. This approach is complementary to now well-established methods leading to the zoo of galaxy populations such as LBGs, SMGs, DRGs, LAEs, DLAs and EROs. At least for GRB host galaxies we are very sure that they point to galaxies that undergo an intense phase of star formation. Since the beginning of GRB host studies, it was highly debated whether GRBs are unbiased tracers of star-formation. This spawned The Optically Unbiased GRB Host Galaxy survey (TOUGH, Hjorth et al. 2012, ApJ, 756, 187). The goal of TOUGH was to make a systematic survey of GRB hosts regardless of burst or afterglow properties with the ESO/VLT that were complemented with the HST. In total, the TOUGH sample comprises 69 localized GRBs, of which 80While the observed GRB host luminosity function matches very well a star-formation-rate weighted LBG luminosity function at 2 < z < 3, we find a clear lack of luminous galaxies at lower and higher redshifts. I will comment on the possible origins of the lack of luminous galaxies and its implications on using GRB hosts as tracers for star formation. B 1 [email protected] Pontificia Universidad Católica de Chile 132 Short Talks Galaxies GAL -6 The Andromeda galaxy M31 in the era of precision cosmology David Valls-GabaudB1 With the advent of precision cosmology, where predictions and measurements can be carried out to a precision level of a few percent, understanding galaxy formation and evolution to the same level of detail appears to be essential for further tests of the paradigm. Here we review recent attempts at (1) understanding the 3-dimensional structure of the satellite system around M31, where half of the dwarfs appear to be orbiting in a vast and thin disc; (2) anchoring M31 very accurately using three independent methods for measuring its distance and hence the Hubble constant; and (3) establishing the variations of star-formation histories across the galaxy through the analysis of the colour-magnitude diagrams of resolved stellar populations. B 1 [email protected] LERMA, Observatoire de Paris, France 133 Galaxies Short Talks COS -3 A data-driven approach to the emission line properties of star-forming galaxies Sodre Jr., L.B1 ; Sirico, A. C. A.1 We present here a quantitative analysis of the correlations between the continuum and emission line equivalent widths, as well as between the equivalent widths of different lines, for a sample of more than 100,000 star-forming galaxies with high S/N spectra and with spectral synthesis performed with the Starlight software. We have done, initially, a Principal Component Analysis (PCA) of the synthesized continuum spectra and used up to 10 components to train an artificial neural network to estimate the equivalent width of Halpha, with excellent results, demonstrating that there is indeed a strong correlation between the continuum and the H-alpha equivalent width. We have also shown, using statistical tools such as the distance correlation and maximal information correlation, that there are important correlations between the most prominent emission lines usually detected in the optical region of galaxy spectra. The main motivation behind this work is to produce realistic spectra for tests of data reduction pipelines of the new generation of galaxy surveys, like the PFS/SuMIRe. B 1 [email protected] IAG-USP 134 Short Talks Galaxies GAL -7 The LMC outer disk stellar population in the light of the Dark Energy Survey Balbinot, E.B1,2 ; Santiago, B.1,2 ; Girardi, L4 ; da Costa, L. N.2,3 ; Maia, M. A. G.2,3 The outermost regions of the Large Magellanic Clouds (LMC) have recently been covered by Dark Energy Camera (DECam) Science Verification data, in preparation for the Dark Energy Survey (DES). Although the DES footprint misses the bar and main star forming regions of the LMC, the available data sample a large and continuous area of the LMC disk down to r ' 24 at distances greater than 5 degrees from its center. This large surveyed region opened the possibility to study the outer LMC star formation history (SFH) with unprecedented detail. In this work we employ the partial models method (Gallart et al 1999; Javiel et al 2005) to recover the SFH and its spatial variations in the outskirts of the LMC from the observed colour-magnitude diagrams. We take the MW foreground stars into account by modelling them with TRILEGAL (Girardi et al. 2005). With this technique we were able to recover the spatial dependency of the LMC outer components SFH and estimate its extension as well as the inclination and depth of the LMC disk. As a byproduct of our analysis we assembled a catalog of new LMC stellar clusters. B 1 2 3 4 [email protected] Instituto de Fı́sica UFRGS Laboratório Interinstitucional de e-Astronomia Observatório Nacional Osservatorio Astronomico di Padova, INAF 135 Galaxies Short Talks GAL -7 The satellite population of Milky Way/Andromeda-sized galaxies Avila-Reese, V.B1 ; Rodriguez-Puebla, A.1 A galaxy group mock catalog is constructed on the basis of stellar-to-(sub)halo mass relations constrained by currently available observations (central and satellite galaxy stellar mass functions, correlation functions). Many thousands of central galaxies of MW and M31 stellar masses are used to study several occupational distributions of their massive satellites as well as the cumulative satellite mass functions in general. We provide also lower limits to the halo masses of MW and M31. Our analysis strongly suggests that the abundance of subhalos agrees with that ones of satellites in all MW- and M31-sized hosts, i.e., there is not a (massive) satellite missing problem for the LCDM cosmology. However, we confirm an internal dynamics problem for the satellites smaller than ms ⇠ 108 M ; at difference of previous works, this conclusion is not limited to the particular case of the MW but it refers to the overall population of MWM31-sized galaxies. Some pieces of evidence suggest that this issue could refer only to satellite dwarfs but not to central dwarfs, in which case astrophysical and environmental effects could be at the basis of the found differences. B 1 [email protected] Instituto de Astronomı́a, Universidad Nacional Autónoma de México 136 Short Talks Galaxies GAL -7 Star formation outside the Elliptical Galaxy NGC2865 Urrutia-Viscarra, F.B1,2 ; Arnaboldi, M.2 ; Mendes de Oliveira, C.1 ; Torres-Flores, S.3 ; de Mello, D.4 ; Carrasco, R.5 Tidal debris, rich in HI gas, formed in interacting and merging systems, may be ideal laboratories to study star formation outside galaxies. We have searched for young stellar complexes in different systems with optical and/or gaseous tidal tails, all of them with available archive GALEX/UV images. One of these systems is NGC2865, which presents a ring of HI around the main galaxy. Using the Multi-Slit Imaging Spectroscopy Technique, we detected all H↵ emitting sources in the surroundings of the galaxy NGC2865, down to a flux limit of 10 18 [erg cm 2 s 1 A 1 ]. In total, we found seven emission-line sources in a 5 x 5 arcmin (60 x 60 kpc) field over the southern tail of HI present around the galaxy NGC2865. These regions are young sources with stellar masses in the range 4x103 M to 17x106 M , coincident with the location of the intergalactic HI gas, where the probability to form stars is expected to be low. Given these physicals parameters, the regions are considered young star forming regions (or clusters), born outside the galaxy. The relevance of these observations is discussed. B 1 2 3 4 5 [email protected] Universidade de Sao Paulo, IAG European Southern Observatory, Garching Universidad de La Serena Catholic University of America Gemini Observatory, Southern Operations Center. 137 Galaxies Short Talks GAL -7 Galaxy evolution-Star formation connection: from pc to kpc scales Melioli, C.B1 ; de Gouveia Dal Pino, E. M.1 Energization of the interstellar medium by supernova explosions covers a crucial role in a number of astrophysical situations. Supernova explosions are important for the gas evolution on small scales, because they drive turbulence and are able to provide a self-regulation mechanism for star formation. Besides, their blast waves may also form molecular clouds by sweeping gas into a turbulent flow. The gas heated by supernova explosions may also acquire an expansion velocity larger than the escape velocity and leave the galaxy through a supersonic wind. The interplay between supernova explosions, stellar winds and interstellar medium is, therefore, important also for the gas evolution at large scales, playing important role on the dynamical and chemical evolution of different galactic sistems, like dwarf, spiral and starburst galaxies and affecting their metalicities, the surface brightness, the total gas mass evolution and the star formation rate itself. Diffuse magnetic fields may play an important role over all these processes, because they reduce the compressibility of a fluid and toghether with the turbulent energy may dominate over the thermal energy in many interstellar environments, providing an important component of the verical pressure that supports the interstellat medium, preventing the vertical expansion of superbubbles and driving galactic outflows by cosmic ray and Alfven wave pressure. In this study we will review these mechanisms and also show 3D MHD simulations of SN-driven turbulence in star formation regions (at small scales) and SN-driven galactic winds (at large scales), demonstrating that stellar feedback may be able to drive new star formation processes, but is unable to change significantly the metal abundance of the surrounding environment of the galaxies. B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências, Universidade de Sao Paulo 138 Short Talks Galaxies GAL -7 Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust Hugo MessiasB1 ; Gustavo Orellana1 ; Shane Bussmann2 ; Jae A. Calanog3 ; Helmut Dannerbauer4 ; Simon Dye5 ; Simone Fleuren6 ; Hai Fu7 ; Edo Ibar8 ; Rob Ivison9,10 ; Andrew Inohara3 ; Neil Nagar1 ; Mattia Negrello11 ; Alain Omont12 ; Dominik A. Riechers7,13 ; Yun-Kyeong Sheen1 ; Simon Amber14 ; Nathan Bourne5 ; Mark Birkinshaw15 ; Dave Clements16 ; Asantha Cooray3,7 ; Stephen Eales16 ; Ricardo Demarco1 ; Loretta Dunne17 ; Roxana Lupu18 ; Steve Maddox17 ; Michal Michalowski9 ; Dan Smith19 ; Matt Smith20 ; Elisabetta Valiante20 ; Gianfranco De Zotti11 This work focus in one lensed system selected via the Negrello et al.(2010) criterion in the Herschel-ATLAS field. Gathering a rich multi-wavelength data-set, we have modelled the background source’s morphology and dynamics, as well as assessed its star-formation rate (SFR) and stellar, dust, and gas (molecular and neutral) contents. The system is comprised by a foreground edge-on disc galaxy (at zsp = 0.218) and an almost complete Einstein ring around it, with possibly a quad-lens morphology. The background source is at zsp = 1.027 and is magnified by a factor of ⇠4. The lens modelling is more successful in the millimetre range, and supports a merger system scenario. Evidences for this come from the clumpy morphology of the reconstructed source-plane, as well as a tidal-feature observed at 1.1 µm, also predicted by the lens-modelling of the CO(4!3) emission. The SED modelling yields a SFR of 509 M yr 1 , in agreement with that estimated at radio frequencies. The stellar and dust masses are, respectively, 7.6 ⇥ 1010 M and 10 1.69 ⇥ 109 M . We estimate a total molecular gas mass of MH2 = 4.86+3.21 1.31 ⇥ 10 M and a total ISM mass of MISM = 1.1 ± 0.5 ⇥ 1011 M . The comparison between the millimetre and radio range yields no evidence for active galactic nucleus activity. This pilot study joining Herschel and ALMA shows the strength of large-field far-IR surveys combined with a follow-up facility such as ALMA, as a means for a systematic study of GL systems. The results already show ALMA as the ultimate tool to study GL systems, as driven by its high spectral and spatial resolution coupled with its detectability power and integral-field spectroscopy capability. B [email protected] Universidad de Concepcion, Chile 2 Harvard-Smithsonian Center for Astrophysics, Cambridge, USA 3 University of California, Irvine, USA 4 Universitä Wien, Austria 5 University of Nottingham, UK 6 Queen Mary University London, UK 7 California Institute of Technology, Pasadena, USA 8 Pontificia Universidad Catolica de Chile, Santiago, Chile 9 UK Astronomy Technology Centre, Edinburgh, UK 10 University of Edinburgh, UK 11 INAF, Padova, Italy 12 Institut d’Astrophysique de Paris, France 13 Cornell University, Ithaca, USA 14 The Open University, United Kingdom 15 Bristol University, UK 16 Imperial College London, UK 17 University of Canterbury, New Zealand 18 School of Arts & Sciences, USA 19 University of Hertfordshire, UK 20 Cardiff University, UK 1 139 140 AGN AGN -1 IFU properties of 10 Early-type galactic nuclei Ricci, T. V.B1 ; Steiner, J. E.1 ; Menezes, R. B.1 Active galactic nuclei (AGN) are commonly associated with the capture of matter by a supermassive black hole (SMBH), located at the central region of galaxies. In the optical, they are characterized by intense and broad emission lines. Quasars are the most luminous type of AGNs, both in optical and in radio. On the other hand, Seyfert galaxies, with prominence of high ionization lines, and low ionization nuclear emission regions (LINERs), whose low ionization emission lines tend to be more intense, belong to the low luminosity regime of AGNs. We analyzed the central region of 10 Early-type galaxies with the GMOS-IFU spectrograph on Gemini South telescope in order to detect and characterize low luminosity AGNs. The sample galaxies are massive ( > 200 km s 1 ) and have distances up to 30 Mpc. Using PCA Tomography and spectral synthesis techniques in order to isolate the gas from stellar emission, we show that all galaxies of the sample possess emission lines in their nuclei. Using standard spectral analysis, we show that all objects may be classified as LINERs. In six galaxies, we detected a broad H↵ component, which confirms the presence of an AGN in these objects. B 1 [email protected] IAG - Universidade de São Paulo 141 AGN Short Talks AGN -1 Co-evolution of Supermassive Black Holes and Galaxies in the near Universe Thaisa Storchi-BergmannB1 Although the bulk of the supermassive black hole (SMBH) growth has occurred at redshifts higher than 2, the feeding processes cannot be resolved at the corresponding distances. It is in the near Universe that these processes – which take place within the inner few hundred parsecs of active galaxies – can be probed down to ⇠ 10 pc spatial resolution. I will discuss integral field spectroscopic observations of the inner kiloparsec of nearby active galaxies which reveal the presence of gas reservoirs and inflows along nuclear spirals and filaments. The derived mass inflow rates are ⇠ 3 orders of magnitude larger than the mass accretion rate to the SMBH and can lead, during an activity cycle, to the accumulation of enough gas in the inner few hundred pc’s to trigger the formation of new stars. This result suggests that co-evolution of SMBH and galaxies is still occurring in the near Universe. The observations also reveal the presence of outflows at similar mass flow rates to that of the inflows, although the inflows are best seen around LINER nuclei and the outflows around Seyfert nuclei, what may imply evolution between these two types of activity. B 1 [email protected] Instituto de Fı́sica, Universidade Federal do Rio Grande do Sul 142 Short Talks AGN AGN -1 Gap Formation in Circumbinary AGN Disks Escala, A.B1 ; Del Valle, L.1 We numerically study the formation of gaps in circumbinary disks of comparable mass massive black hole binaries (q ⇠ 1). We vary the disk properties (mass, termodynamics, etc.) and found that most massive and thicker disks are able to prevent the gap formation in them. We contrast our results against analytical models based on the non-axisymetric perturbation enhanced in the disk, which succesfully predicts the disks that opens a gap. We discuss the implications for the occurence of opened and failed gaps in the final separations and posible merging of binary AGNs. B 1 [email protected] Universidad de Chile 143 AGN Short Talks AGN -1 Coronal Emission in the Active Galactic Nuclei and its relationship to outflows Rodriguez-Ardila, A.B1 ; Mazzalay, Z.2 ; Riffel, R.3 SOAR/Goodman spectroscopy is employed to detect the coronal lines [Fe VII] 3759, 5159, 6087 Å, [Ne V] 3423 Å and [Fe X] 6083 Å, in a sample of 12 active galactic nuclei (AGN). The three [Fe VII] lines are found to be suitable to determine the temperature and density of the high-ionization gas, allowing us to determine, for the first time, the physical conditions of the coronal line region in these objects. The spectra are also employed to fully characterize the profiles of the most conspicuous coronal lines and the low ionization gas (asymmetries, shifts from the centroid position, line width and kurtosis) and to relate these properties to the presence of nuclear ouflows. The combined results allow us to associate the detection of broad highly assymmetric forbidden line profiles to hot (Te > 3 ⇥ 104 K) and high-density (ne > 104 cm 3 ) gas, suggesting that it originates very likely from nuclear outflows. Most of the coronal emission is highly compact. However, in a few objects, coronal emission up to 1000 from the galaxy nucleus is detected, mostly in radio-sources, suggesting that shocks between the radio-jet and the ISM medium can also be responsible for the emission of highly ionized species. All above results allow us to confirm the role that coronal lines have to trace outflows either at the inner regions or at kiloparsec scales of AGNs. B 1 2 3 [email protected] Laboratorio Nacional de Astrofı́sica / MCTI Max-Planck-Institut für Extraterrestrische Physik Universidade Federal do Rio Grande do Sul 144 Short Talks AGN AGN -2 Gas dynamics in the Galactic Centre: clump accretion and outflows Cuadra, J.B1 We present numerical models of the gas dynamics in the central parsec of the Galaxy, from its origin as stellar winds, until its capture by Sgr A*, the central massive black hole. We show that the gas forms a two-phase medium, with cold clumps embedded in a hot tenuous gas. We find the accretion rate to be variable, due to the effect of the stellar orbits and the stochastic accretion of clumps. We suggest that the recently discovered infalling cloud, G2, could be one of the predicted clumps. We also study the possibility of detecting the effect of a recent outflow from Sgr A*. B 1 [email protected] Instituto de Astrofı́sica, Pontificia Universidad Católica de Chile 145 AGN Short Talks AGN -2 Parsec-scale Activity in BL Lacertae: Signature of Relativistic Jet Precession Caproni, A.B1 ; Abraham, Z.2 ; Monteiro, H.3 BL Lacertae is the prototype of the BL Lac class of active galactic nuclei. High-resolution interferometric images at radio wavelengths show the presence of a compact core and a diffuse halo-like source at arcsecond scales, while at an intermediate resolution (< ⇠ 10 mas), BL Lacertae shows a core-jet structure. At parsec scales, BL Lacertae exhibits intensive activity, such as intense core variability and multiple ejections of superluminal jet components, with components following different trajectories on the plane of the sky. In this work we analyze temporal changes of the observed right ascension and declination core-component offsetsin BL Lacertae in terms of our relativistic jet-precession model. The seven free parameters of our precession model were optimized via a heuristic cross-entropy method, comparing the projected precession helix with the positions of the jet components on the plane of the sky and imposing constraints on their maximum and minimum superluminal velocities. Our optimized best model is compatible with a jet having a bulk Lorentz factor of 5.4, which is precessing with a period of about 12.1 yr in the observer’s reference frame and changing its orientation in relation to the line of sight between 4o and 5o , approximately. B 1 2 3 [email protected] Núcleo de Astrofı́sica Teórica - Universidade Cruzeiro do Sul Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas - Universidade de São Paulo Instituto de Ciências Exatas - Universidade Federal de Itajubá 146 Short Talks AGN AGN -2 The incidence of short time scale variability on different types of Blazars Andruchow, I.B1,2 ; Cellone, S. A.1,2 ; Romero, G. E.1,3 Active Galactic Nuclei (AGNs) have an extreme behavior at almost all wavelengths. In particular, the kind of AGNs know as blazars are one of the most extreme. With their jets pointing near to our direction, those object show a variety of distinctive features from radio to very high energies. We present the results of an extended campaign to study the behavior of the optical emission of blazars. This work is centered on variability at short scales of both the total flux (at different optical wavebands) and the linear optical polarization. We took special care in data treatment, e.g. considering the influence of the host galaxies, the good choice of the field stars used for differential photometry, the statistical test used to study the variability, etc. Over the last years, we specially followed blazars that were detected at very high energies (TeV). We found differences in the incidence of variability at short time-scales between blazars that have the peak of their synchrotron flux low frequencies from those that have it at high energies. B 1 2 3 [email protected] Facultad de Ciencias Astronómicas y Geofı́sicas, UNLP Instituto de Astrofı́sica de La Plata, CONICET Instituto Argentino de Radioastronomı́a, CONICET. 147 AGN Short Talks AGN -2 The Multiwavelength Study of OH Megamaser Galaxy IRAS16399-0937 Dinalva A. SalesB1 ; A. Robinson; D. J. Axon; J. Gallimore; P. Kharb; R. L. Curran; C. O’Dea; S. Baum; R. Mittal In this work we present a spectacular morphology of OH Megamaser galaxy (OHMG) IRAS16399-0937 taken from our HST snapshot imagery program. We also conduce a detailed multi-wavelength analysis of IRAS163990937 using HST/NICMOS, 2MASS, Spitzer (IRAC, IRS, and MIPS) as well as Herschel/SPIRE data archive. The HST H↵+[NII] and F814W image of IRAS16399-0937 reveal a dual point like source seeming in the middle to final stage of interaction with a projected separation of ⇠ 6 (3.4 kpc) with a dust lane crossing through LINER (North) and Starburst (South) nuclei and a bright tail arc of dust and gas connecting a both nuclei. The North and South nuclei, as well as interstellar medium (ISM) of this merger system show strong feature of the polycyclic aromatic hydrocarbons (PAH) molecules, which is indicator for recent star formation activity, in the mid-IR (MIR) Spitzer spectra. However, the MIR spectrum of the whole IRAS16399-0937 system presents only ionic emission lines with low ionization potential (IP < 50 eV) and no evidence of those that is a clear indicator of powerful AGN activity. The same scenario was found to that nucleus (North) classified as active galactic nuclei (AGN) in the optical wavelength. In spite of the lack of a direct evidence of AGN activity to the North nucleus the decomposition of the optical - FIR spectral energy distribution (SED) using our own tool, CLUMPY DREAM, find a moderately powerful AGN (Lbol ⇠ 1.24 ⇥ 1044 ergs/s) quite embedded in a clumpy torus environment. Overall, our observations emphasize a presence of an AGN and Starburst nuclei in major IRAS16399-0937 merger. B 1 2 3 [email protected] Department of Physics, Rochester Institute of Technology, 84 Lomb Memorial Drive, Rochester, NY 14623, USA Department of Physics Bucknell University Lewisburg, PA 17837, USA Indian Institute of Astrophysics, II Block, Koramangala, Bangalore - 5600034, India 148 Short Talks AGN AGN -3 AGN torus properties with WISE B1,2 Nikutta, R. ; Nenkova, M.3 ; Hunt-Walker, N.4 ; Ivezic, Z.4 ; Elitzur, M.2 The WISE satellite mission has collected an unprecedented infrared dataset. Its four photometric filter bandpasses at 3.4, 4.6, 12 and 22 micron enable studies of dust emission from various astronomical sources, including quasars and Active Galactic Nuclei (AGN). With its sensitivity up to 1000 times better than previous missions (e.g. IRAS) and a spatial resolution between 6 and 12 arcsec, WISE measured brightness and colors on hundreds of millions of point sources, and among them many tens of thousands of AGN. Using a large cross-matched sample of previously classified SDSS objects, we define reliable selection criteria for type-1 AGNs with dust torus emission. Aided by our large database of CLUMPY torus models (Nenkova et al. 2008a,b), we identify the ranges of model parameter values supported by WISE observations, and derive likely properties of AGN tori in general. Unlike previous studies, this AGN torus characterization has been performed with high statistical significance thanks to the unprecedentedly large sample size. For the very first time we are now able to predict the number of observable type-2 AGN from an observed sample of unobscured type-1 objects. We also derive color selection criteria for type-2 sources using best-fit models for confirmed type-1 sources but with complementary viewing angles (i.e. preferentially edge-on lines of sight). We find that type-2 objects are type-2 precisely because they are intrinsically more likely to be observed along optically obscured lines of sight: type-1 and type-2 AGN have significantly different dust covering factors and line-of-sight photon escape probabilities. Finally, using recent studies of BL Lac objects, we show that in certain configurations CLUMPY torus models are compatible with the relatively blue WISE colors seen in these sources. B 1 2 3 4 [email protected] Departamento de Ciencias Fisicas, Universidad Andres Bello, Santiago/Chile Department of Physics and Astronomy, University of Kentucky, Lexington/USA School of English and Liberal Studies, Seneca College, Toronto/Canada Astronomy Department, University of Washington, Seattle/USA 149 AGN Short Talks AGN -3 HST and Spitzer point source and dust lane detection in powerful narrow-line radio galaxies Edgar A. RamirezB1 ; C. N. Tadhunter2 ; D. Dicken3 ; M. Rose2 ; D. Axon4,5 ; W. Sparks6 We present the analysis of infrared HST and Spitzer data for a sample of 13 FRII powerful radio galaxies at 0.03 < z < 0.11 that are optically classified as narrow-line radio galaxies (NLRG). Under the context of the unified schemes of Active Galactic Nuclei (AGN), the direct view of the AGN in NLRG is impeded by a parsecscale toroidal structure when this is viewed edge-on. Our high resolution infrared observations provide new information about the optical extinction, orientation, and direct AGN detection of the inner kpc-scale region of the AGN. We have found that the point-like nucleus detection rate increases from 25% detected at 1.025 µm to 80% and 100 detection rate at 2.05 and 8 µm, respectively. This detection towards longer infrared wavelengths supports the idea that a large proportion of NLRG host an obscured AGN in their centre. Furthermore, at 1.025 µm, we detect a kpc-scale dust lane in 70% of our sample, of which 55% are perpendicular to their inner kpc radio jet axis. Assuming that the torus is perpendicular to the radio jet, this suggests a continuity from the parsec-scale torus to the kpc-scale dust lane. The optical extinction produced by the obscuring structures have been estimated from X-rays, near-IR and mid-IR data using five different methods. All the extinction estimates are consistent (AV = 3 170 mag), with the exception of that estimated using the silicate absorption line, which is lower (AV = 0 25 mag). This discrepancy challenges the simplified idea of an homogeneous dust torus extinguishing the AGN light as a foreground screen. The disagreement can be explained by thermal mid-IR emission from an extended narrow-line region, by non-thermal emission from the base of the radio jets, or by a clumpy torus model diluting the silicate absorption line. B 1 2 3 4 5 6 [email protected] IAG- U. Sao Paulo Department of Physics and Astronomy, University of Sheffield Institut d’Astrophysique Spatiale, Université Paris Sud Physics Department, Rochester Institute of Technology School of Mathematical and Physical Sciences, University of Sussex SpaceTelescope Science Institute, Baltimore 150 Short Talks AGN AGN -3 Collimation and scattering of the AGN emission in the Sombrero galaxy Menezes, R. B.B1 ; Steiner, J. E.1 ; Ricci, T. V.1 M104, the Sombrero galaxy, is a highly inclined (nearly edge-on) SA(s)a galaxy at a distance of about 9.2 Mpc. Based on its optical emission line spectrum, the nucleus of this object has been classified as a LINER (Low Ionization Nuclear Emission-line Region). We present an analysis of a data cube of the central region of M104, obtained with the GMOS-IFU of the Gemini-South telescope, and report the discovery of collimation and scattering of the AGN emission in the circum-nuclear region of this galaxy. Analysis with PCA Tomography and spectral synthesis revealed the existence of collimation and scattering of the AGN featureless continuum and also of a broad component of the H↵ emission line. The collimation and scattering of this broad H↵ component was also revealed by fitting the [N II] 6548, 6583 and H↵ emission lines as a sum of Gaussian functions. The spectral synthesis, together with a V-I image obtained with the HST, showed the existence of circum-nuclear dust, which may cause the light scattering. We also identify a dusty feature that may be interpreted as a torus/disk structure. The existence of two opposite regions with featureless continuum along a direction perpendicular to the torus/disk suggests that this structure is approximately edge-on and collimates the AGN emission. The edge-on torus/disk also hides the BLR. The proposed scenario is compatible with the Unified Model and explains why only a weak broad component of the H↵ emission line is visible and also why many previous studies detected no broad H↵. B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo 151 AGN Short Talks AGN -3 The Role of AGN Feedback in the Evolution of Seyfert Galaxies Mueller-Sanchez, F.B1 ; Malkan, M.1 ; Hicks, E.2 ; Davies, R.3 Adaptive optics integral-field observations of Seyfert Galaxies have recently revealed clear evidence of AGNdriven outflows of ionized gas. By resolving the inner 10-20 parsecs, we are successfully modeling the geometry and kinematics of the outflows in 3D. The model parameters are used to estimate mechanical feedback from the AGN and test unification models. The mass outflow rates are 2–3 orders of magnitude greater than the accretion rates, but they are comparable to the estimated inflow rates to the central 10-25 pc, suggesting that the outflows may remove a considerable amount of the infalling gas before it reaches the accretion disk. The outflows seem to form two distinct groups which differ by outflow power variations with radio flux. While powerful outflows (with kinetic powers > 1.0% Lbol) are observed in objects with extended radio jets, in the other AGN -in which the outflow power is less than 0.1% Lbol- the radio jet is weak and compact. B 1 2 3 [email protected] University of California Los Angeles University of Washington MPE, Germany 152 Cosmology COS -1 The Local Group in a explicit cosmological context Jaime E. Forero-RomeroB1 ; Yehuda Hoffman2 ; Sebastian Bustamante3 ; Stefan Gottloeber4 ; Gustavo Yepes5 In this talk we present recent results on the effort to simulate the Local Group (LG, composed by the Milky Way and M31) in a explicit cosmological context. The main results are obtained through cosmological Nbody simulations which use constrained initial conditions that aim at reproducing the observed large scale environment. We show that in the constrained simulations there is a bias in the formation properties of the simulated LG and also that the observed radial motion of Andromeda towards us is not common in the context provided by LCDM. In the effort to better understand these results, we finish by discussing preliminary results on the effect of the cosmic web on the formation of LG-like systems. B 1 2 3 4 5 [email protected] Departamento de Fisica, Universidad de los Andes, Colombia Racah Institute of Physics, Hebrew University of Jerusalem Instituto de Fisica - FCEN, Universidad de Antioquia Leibniz Institut fuer Astrophysik - Potsdam Grupo de Astrofisica, Departamento de Fisica Teorica, Universidad Autonoma de Madrid 153 Cosmology Short Talks COS -1 Cosmology from the Angular Correlation Function and Galaxy Clusters Marcos LimaB1 ; Hugo Camacho; Michel Aguena; DES-Brazil consortium The large-scale clustering properties of galaxies allows us to investigate models which attempt to explain the recent acceleration of the Universe background expansion. These properties include the correlations of galaxies and the abundance of galaxy clusters. I will present some of the relevant aspects when using these probes to constrain cosmological models. If time allows I will also present some of our recent results on real data from the Sloan Digital Sky Survey DR8 and on mock catalogs of the Dark Energy Survey. B 1 [email protected] Instituto de Fı́sica, Universidade de São Paulo 154 Short Talks Cosmology COS -1 Halo-based reconstruction of the cosmic mass density field Muñoz-Cuartas, J. C.B1 ; Müller, V.2 ; Forero-Romero, J. E.3 We present the implementation of a halo-based method for the reconstruction of the cosmic mass density field. The method employs the mass density distribution of dark matter haloes and its environments computed from cosmological N-body simulations and convolves it with a halo catalogue to reconstruct the dark matter density field determined by the distribution of haloes. We applied the method to the group catalogue of Yang et al. built from the Sloan Digital Sky Survey (SDSS) Data Release 7. As a result we obtain reconstructions of the cosmic mass density field that are independent of any explicit assumption of bias. We describe in detail the implementation of the method, present a detailed characterization of the reconstructed density field (mean mass density distribution, correlation function and counts in cells) and the results of the classification of large-scale environments (filaments, voids, peaks and sheets) in our reconstruction. Applications of the method include morphological studies of the galaxy population on large scales and the realization of constrained simulations. B 1 2 3 [email protected] Instituto de Fisica, Universidad de Antioquia, Medellin-Colombia Leibniz-Institut für Astrophysik Potsdam Departamento de Fisica, Universidad de los Andes, Bogota-Colombia 155 Cosmology Short Talks COS -1 Globular clusters as tracers of the hierarchical formation of the Milky Way Carballo-Bello, J. A.B1,2,3 ; Martı́nez-Delgado, D.4 ; Sollima, A.5 ; Muñoz, R.1 Globular clusters have played an important role in the study of the processes that led to the formation of our Galaxy. Moreover, the dual Galactic globular cluster system is considered a manifestation of its hierarchical formation in the context of the Lambda-CDM scenario. Wide-field imaging - as the one obtained in our work - and follow-up spectroscopy are crucial tools to unveil the remnants of their progenitor dwarf galaxies, already assimilated by the Milky Way. In this talk, I will review some of the clues pointing to the external origin of an important fraction of the Galactic globular clusters and the importance of these interesting stellar systems in the searching for known and unknown halo substructures and tidal streams. B 1 2 3 4 5 [email protected] Departamento de Astronomı́a, Universidad de Chile Instituto de Astrofı́sica de Canarias Departamento de Astrofı́sica, Universidad de La Laguna Max Planck Institut für Astronomie Osservatorio Astronomico di Bologna 156 Short Talks Cosmology COS -1 Huge-LQG- the largest structure in the universe Roger G. Clowes ; Srinivasan Raghunathan2 ; Kathryn A. Harris3 ; Luis E. CampusanoB2 ; Ilona K. Sochting4 ; Matthew 1 J. Graham5 A large quasar group (LQG) of particularly large size and high membership has been identified in the DR7QSO catalogue of the Sloan Digital Sky Survey. It has characteristic size (volume1/3 ) ⇠ 500 Mpc (proper size, present epoch), longest dimension ⇠ 1240 Mpc, membership of 73 quasars and mean redshift z=1.27. In terms of both size and membership, it is the most extreme LQG found in the DR7QSO catalog for the redshift range 1.0 < z < 1.8 of our current investigation. Its location on the sky is ⇠ 8.8 degrees north (⇠ 615 Mpc projected) of the Clowes & Campusano LQG at the same redshift, z=1.28, which is itself one of the more extreme examples. This new, Huge-LQG appears to be the largest structure currently known in the early Universe. Its size suggests incompatibility with the Yadav et al.(2010) scale of homogeneity for the concordance cosmology, and thus challenges the assumption of the cosmological principle. B 1 2 3 4 5 [email protected] Jeremiah Horrocks Institute, University of Central Lancashire, UK Departamento de Astronomı́a, Universidad de Chile, Santiago, Chile Department of Physics, Virginia Tech, Blacksburg, VA Astrophysics, Denys wilkinson Building, Keble Road, University of Oxford, UK California Institute of Technology, Pasadena, CA 157 Cosmology Short Talks COS -2 The SOAR Gravitational Arc Survey B1 Makler, M. 2,3 ; Furlanetto, C. ; Santiago, B. X.2,3 ; Caminha, G. B.1 ; Cypriano, E.4 ; Cibirka, N.4 ; Pereira, M. E. S.1 ; Bom, C. R. D.1 ; Lima, M. P.1,5 ; Brandt, C. H.1 ; Neto, A. F.3 ; Estrada, J.6 ; Lin, H.6 ; Hao, J.6 ; McKay, T. M.7 ; da Costa, L. A. N.3,8 ; Maia, M. A. G.3,8 We present the first results of the SOAR Gravitational Arc Survey (SOGRAS). The survey imaged 47 clusters in two redshift intervals centered at z = 0.27 and z = 0.55, targeting the richest clusters in each interval. Images were obtained in the g 0 , r0 and i0 bands with a median seeing of 0.83, 0.76 and 0.71 arcsec, respectively, in these filters. Most of the survey clusters are located within the Sloan Digital Sky Survey (SDSS) Stripe-82 region and all of them are in the SDSS footprint. We present the first results of the survey, including the 6 best strong lensing systems, photometric and morphometric catalogs of the galaxy sample, and cross matches of the clusters and galaxies with complementary samples (spectroscopic redshifts, photometry in several bands, X-ray and Sunyaev Zel’dovich clusters, etc.), exploiting the synergy with other surveys in Stripe-82. We apply several methods to characterize the gravitational arc candidates, including the Mediatrix method (Bom et al. 2012) and ArcFitting (Furlanetto et al. 2012), and for the subtraction of galaxy cluster light. Finally, we apply strong lensing inversion techniques to the best systems, providing constraints on their mass distribution. The analyses of a spectral follow-up with Gemini and the derived dynamical masses are presented in a poster submitted to this same meeting (Cibirka et al.). Deeper follow-up images with Gemini strengthen the case for the strong lensing nature of the candidates found in this survey. B 1 2 3 4 5 6 7 8 [email protected] Centro Brasileiro de Pesquisas Fı́sicas Departamento de Astronomia, Universidade Federal do Rio Grande do Sul Laboratório Interinstitucional de e-Astronomia Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo Instituto Nacional de Pesquisas Espaciais Center for Particle Astrophysics, Fermi National Accelerator Laboratory Department of Physics, University of Michigan Observatório Nacional 158 Short Talks Cosmology COS -2 A Systematic Study of the NFW and SIS Elliptical Lensing Models in the Strong Regime Dúmet-Montoya, H. S.B1 ; Caminha, G. B.1 ; Makler, M.1 The increasing number of gravitational arc systems expected to be detected in the next generation widefield surveys requires the fast numerical evaluation of lensing quantities to obtain the matter distribution of lenses and to make predictions for arc statistics in several cosmologies. It is therefore useful to employ approximate (or semi-analytical) methods to speed up the numerical computations. In this presentation we discuss two such classes of methods.The first one is to use pseudo-elliptical models (with lensing potential constant over ellipses) instead of elliptical ones (with surface mass density constant over ellipses), which are more physically motivated, but more computationally complex. The second one is to use the Perturbative Approach (PA) that provides approximate solutions for the lens equation near the tangential critical curve, leading to analytic solutions for arcs. We present our recent progress on inverse modelling and arcs statistics for models based on the Singular Isothermal Sphere (SIS) and Navarro–Frenk–White (NFW) density profiles, widely used to represent lenses from galaxy to cluster of galaxies mass scales. We derive analytic solutions for the Singular Isothermal Ellipsoid (SIE) and Elliptic Potential (SIEP), which are valid even in the presence of constant convergence and shear fields. These solutions include i) the lens equations for elliptical finite sources, ii) iso-convergence contours and constant distortion curves (including critical curves) and iii) the deformation cross section. We also investigate the mapping between the Elliptic and Pseudo-Elliptic NFW models (ENFW and PNFW) deriving constraints on the ellipticity as a function of convergence such that the PNFW can replace the ENFW to represent the mass distribution and deformation cross section. In the limit of small characteristic convergences we obtain analytic solutions for i) iso-convergence contours and constant distortion curves and ii) the deformation cross section. We implemented the PA for pseudo-elliptical models deriving analytic solutions for i) the lens equations for finite sources, ii) for constant distortion curves and iii) an approximate formula (up to second order in the ellipticity parameter) for the deformation cross section. We show that the solution of the PA for the SIEP model is exact. For the PNFW we determine a domain of validity on the space of model parameters such that the PA can replace the exact solutions for constant distortion curves and deformation cross section. The solutions and mapping relations presented here, within their determined domain of validity, can be used to speed up numerical codes and applied to arc statistics and other lensing observables. B [email protected] Instituto de Cosmologia, Relatividade e Astrofı́sica — ICRA, Centro Brasileiro de Pesquisas Fı́sicas, Rua Dr. Xavier Sigaud 150, CEP 22290-180, Rio de Janeiro, RJ, Brazil 1 159 Cosmology Short Talks COS -2 The CFHT/MegaCam Stripe-82 Survey B1 Moraes, B. 2 ; Kneib, J.-P. ; Leauthaud, A.3 ; Makler, M.1 ; Van Waerbeke, L.4 ; Bundy, K.3 ; Erben, T.5 ; Heymans, C.6 ; Hildebrandt, H.4,5 ; Miller, L.7 ; Shan, HY.8,9 ; Woods, D.4 ; Charbonnier, A.1 ; Pereira, M. E.1 The CFTH/MegaCam Stripe-82 Survey (CS82) is a joint Canada-France-Brazil project covering ⇠ 170 sq. deg. in the SDSS Stripe-82 area down to magnitude 24.1 in the optical i-band with a mean 0.6” seeing (PIs: J.-P. Kneib, A. Leauthaud, M. Makler, L. Van Waerbeke). Its main focus is the study of weak and strong gravitational lensing, with additional applications in other fields such as galaxy evolution and galaxy cluster science. Furthermore, the multitude of existing and future projects in Stripe-82, covering from the radio to the UV and including a large set of spectroscopic data, offers the possibility of exploring applications in many fields of astronomy, thereby enhancing the scientific value of the survey. In this Short Talk, we will give an overview of the main published and ongoing CS82 scientific projects. They include the measurement of the largest contiguous lensing convergence map to date and its peak statistics, providing direct information on the large scale dark matter distribution; the first CMB-lensing ⇥ shear cross-correlation measurement, probing the dark matter distribution at redshifts of order 1; galaxy-galaxy lensing measurements around SDSS-III/BOSS galaxies, constraining halo occupation distribution (HOD) models and obtaining complementary mass measurements in combination with BOSS spectroscopic data; the discovery of several new gravitational arc systems and more. B 1 2 3 4 5 6 7 8 9 [email protected] ICRA, Centro Brasileiro de Pesquisas Fı́sicas Laboratoire d’Astrophysique de Marseille, Aix Marseille Université Institute for the Physics and Mathematics of the Universe, University of Tokyo Department of Physics and Astronomy, University of British Columbia Argelander Institute for Astronomy, University of Bonn Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Royal Observatory Department of Physics, Oxford University Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne Department of Physics and Tsinghua Center for Astrophysics, Tsinghua University 160 Short Talks Cosmology COS -2 High Mass X-ray Binaries at the Dawn of the Universe I. F. MirabelB1 Based on the observations of accreting stellar black holes in the local universe, I propose that a large fraction of the first generations of massive stars in primordial galaxies ended as black holes and neutron stars in High Mass X-ray Binaries. Besides the ultraviolet radiation from their massive stellar progenitors, feedback from HMXBs was an additional, important source of heating and reionization of the IGM. X-rays and relativistic jets from the large populations of HMXBs, determined the early thermal history of the universe and maintained it ionized over large volumes of space. This has a direct impact on the properties of the faintest galaxies at high redshifts, the smallest dwarf galaxies in the local universe, and on the existing and future surveys at radio wavelengths of atomic hydrogen in the early universe. B 1 [email protected] IAFE-CONICET-Argentina 161 Cosmology Short Talks COS -3 Multi-fractal and lacunarity spectrum analysis of the galaxy distribution in the SDSS 9th data release Chacón-Cardona, C. A.1,2 ; Casas-Miranda, R. A.B2 The cosmological principle states that the cosmos is homogeneous and isotropic, such that the observed inhomogeneities are only perceived locally and should vanish on sufficiently large scales. In modern cosmology the cosmological principle is one of the fundamental hypotheses from which the observations and theoretical developments are contrasted and interpreted. Thus, it is important to investigate if the cosmological principle is supported by the observations of galaxies in the most recent catalogues and, in the affirmative case, what is the distance scale at which the transition to homogeneity is observed. Some researchers report that astrophysical objects are grouped in highly structured hierarchical patterns that exhibit properties of self-similarity and a fractal dimension smaller than the physical space dimension (i.e., no transition to homogeneity), while other authors claim to have found the scale of transition to homogeneity. We develop a statistical analysis of the large-scale clustering of matter in the universe from the fractal point of view using galaxies from the Ninth Sloan Digital Sky Survey (SDSS) Data Release (DR9). From the total set of galaxies, a galaxy sample with redshifts in the range 0 < z < 0.25 is created. The sample covers the largest completely connected area of the celestial sphere within the catalogue, with limits in right ascension of 120 < ↵ < 240 and declination 0 < < 60 , which is a region that includes the largest galactic samples that have been studied from the fractal viewpoint to date. From this initial sample which contains 296,465 galaxies we create four volume-limited samples in order to avoid radial incompleteness that would create a spurious detection of clustering up to the largest scales analyzed. We use the sliding-window technique to determine the multi-fractal dimension, the lacunarity spectrum and its dependence on radial distance from the centers for the four volume limited samples used. Using these statistical tools, we find that the clustering of galaxies shows a fractal behavior, that is function of the radial distance, for all calculated quantities. A transition to homogeneity is not observed in the complete multi-fractal dimension set; instead, the galaxies exhibit a persistent multi-fractal behavior with a dimensional spectrum that does not reach the physical space dimension for all values of the structure parameter analyzed, at least for radial distances up to 140 Mpc/h from each available center within the four volumelimited samples. Our results are discussed in the context of the formation of large-scale structure in the Universe. B 1 2 [email protected] Facultad Tecnológica, Universidad Distrital ”Francisco José de Caldas” Universidad Nacional de Colombia 162 Short Talks Cosmology COS -3 Contrast density and mass function for spherical collapse of Lemaitre-Tolman-Bondi metric since fractal point of view. Chacón-Cardona, C. A.B1,2 ; Casas-Miranda, R. A.1 In the nearby universe large inhomogeneities are observed, the galaxies are grouped in comparatively small sections of the space while larges voids are frequently found between the galaxy clusters. According to the standard cosmological principle this behavior must give pass to a statistical homogeneity on a scale that some research groups have located around 100 Mpc/h. On the other hand, recent works on the clustering of astrophysical objects put into question the homogeneity transition universally accepted. Whether or not there is a definite transition to homogeneity, local inhomogeneities should lead us to consider whether physical models based on the cosmological principle are really consistent with observations. Since the dawn of general relativity several researchers have been working on non-homogeneous models of the universe, showing us alternative cosmological research ways both in data interpretation as in theoretical developments. In this presentation we show a theoretical development for the mass density contrast required for the spherical collapse of a dark matter over-density perturbation that evolves in a non-homogeneous universe. In our development we use the fractal cosmology with the Lemaitre-Tolman-Bondi (LTB) metric developed by Ribeiro in the 1990’s. First we demonstrate the correspondence between the respective quantities in the standard cosmology in a homogeneous Friedmann-Robertson-Walker universe and our development based on the fractal metric when the dimension of the mass enclosed in a sphere of co-moving radius r obtained from the fractal metric takes the same value of the physical space dimension D = 3, i.e., homogeneity condition. We find an expression for the halo mass function within the Press-Schechter formalism using the theory of brownian random paths, also known as excursion set theory. Finally, we compare our results with the galaxy clustering information from the Millennium Simulation and from the Sloan Digital Sky Server (SDSS) galaxy catalogue in its ninth data release. Our theoretical model and its predictions are discussed in the context of the large-scale structure formation in the Universe from the viewpoint of the conditional cosmological principle proposed by Mandelbrot. B 1 2 [email protected] Universidad Nacional de Colombia, Departamento de Fı́sica Universidad Distrital Francisco José de Caldas, Facultad Tecnológica 163 Cosmology Short Talks COS -3 Gaussian analyses on PLANCK CMB maps Bernui, ArmandoB1 Extremely precise cosmic background radiation (CMB) data from Planck satellite confirmed the cosmological model ⇤CDM and established tight constraints for several features of the primary and secondary CMB temperature fluctuations. Possible non-Gaussian (NG) contributions to the CMB field could be originated during (or soon after) primordial cosmic inflation, where the types, scale dependences, and intensities expected depend on the inflationary models. For this, the robust detection –or not– of primordial NG in the CMB signify a unique probe to the early universe, allowing to distinguish between competing models. Recent analyses from Planck CMB data strongly limit the level of NG and show consistency with the Gaussian hypothesis although they do not exclude the presence of weak Gaussian deviations. A problem inherent with the confidence of a positive detection is the possibility that any non-primordial contamination could be mixed with primary contributions leading to qualitative and/or quantitative imprecise detections. A variety of methods are being used to search for different NG signals in CMB data because one does not expect that a single statistical tool can be able to identify all possible forms of Gaussian deviations. Using two directional large-angle NG indicators based on skewness and kurtosis statistical momenta of patches of the CMB sphere, we analyze the three nearly full sky foreground-cleaned Planck maps: SMICA, NILC, and SEVEM. Our results show that these foreground-cleaned Planck maps exhibit different levels of NG at large angles, depending on the cut-sky mask used (all of them released by the Planck collaboration). The separation component minimum mask, termed M82, and the U73 mask appear to be equally efficient to Gaussianize all these CMB Planck maps. B 1 [email protected] Observatório Nacional, MCTI 164 High Energy Astrophysics HEAP-1 Acceleration of Cosmic Rays in the FERMI and CTA Era de Gouveia Dal Pino, E. M.B1 ; Kowal, G.2 ; Lazarian, A.3 The gamma ray emission detected from cosmic sources is currently challenging the researchers. Its origin is in most cases associated to cosmic ray production. Very fast particles may be accelerated by a variety of processes. In particular, acceleration by magnetic reconnection has lately attracted the attention of researchers not only for its potential importance in the solar system context, but also beyond it, in astrophysical environments like galactic black holes, pulsars, AGNs and GRBs, and even in the diffusive ISM and IGM, especially in magnetically dominated regions. In this talk, we review this process and present three-dimensional MHD simulations of astrophysical sites with the injection of thousands of test particles and show from the evolution of their energy spectrum that they are efficiently accelerated by reconnection through a first-order Fermi process within large scale magnetic current sheets (especially when local turbulence is present making reconnection fast and the acceleration region thick). The resulting acceleration will be also confronted with shock acceleration in distinct cosmic ray accelerators. B 1 2 3 [email protected] Instituto de Astronomia, Geofisica e Ciencias Atmosfericas, Universidade de Sao Paulo EACH, Universidade de Sao Paulo Astronomy Department, University of Wisconsin at Madision 165 High Energy Astrophysics Short Talks HEAP-1 The Gravitational Drag Force on an Extended Object Moving in a Gas Bernal, C. G.B1 ; Sánchez-Salcedo, F. J.1 A gravitational perturber moving through a gaseous background creates a density wake in the medium. At large enough impact parameters, the perturber induce a small perturbation in the far-field ambient medium and the density structure of the wake can be derived in linear perturbation theory. Using this approach, Ostriker (1999) derived the density wake behind a gravitational body of mass M moving at velocity V0 on a straight-line trajectory through a homogenous medium with unperturbed density rho0 and sound speed c0 , when the perturber is dropped at t = 0. For subsonic perturbers, the isodensity contours are closed ellipsoids, which do no contribute to the drag force, except in the outer parts of the wake where the ellipsoids are not closed. Supersonic perturbers generate a density wake only within the rear Mach cone. The gravitational interaction with its own induced wake produces a drag force on the perturber. In this work, we revisit the drag force on a non-accreting body. Our aim is to provide a physically more motivated and more insightful formula for the drag force in the linear and nonlinear cases. Our analytical equation will be compared with numerical simulations. B 1 [email protected] Instituto de Astronomı́a - UNAM 166 Short Talks High Energy Astrophysics HEAP-1 Time lags of the kilohertz quasi-periodic oscillations in the low-mass X-ray binaries 4U 1608-52 and 4U 1636-53 Marcio G B de AvellarB1 ; Mariano Méndez2 ; Andrea Sanna3 ; Jorge Horvath1 We studied the energy and frequency dependence of the Fourier time lags and intrinsic coherence of the kilohertz quasi-periodic oscillations (kHz QPOs) in the neutron-star low-mass X-ray binaries 4U 1608-52 and 4U 1636-53, using a large data set obtained with the Rossi X-ray Timing Explorer. We confirmed that, in both sources, the time lags of the lower kHz QPO are soft and their magnitude increases with energy. We also found that: (i) In 4U 1636-53, the soft lags of the lower kHz QPO remain constant at ⇠ 30 µs in the QPO frequency range 500-850 Hz, and decrease to ⇠ 10 mus when the QPO frequency increases further. In 4U 1608-52, the soft lags of the lower kHz QPO remain constant at 40 µs up to 800 Hz, the highest frequency reached by this QPO in our data. (ii) In both sources, the time lags of the upper kHz QPO are hard, independent of energy or frequency and inconsistent with the soft lags of the lower kHz QPO. (iii) In both sources the intrinsic coherence of the lower kHz QPO remains constant at ⇠0.6 between 5 and 12 keV, and drops to zero above that energy. The intrinsic coherence of the upper kHz QPO is consistent with being zero across the full energy range. (iv) In 4U 1636-53, the intrinsic coherence of the lower kHz QPO increases from ⇠0 at ⇠600 Hz to ⇠1, and it decreases to ⇠0.5 at 920 Hz; in 4U 1608-52, the intrinsic coherence is consistent with the same trend. (v) In both sources the intrinsic coherence of the upper kHz QPO is consistent with zero over the full frequency range of the QPO, except in 4U 1636-53 between 700 and 900 Hz where the intrinsic coherence marginally increases. We discuss our results in the context of scenarios in which the soft lags are either due to reflection off the accretion disc or up-/down-scattering in a hot medium close to the neutron star. We finally explore the connection between, on one hand the time lags and the intrinsic coherence of the kHz QPOs, and on the other the QPOs’ amplitude and quality factor in these two sources. B 1 2 [email protected] Departamento de Astronomia, Geofı́sica e Ciências Atmosféricas da Universidade de São Paulo Kapteyn Astronomical Institute - University of Groningen 167 High Energy Astrophysics Short Talks HEAP-1 Unveiling the nature of an ultra-luminous X-ray source through the kinematics and structure of its optical counterpart Fuentes-Carrera, I.B1 ; Rosado, M.2 ; Arias, L.3 ; Moreno-Mendez, E.2 ; Borissova, J.4 ; Flores, H.5 ; Goncalves, D.6 ; Salinas, A.1 With luminosities between 1039 - 1041 erg/s in the 0.5-10 keV band, ultra-luminous X-ray sources (ULXs) lie between classic X-ray binaries and active galactic nuclei, and their nature is still far from clear. Current models include accreting stellar black holes (BHs) with strongly beamed emission, super-Eddington accretion in stellar-mass BHs, extremely energetic supernovae, hypernovae, or intermediate-mass black holes (IMBH). We present observations of the extended optical counterpart of the bright ULX in the S+S interacting galaxy pair NGC 5953/54 using the FLAMES-GIRAFFE integral field spectrograph in its ARGUS mode in order to derive detailed spectroscopical and spatial information of the surroundings of this apparently elongated ULX. The kinematics of the extended counterpart of this ULX and nature of the ionization of the gas is analysed in the light of the different scenarios. Along with IFU observations we present long-slit observations taken with the OSIRIS spectrograph on the Gran Telescopio de Canarias (GTC), near the location of the ULX and along the star-forming region that seems to be enhanced by the interaction between the two galaxies in search of peculiarities that could be associated with the origin of this energetic source. B 1 2 3 4 5 6 [email protected] Escuela Superior de Fisica y Matematicas, Instituto Politecnico Nacional, Mexico Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Mexico Universidad Iberoamericana, Mexico Universidad de Valparaiso, Chile Observatoire de Paris-Meudon, France Observatorio do Valongo, Brazil 168 Short Talks High Energy Astrophysics HEAP-2 Mass and energy of GRB-SN events: multi-wavelength analysis of three associations in the context of the full sample Olivares E., F.B1,2 ; Greiner, J.1 ; Schady, P.1 ; Klose, S.3 ; Krühler, T.4 ; Rau, A.1 ; Savaglio, S.1 ; Kann, D. A.3 ; Pignata, G.2 ; Elliott, J.1 ; Rossi, A.3 ; Nardini, M.5 ; Afonso, P. M. J.6 ; Filgas, R.7 ; Nicuesa Guelbenzu, A.3 ; Schmidl, S.3 ; Sudilovsky, V.1 After the discovery of SN 1998bw associated with GRB 980425, the first connection between Gamma-Ray Bursts (GRBs) and Supernovae (SNe) occured almost 15 years ago, no more than two dozens SN-like rebrightenings and seven solid spectroscopically-confirmed associations have been observed to date. In this talk we present data from the Gamma-Ray Burst Optical and Near-infrared Detector (GROND) and from the Swift X-Ray Telescope (XRT) and Ultra-Violet/Optical Telescope (UVOT) for three GRB afterglows showing SN rebrightenings. We studied the luminosity and evolution of each GRB-SN event and derived accurate values of the host-galaxy extinction through the modelling of the broad-band afterglow spectral energy distribution. After correcting for all sources of foreground extinction, SNe 2009nz (associated with GRB 091127), 2010ma (GRB 101219B), and 2008hw (GRB 081007), exhibited 1.15 ± 0.09, 1.78+0.08 0.17 , and 0.80 ± 0.10 times the luminosity of SN 1998bw, respectively. After subtracting the afterglow component, we constructed quasi-bolometric light curves and modelled them using Arnett’s analytical approach to obtain the physical parameters of the SN explosion, such as synthesised 56 Ni mass (MNi ), ejecta mass (Mej ), and kinetic energy (Ek ). From the full sample of 29 GRB-SNe, the largest ever presented, we utilised the SN and GRB parameters to assess the nature of the connection statistically. The average brightness for 27 GRB-SNe corresponds to an absolute magnitude of MV = 19.46(±0.12 RMS), where only 7% of all GRB-SNe are significantly brighter than SN 1998bw. Two populations are identified in the MNi -Mej plane. We attribute this bimodality to two mass-loss scenarios distinguished mainly by how much mass was lost at late evolutionary stages. Moreover, marginal anti-correlations are found between GRB isotropic energy release E ,iso and Ek from the SN, however, we show that the GRB and SN energetics are decoupled overall. The data suggest a preference for SN events to be on average associated with soft low-luminosity, however, this can be explained by selection effects solely. B 1 2 3 4 5 6 7 [email protected] Max-Planck-Institut fur extraterrestrische Physik, Giessenbachstraße 1, 85740 Garching, Germany Departamento de Ciencias Fisicas, Universidad Andres Bello, Avda. Republica 252, Santiago, Chile Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark Università degli studi di Milano-Bicocca, Piazza della Scienza 3, 20126, Milano, Italy American River College, Physics and Astronomy Dpt., 4700 College Oak Drive, Sacramento, CA 95841, USA Institute of Experimental and Applied Physics, Czech Technical University in Prague, Horska 3a/22, 12800 Prague 2, Czech Republic 169 High Energy Astrophysics Short Talks HEAP-2 Runaway massive stars as a new class of galactic gamma-ray sources del Valle, M. V.B1 ; Romero, G. E.1 Runaway stars have high spatial velocities, V > 30 km s 1 , and if the are massive, can produce bowshocks in the surrounding ISM. These bowshocks develop as arc-shaped structures pointing in the same direction as the supersonic stellar velocity. The piled-up shocked matter emits thermal radiation. Additionally, a population of locally accelerated relativistic particles can produce non-thermal emission over a wide range of energies. This has been recently confirmed by a bunch of observations at radio, X-ray and even gamma-ray wavelengths. Runaway early-type stars might be variable gamma-ray sources, with variability time scales depending on the scales of density inhomogeneities in the medium and the stellar velocity. Protons can easily escape from the emitting region without much loss on energy. These protons might diffuse in the surrounding molecular cloud interacting with the matter via p-p inelastic collisions. These yield gamma rays and secondary particles. Molecular clouds illuminated by these relativistic particles might become into diffuse non-thermal sources. We calculate all relevant non-thermal processes related to these stellar objects and discuss the observational prospects. B 1 [email protected] Instituto Argentino de Radioastronomia (IAR) 170 Short Talks High Energy Astrophysics HEAP-2 Spectral analysis of type II Supernovae B1 Claudia P. Gutiérrez ; Joseph P. Anderson1 ; Mario Hamuy1 ; Santiago Gonzalez-Gaitán1 ; Gastón Folatelli2 ; CSP team3 We present a spectroscopic analysis of the H↵ profiles of hydrogen-rich type II supernovae. A total of 56 type II supernovae were analyzed concentrating on the H↵ P-Cygni profiles. Expansion velocities and the ratio of absorption to emission (a/e) at the epoch of transition between initial and plateau decline phases in the light curve are defined to describe the diversity in this line. These spectral properties are correlated with photometric properties: absolute magnitudes, decline rates and the optically thick duration phase. Testing the strength of various correlations we find that a/e appears to be the dominant parameter in terms of describing the diversity in our measured supernovae properties. It is found that supernovae with smaller a/e have higher H↵ velocities, more rapidly declining light-curves from maximum, during the ‘plateau’ and radioactive tail phase, are brighter at maximum light and have smaller optically thick duration values. We discuss possible explanations of these results in terms of physical properties of type II supernovae, speculating that the most likely parameters which influence the morphologies of H↵ profiles are the mass and density profile the hydrogen envelope, together with extra emission components due to circumstellar interaction. B 1 2 3 [email protected] Departamento de Astronomia, Universidad de Chile Institute for the Physics and Mathematics of the Universe (IPMU) University of Tokyo Carnegie/Las Campanas Observatories 171 High Energy Astrophysics Short Talks HEAP-2 Astronomy and Astrophysics in the Colombian Andes: the PAS Project Asorey, H.B1,2 ; Núñez, L. A.1 The PAS (Polo de Astronomı́a Social) project aims to establish a permanent link, a bridge, between science and society. This project is focused on building an astrophysical touristic center at the north eastern region of the Colombian Andes. Two 12-meter hemispheric domes will allocate the scientific and outreach installations. In one of them, the ”Science dome”, a 20r̈obotic telescope will be installed, and would be controlled remotely. In this first dome, offices, laboratories and data acquisition, simulation and distribution mainframes will be operated. All the collected data will be available trough a collaborative framework that allow to register, to catalog, to analyze and to share the obtained results. In the second dome, the ”Society dome”, a planetary system and a convention center will be builded, with emphasis in the complex scientific data visualization capabilities of this system. Both domes will be linked by a tunnel, the ”Science Tunnel”, which will be a conceptual representation of this wanted bridge between science and society. In this tunnel, a complex visualization wall will allow the visitors to share different interactive experiences. Outreach activities, such as the ”Stars Camping Weekend”, are being planned. Due to its geographic characteristics, the Andinian Páramo located near Berlı́n, Colombia, at 3500 m a.s.l., is an excellent location to build an array of particle detectors to study cosmic rays in a wide energy range, including solar activity modulation of cosmic rays, gamma ray bursts (GRB), and the high energy region of the cosmic rays spectrum. The proposed array will consist in more than one hundred of autonomous and wireless water Cherenkov detectors (WCD) located over different concentric triangular grids with different spacing between neighbor detectors, spanning over a total area of more than 16 km2 . This facility will be operated by an international and interdisciplinary group of researchers. The design of the detector array is based on Corsika air showers and Geant4-based detector response simulations. The proposed design of this array will allow to implement two different measurement modes: the counting mode and the shower mode. In the counting mode, the variations in the recorded flux of secondary particles at detector level can be correlated with transient phenomena, such as the solar modulation of galactic cosmic rays or the arrival of the highest energy component of an energetic GRB; or long term flux modulations related, e.g., with the solar activity cycle. In the shower mode, in contrast, we will look for time-space correlated signals in different, non-aligned, detectors of the array. In this way, it will be possible to determine the main parameters that characterize the extensive air shower (EAS) produced by the interaction of a single high-energy cosmic ray with the atmosphere. From this parameters, the arrival direction and the energy of the impinging cosmic ray will be obtained. The size of the array and the increasing spacing between detectors will allow to complement present measurements in the so called knee region of the cosmic ray energy spectrum (E ⇠ 1015 eV) and beyond. In this work, we show the present status of the design of this facility, its academic and social goals and its scientific capabilities are presented. B 1 2 [email protected] Escuela de Fı́sica, Universidad Industrial de Santander, Bucaramanga, Colombia Centro Atómico Bariloche and Instituto Balseiro (CNEA, UNCuyo, CONICET), San Carlos de Bariloche, Argentina 172 Instrumentation INST-1 LLAMA Project B1 E. M. Arnal 2 ; Z. Abraham ; G. Giménez de Castro3 ; E. M. de Gouveia dal Pino2 ; J. J. Larrarte4 ; J. Lepine2 ; R. Morras1 ; J. Viramonte5 LLAMA, acronymum of Long Latin American Millimetre Array, is a joint scientific and technological undertaking of Argentina and Brazil whose main goal is to install and to operate a 12m dish capable of studying the Universe at millimetre and sub-millimetre wavelengths. This facility will be erected in the norwestern part of Argentina, some 20 km away from the town of San Antonio de los Cobres (Salta province), at a site located 4830m above sea level. In this presentation we would like to formally introduce this project to the Latin American astronomical community by briefly describing its current status. Besides working as a stand alone instrument (or single dish mode), this radiometer may also become part of a local network of Very Long Baseline Interferometry (VLBI) that may be integrated by existing telescopes like APEX, ASTE, Itapetinga and some of the ALMA dishes. In its way, this VLBI network may be able to increase the resolving power of ALMA by an order of magnitude. The construction phase of this facility is being financed by Ministerio de Ciencia, Tecnologı́a e Innovación Productiva (MINCyT, Argentina) and Fundação de Amparo á Pesquisa do Estado de São Paulo (FAPESP), on the basis of an equal investment share. B [email protected] Instituto Argentino de Radioastronomia (IAR), CCT-La Plata, CONICET and Facultad de Ciencias Astronómicas y Geofı́sicas, Universidad Nacional de La Plata, Argentina 2 Instituto de Astronomia e Geofisica, Universidad de San Pablo, Brazil 3 CRAAM, Universidad Presbiteriana Mackenzie, San Pablo, Brazil 4 Instituto Argentino de oéomia, Radioast (IAR), CCT-La Plata, CONICET 5 Instituto Geonorte, CONICET-UNSa, Argentina 1 173 Instrumentation Short Talks INST-1 SOUTH POL: Revealing the Polarized Southern Sky Magalhães, A. M.B1 SOUTH POL will be a survey of the Southern sky in optical polarized light. It will use a newly designed polarimeter for an 80cm Robotic Telescope. Telescope and polarimeter will be installed at CTIO, Chile. The initial goal is to cover the sky south of declination 15 in about two years of observing time, aiming at a polarimetric accuracy  0.1% down to V=15, with a camera covering a field of about 2.0 square degrees. SOUTH POL will impact areas such as Cosmology, Extragalactic Astronomy, Interstellar Medium of the Galaxy and Magellanic Clouds, Star Formation, Stellar Envelopes, Stellar Explosions and Solar System, among others. The polarimeter is currently being built and its optics and electronics assembled. We will describe the current status of the project. This project is supported by FAPESP. AMM is also supported by CNPq. B 1 [email protected] Departamento de Astronomia, IAG, Universidade de São Paulo 174 Short Talks Instrumentation INST-1 The hard X-ray telescopes for MIRAX and protoMIRAX B1 Braga, J. ; D’Amico, F.1 ; Ávila. M. C.1 ; Rodrigues, B. H.1,2 ; Grindlay, J. E.2 ; Allen, B.2 ; Hong, J.2 ; Barthelmy, S.3 ; Rothschild, R. E.4 The Monitor e Imageador de Raios X (MIRAX), under development at the National Institute for Space Research (INPE), Brazil, is a hard X-ray astronomy experiment that will be launched in low-Earth orbit (650 km altitude, 15 inclination) onboard the Lattes satellite mission in 2018. MIRAX consists essentially in two coded-aperture imaging telescopes equipped with cadmium-zinc-telluride (CZT) solid-state room-temperature semiconductor detectors. One telescope (T1) has been in development at INPE0 s Astrophysics Division and will fly in a high altitude (⇠43 km) balloon in 2014 for testing and demonstration; this development is called the protoMIRAX project. T1 uses an array of 13⇥13 CZT planar detectors with dimensions 10mm⇥10mm⇥2mm and a 1 mm-thick lead coded mask with 20 mm openings in a 13⇥13 Modified Uniformly Redundant Array (MURA) basic pattern. It will have a 20 ⇥ 20 fully-coded field-of-view (FCFOV) and an angular resolution of 1.5 . T1 will be mounted in a balloon gondola with an attitude control and pointing systems as well as a 500 kbps telemetry and command capability for real-time operation and data acquisition. The imaging CZT detectors for the second telescope (T2) are being developed at the Harvard Smithsonian Center for Astrophysics (CfA). The detector plane for T2 will have a 0.6 mm spatial resolution and an area of 250 cm2 . A 0.3mm-thick tungsten mask with a random pattern will provide images with 60 angular resolution with a 20 ⇥ 20 FWHM FOV. In this presentation we will describe the current status of MIRAX and present results of the protoMIRAX detector, telescope and balloon gondola developments. B 1 2 3 4 [email protected] Astrophysics Department, National Institute for Space Research, Brazil Harvard Smithsonian Center for Astrophysics NASA Goddard Space Flight Center Center for Astrophysics and Space Science, University of California San Diego 175 Instrumentation Short Talks INST-1 Cherenkov Telescope Array (CTA) Barres de Almeida, U.B1 ; De Gouveia Dal Pino, E.2 Gamma-ray astronomy holds a great potential for Astrophysics, Particle Physics and Cosmology. The CTA is an international initiative to build the next generation of ground-based gamma-ray observatories, which will represent a factor of 5-10x improvement in the sensitivity of observations in the range 100 GeV - 10 TeV, as well as an extension of the observational capabilities down to energies below 100 GeV and beyond 100 TeV. The observatory consists of two telescope networks (one in the Northern Hemisphere and another in the South, the latter with about 60 telescopes) so to achieve a full-sky coverage. It will grant open access to the community, through call for submission of proposals competing for observation time. The CTA will give us access to the non-thermal and high-energy universe, to a level never reached so far, and will be one of the main instruments for high-energy astrophysics and astroparticle physics of the next 30 years. Brazil is a member of the CTA consortium, and the project is represented in Latin America by Argentina and Mexico as well. In this talk we will present the basic concepts of the CTA and the project of the observatory which is now under development. Emphasis will be put on its scientific potential and on the Latin-American involvement in the preparation and construction of the experiment. The CTA is expected to be fully operational by 2018, and by the end of this year the site of installation of CTA should be defined. Among the most promising sites for the southern array there are three South American candidates, two in Argentina and one in Chile. B 1 2 [email protected] Centro Brasileiro de Pesquisas Fı́sicas (CBPF/MCTI) Instituto Astronômico, Geofı́sico e de Ciências Atmosféricas, Universidade de São Paulo (IAG/USP) 176 Short Talks Instrumentation INST-2 Observational Results using BTFi Quint, B.B1 ; Mendes de Oliveira, C.1 ; BTFI Team We present here an overview of a new tunable filter instrument for the SOAR telescope. The Brazilian Tunable Filter Imager (BTFI) is a highly versatile new technology to be used both in seeing-limited mode and at higher spatial fidelity using SAM Ground-Layer Adaptive Optics facility (SOAR Adaptive Module) which is being deployed at the SOAR telescope. It presents important new science capabilities for the SOAR astronomical community, from studies of the centers of nearby galaxies and the insterstellar medium to statistical cosmological investigations. BTFI will deliver XY data-cubes that can be seen as set of images at different wavelengths or a set of spectra for each XY pixel. For that, it relies on three new technologies. The imaging Bragg Tunable Filter (iBTF) concept utilizes Volume Phase Holographic Gratings in a double-pass configuration as a tunable filter, while a new Fabry-Perot (FP) concept involves the use of commercially available technologies which allow a single FP etalon to act over a very large range of interference orders and hence spectral resolutions. Both of these filter technologies will be used in the same instrument. The combination allows for highly versatile capabilities. Spectral resolutions spanning the range between 25 and 2000 can be achieved in the same instrument through the use of iBTF at low resolution and scanning FPs beyond R ⇡ 2000 with some overlap in the mid-range. The third component of the new technologies deployed in BTFI is the use of EMCCDs, which allow for rapid and cyclical wavelength scanning thus mitigating the damaging effect of atmospheric variability through the acquisition of the data cube. The system was designed to supply tunable filter imaging with a field-of-view of 3’ on a side, sampled at 0.12” for direct Nasmyth seeinglimited area spectroscopy and for SAM’s visitor instrument port for GLAO-fed area spectroscopy. The final data-cube is obtained throught scanning in wavelength while acquiring images, stacking these images together and processing this stack thoght software so the cube has XY information. The instrument has been already tested on sky and we are presenting observational data of the planetary nebulae NGC 7009 in high resolution mode and NGC 2440 in low resolution. For high resolution, we used a QueensGate Fabry-Perot installed inside BTFi with R = 4500 while, for low resolution, the iBTF was used with R = 1200 gratings, both near H-alpha. B 1 [email protected] IAG/USP 177 Instrumentation Short Talks INST-2 BOMBOLO: a Multi-Band, Wide-field, Near UV/Optical Imager for the SOAR 4m Telescope Angeloni, R.B1,2,3 ; Guzman, D.2 ; Puzia, T. H.1 ; Infante, L.2 ; Kanaan, A4 ; Oliveira, C.5 ; et al. In this contribution I will present BOMBOLO, a new astronomical multi-passband instrument proposed for the SOAR 4m Telescope. As the first Chilean instrument of its kind, it is a three-arms imager covering the near-UV and optical wavelengths. The three arms work simultaneously and independently, providing synchronized imaging capability for rapid astronomical events. BOMBOLO will be able to address largely unexplored events in the minute-to-second timescales, with the following leading science cases: 1) Simultaneous Multiband Flickering Studies of Accretion Phenomena; 2) Near UV/Optical Diagnostics of Stellar Evolutionary Phases; 3) Exoplanetary Transits; 4) Microlensing Follow-Up; 5) Solar System Studies. BOMBOLO has been approved by the SOAR Board of Directors as a visitor instrument. B 1 2 3 4 5 [email protected] Instituto de Astrofı́sica, Pontificia Universidad Católica de Chile - Santiago, Chile Centro de Astro-Ingenierı́a, Pontificia Universidad Católica de Chile - Santiago, Chile The Milky Way Millennium Nucleus, Santiago, Chile Physics and Astronomy Dept., University of Santa Catarina, Brazil Astronomy, Geophysics & Atmospheric Sciences, University of Sao Paulo, Brazil 178 Short Talks Instrumentation INST-2 New algorithm for centroiding in elongated Shack-Hartmann wavefront sensors spots using artificial neural networks Mello, A. T.B1 ; Kanaan, A.1 ; Guzman, D.2 ; De Cos, F. J.3 To recover the resolution lost in a ground-based telescope due to the atmosphere, it is necessary to use a technique known as Adaptive Optics (AO). The next generation of telescopes will have primary mirrors of more than 25 meter in diameter and will require AO systems from the ground up. There are a number of challenges to implement an AO system at these scales. One of these challenges is the accurate measurement of the aberrated wavefronts using a laser guide star and a Shack-Hartmann wavefront sensor. Due to the diameter of the telescope and the use of the Sodium layer in the upper atmosphere as photon return for the laser guide stars, the image of the guide star will appear elongated in the wavefront sensor. Typical centroiding algorithms such as Center of Gravity do not perform well under these conditions. This article presents a new technique based on artificial neural networks for measuring the spot position with better accuracy than existing methods. Simulation results will confirm that the new algorithm incurs in smaller errors with respect to other centroiding techniques in use. B 1 2 3 [email protected] Universidade Federal de Santa Catarina, Brazil Pontificia Universidad Catolica de Chile Universidad de Oviedo, España 179 Instrumentation Short Talks INST-2 GeMS/GSAOI: from commissioning to operations and science results E. R. CarrascoB1 ; B. Neichel1 ; F. Rigaut2 ; C. Winge1 ; F. Vidal1 ; P. Pessev1 ; A. Serio1 ; G. Arriagada1 ; W. Rambold1 ; J. Luhrs1 ; M. Boccas2 ; C. Dorgeville2 ; V. Fesquet1 ; A. Lopez1 ; C. Trujillo3 ; R. Galvez1 ; G. Gausachs1 ; C. Araujo1 ; T. Vucina1 ; V. Montes1 ; C. Urrutia1 ; C. Moreno1 ; C. Marchant1 ; F. Collao1 ; S. Diggs1 ; F. Collao1 ; G. Trancho4 ; M. Bec4 The Gemini Multi-conjugate Adaptive Optics System (GeMS) and the Gemini South Adaptive Optics Imager (GSAOI) are unique and complex facility Gemini instruments. GeMS/GSAOI provide a uniform, diffraction limited image quality at near-infrared (NIR) wavelengths over a field of view of 85” x 85” on the sky. The GeMS/GSAOI commissioning started at the beginning of 2011. After ⇠2 years of dedicated work and more than 90 nights of on-sky commissioning, at the end of 2012 GeMS/GSAOI started to produce the first science results. In this presentation we describe in details the system performance, on-sky efficiency and present the scientific results produced by GeMS/GSAOI during the system verification process. B 1 2 3 4 [email protected] Gemini Observatory/AURA, Southern Operations Center Research School of Astronomy and Astrophysics, The Australian National University Gemini Observatory/AURA, Northern Operations Center Giant Magellan Telescope Organization 180 Short Talks Instrumentation PS -3 Solar astrometry and the heliometer of Rio de Janeiro Sigismondi C.B1,4 ; Boscardin S. C.1 ; Andrei A. H.1,2,3 ; Reis Neto E.5 ; Penna J. L.1 ; D’Avila V. A.1,6 Three quantities characterize the state of a self gravitating gaseous body: pressure, temperature and volume, but the radius is the only one directly measurable for the Sun, what is specially true in the optical window and for ground-based measurements. The Heliometer of the Observatório Nacional, in Rio de Janeiro, measures the distance between two opposite limbs of the Sun in the same field of view, through the reflection on a 10 cm parabolic mirror split on its half and forming an appropriate angle. This configuration is free from optical aberrations and focal variations along the measurement direction. The mirrors are made on CCZ vitro-ceramic and the telescope structure is of carbon fiber, resulting that there is no flexion or temperature deformation. The instrument is compact, and it can perform hundreds of measurements per duty day, around all heliolatitudes. Vertical and horizontal differential refractions to the solar image and their dependance on air pressure, temperature and water vapour content are taken into account for data reductions: they are minimum when the center of the Sun approaches the zenith as this is verified for more than a month in Rio de Janeiro. The heliometer attains an accuracy on the solar radius of 0.01 arcsec, becoming the ideal instrument to monitor the solar diameter from the ground, and to bridge satellites and astrolabes historical series of data. We discuss the first years of regular observation, with emphasis on the instrumental calibrations and on the statistic study of the derived time series and solar geometry series. On basis of these analysis we obtain how well the Heliometer and Solar Astrolabe results are matched, extending a continuous solar semi diameter series over forty years. B 1 2 3 4 5 6 [email protected] Observatório Nacional/MCTI Observatório do Valongo/UFRJ SYRTE/Observatoire de Paris ICRANet/Sapienza Universitá di Roma and Ateneo Pontificio Regina Apostolorum MAST/Museu de Astronomia e Ciências Afins/MCTI UERJ/Universidade do Estado do Rio de Janeiro 181 182 Teaching & Outreach TO -1 Assessing and evaluating: a case study in the framework of EU-UNAWE Italy project Lara AlbaneseB1 ; James Bradburne2 ; Alessandra Zanazzi1 A special case study evaluation will be presented, relative to a whole year work in the framework of EU UNAWE Italy, with teachers in training sessions and in the classrooms, children, and parents also. When it comes to activities with children or very young children, evaluation and assessment needs to be comprehensive and take into account different aspects such as parents involvement, spontaneous interest and spontaneous play, curiosity and awareness. In such a context, it assumes a huge importance to acquire a varied and exhaustive documentation, that could possibly give the chance of reflecting, registering and also quantifying the goals that have been reached and the achievements, also in following steps and after the activities ended. The goals are not only those regarding a cognitive level, but involve all the possible “languages” of the child; in particular they are connected to the child imagery. B 1 2 [email protected] INAF - OSSERVATORIO ASTROFISICO DI ARCETRI FONDAZIONE PALAZZO STROZZI, FLORENCE 183 Teaching & Outreach Short Talks TO -1 Life in the Cosmic Context. An Astrobiology Course as an Experiment in Transdisciplinarity Amancio Cesar Santos FriaçaB1 ; Eduardo Janot Pacheco1 Astrobiology is a new interdisciplinary field of research concerned with the study of the origin, distribution, and destiny of life in the universe. It is rapidly gaining the attention of scientists and the public. The appeal of astrobiology is due to the fundamental questions it poses: what is life? are we alone in the universe? what will be the future of life on Earth and elsewhere? In 2003, University of São Paulo (USP) created the course of astrobiology “Life in the Cosmic Context”, addressing these questions taking into account several disciplines – astrophysics, biology, chemistry, geology, meteorology, environmental sciences. The course is provided by IAG (Instituto de Astronomia, Geofı́sicas and Ciências Atmosféricas) to undergraduate students of science and humanities majors. The fact that a large number of majors is represented in the course illustrates the capability of astrobiology in integrating several fields of knowledge. The central underlying questions are explored in class by a wide variety of activities designed to build a transdisciplinary frame. At the same time that the course focuses on issues related to the idea of extraterrestrial life, the reflections and activities of the students leads them to broaden their conceptions about life and to bridge disciplinary barriers. In this work, we present some learning activities done during during the classes and the students feedback. Nearly 1,500 students have attended the “Life in the Cosmic Context” and we chart their impact in teaching and outreach and their role in promoting the scientific literacy. B 1 [email protected] IAG-USP 184 Short Talks Teaching & Outreach TO -1 “Planetário e Teatro Digital Johannes Kepler” and its Institutional Pedagogical Project Faria, R. Z.1 ; Calil, M. R.B1 ; Perez, E. R.1 ; Kanashiro, M.1 ; Silva, L. C. P.1 ; Calipo, F.1 This work relates the reception of schools, started on August 2012, in the astronomic laboratory of the “Planetário e Teatro Digital Johannes Kepler”, located in the “Sabina - Escola Parque do Conhecimento” in Santo André, São Paulo. The idealization of this project, authorship of Marcos Calil, PhD, consists in four apprenticeship environments disposed around the planetary dome. They make reference to the System Sun - Earth - Moon (Tellurium), Solar System, Astronautic and Stars. On Tuesdays and Wednesdays the astronomic laboratory is used by Santo André municipal schools for focused lessons, being possible on Thursdays scheduling for private and public schools. On weekends and holidays is opened for the visitors. Since the inauguration to the beginning of activities with students, the monitor team was guided and trained on contents of Astronomy and Aeronautic to execute the schools service. This is done in four stages, which are: reception, course trough the astronomic laboratory, dome session and activities closure. During the reception the acquaintance rules are passed on for a better visit. Before starting the course the monitors do a survey about the previous knowledge of the students. On the astronomic laboratory resources of the environment are used to explain the contents of Astronomy and Astronautic, always considering the age group and the curriculum developed in classroom. After the course the students watch a planetary session supporting the contents seen on the astronomic laboratory. At the end a feedback is done with the students about the subject discussed. During the visit the teachers fulfill an evaluation about the place and the service. From August 2012 to November 2012 were attended between municipal, public and private schools. From the 4932 students attended, 92% belonged to the municipal network, 5% to the private network and 3% to the public network. From the 189 evaluations done by the teachers, 97.8% were satisfied, 2.1% partially satisfied e 0.1% unsatisfied with the reception promoted by the team of the planetary. Meantime the satisfaction presented on the evaluation is thought that the use of non-formal places is an ally of apprenticeship. The “Planetário e Teatro Digital Johannes Kepler” by its team collaborates for an education and divulgation of the Astronomy and Astronautic make part of the reality and quotidian of the students of the city of Santo André. B 1 [email protected] Theatre Digital and Planetarium Johannes Kepler 185 Teaching & Outreach Short Talks TO -1 Brazilian Participations in the International Astronomical Search Collaboration Rojas, G. A.B1 ; Dalla-Costa, L. J.; Kalmus, A. T.; Kroth, E. C.; Matos, M. F.; Silva, A. L.; Silva, G. G. International Astronomical Search Collaboration (IASC) is an international educational project between universities, schools, observatories and research institutions. Its main objective is to enroll high school and college students in the monitoring and discovery of asteroids and Near Earth Objects (NEOs), especially Potentially Hazardous Asteroids. The methodology consists in the analysis of astronomical images obtained in several observatories in North America and Hawaii. The images are distributed throughout the school network and the results must be delivered in a 72-hour timeframe. Since 2010 Brazilian universities and schools have joined IASC, resulting in over a dozen new asteroids found (3 of them NEOs), and hundreds of measurements for already known asteroids. A major event in this collaboration was the All-Brazil Asteroid Search Campaign, which was conducted in September 2012. 2013 marks the fourth year of Brazilian participations in IASC, with one important milestone: the third straight appearance of a Brazilian institution in the Pan-STARRS campaign, which uses the PS1 telescope in Haleakala, Hawaii. We will present a summary of the overall results, as well as the latest news from 2013 campaigns. We will discuss the impact promoted by the past events, such as how the interest in astronomy changed before and after the campaigns, and it has helped the students to choose their future careers. B 1 [email protected] Universidade Federal de São Carlos, Brazil 186 Short Talks Teaching & Outreach TO -1 Alfabetización en Astronomı́a de docentes de Educación Primaria y de Educación Secundaria en La Plata De Biasi, M. S.B1 ; Orellana, R. B.1 La educación de este siglo tiene como uno de sus retos alcanzar la alfabetización cientfica de todos los ciudadanos para que comprendan y tomen decisiones sobre el mundo natural y sus cambios originados por la actividad humana utilizando el conocimiento cientı́fico. En esta misión los docentes de los niveles obligatorios de enseñanza juegan un papel clave por su rol de agentes multiplicadores del conocimiento. Se requiere, entonces de una adecuada alfabetización en ciencias de los docentes o, como mı́nimo, que dominen los temas cientı́ficos a enseñar. En el campo de la Astronomı́a, numerosas investigaciones han señalado que maestros de primaria y estudiantes de profesorados poseen una escasa formación en estos temas (Camino 1995 y 1999, Gangui 2010), que frecuentemente presentan a los alumnos concepciones alternativas o no cientı́ficas de los fenómenos astronómicos cotidianos (Kriner 2004, Vega Navarro 2007, Gangui et al 2010); a lo que se suma la presentación confusa o errónea de algunos temas astronómicos en los textos escolares (Kriner 2004). Desde 2011, la Facultad de Ciencias Astronómicas y Geofı́sicas, UNLP, ofrece un curso de capacitación destinado a fortalecer y actualizar los contenidos académicos y didácticos de los docentes del distrito La Plata utilizando diversas estrategias didácticas. Los contenidos comprenden los temas astronómicos de los diseños curriculares vigentes. La evaluación diagnóstica de los conocimientos previos de los docentes cursantes sobre los contenidos de mayor presencia en los diseños curriculares mostró resultados similares a las investigaciones arriba mencionadas. Referente a los movimientos de la Tierra, en promedio, el 54% poseı́a conceptos erróneos y el 16% no los sabı́a; con referencia a la Luna el 56% poseı́a conceptos erróneos y un 4% no los sabı́a. Los resultados del curso mostraron que el 95% de los docentes revirtió sus conceptos previos erróneos, que adquirió criterios para la búsqueda de fuentes de información confiables y que el grado de conocimientos disciplinares y didácticos alcanzados por los docentes garantiza el efecto multiplicador de esta propuesta. Esta capacitación fue acreditada con puntaje por el organismo educativo provincial en 2011, 2012 y 2013. B mariasilvina [email protected] Facultad de Ciencias Astronómicas y Geofı́sicas, UNLP, Paseo del Bosque s/n, 1900, La Plata, Argentina e Instituto de Astrofı́sica de La Plata (CCT La Plata - CONICET, UNLP) 1 187 Teaching & Outreach Short Talks TO -2 The IAU Office of Astronomy for Development: Opportunities for Latin America Kevin GovenderB1 In 2009, the IAU General Assembly approved a strategic plan to use astronomy as a tool for global development. Soon afterwards the IAU established its Office of Astronomy for Development (OAD) to realise a vision of ”Astronomy for a better world.” Since 2011 the OAD has established two regional offices and released two open calls for proposals. This presentation will discuss these and other activities of the OAD, specifically in the three focus areas of (i) universities and research; (ii) children and schools; and (iii) public outreach. The presentation will also focus on opportunities available for Latin America both in terms of developing the astronomy field and also using astronomy to stimulate development in the region. B 1 [email protected] IAU Office of Astronomy for Development 188 Short Talks Teaching & Outreach TO -2 The GalileoMobile Project 1 2 3 Benı́tez, S. ; Bhatt, M. ; Bonoli, S. ; Bühler, D.1 ; Canas, L.4 ; Candelaresi, S.5 ; Dası́ Espuig, M.1 ; Gomes, N.6 ; Joshi, J.1 ; Kobel, P.7 ; Penteado, E. M.8 ; Rivero González, J.9 ; Schoenell, W.10 ; Silva, P. B.4 ; Sordo, F.5 ; Spinelli, P. F.B11 ; Strubbe, L.12 ; Varguez, M.13 ; Vasquez, M.14 GalileoMobile is a traveling science education project by an international team of PhD students, recent graduates and science communicators (partnering with the Universe Awareness program) that brings astronomy to young people in regions where outreach science programs are a rare opportunity. Our primary project goals are: (1) to stimulate students’ curiosity and interest in learning, (2) to exchange different visions of the cosmos and cultures, and (3) to inspire a feeling of unity ”under the same sky” between people from different parts of the world. In 2009, GalileoMobile traveled to 30 schools in Chile, Bolivia and Peru, bringing handson activities and Galileoscopes; the team also produced a documentary movie to share the experiences and culture with the world. In 2012 the team accomplished two new expeditions, visiting 12 villages in the Indian state of Karnataka and 5 communities in the Bolivian Amazon. In 2013, GalileoMobile is heading to Uganda to a twelve-day trip (september 2013) to work in schools and villages. In these talk, I will briefly introduce the GalileoMobile project, review our methods and outcomes in the countries the project have visited and provide an outlook of our upcoming 2014 Brazil-Boliva (BraBo) expedition. B [email protected] Max Planck Institute for Astrophysics 2 Max Planck Institute for Solar System 3 University of Zurich 4 Navegar Foundation, Centro Multimeios de Espinho 5 Nordic Institute for Theoretical Physics 6 European Southern Observatory 7 École Polytechnique Fédérale de Lausanne 8 Institute for Molecules and Materials 9 University Observatory Munich 10 Instituto de Astrofı́sica de Andalucı́a 11 Museu de Astronomia e Ciências Afins 12 Canadian Institute for Theoretical Astrophysics 13 Humanistic Studies in Science and Culture of Monterrey Institute of Technology and Higher Education 14 Ferman Aerospace Center 1 189 Teaching & Outreach Short Talks TO -2 IOAA 2012: The first scientific international olympiad in Brasil, opening doors for 2016 Thais Mothé-Diniz1 ; Albert Bruch2 ; Carlos Alexandre Wuensche3 ; Eugênio Reis Neto4 ; Josina Nascimento5 ; Jorge CarvanoB5 ; Fernando Vieira6 ; Helio Jacques Rocha-Pinto1 ; Carlos Eduardo Quintanilha7 ; Jaime Fernando Villas da Rocha8 ; João Batista Garcia Canalle9 The International Olympiad on Astronomy and Astrophysics (IOAA) is an international level astronomy competition for high school students aged below 20 years old, held annually since 2007. In the years between 2007 and 2011 it was hosted by the founding countries: Thailand, Indonesia, Iran, China and Poland, with Brazil represented in all editions of the competition. Between 2012, August 04 and 14, the IOAA was hosted by Brazil, in the cities of Vassouras and Barra do Piraı́, in the state of Rio de Janeiro. Brazil hosted for the first time a scientific competition at an international level. Twenty six countries from four continents were represented, doing the exams, performing tasks and observations of the night sky, and experiencing the brazilian culture and hospitality. The VI IOAA counted with the collaboration of dozens of enthusiastic people, young and not so young astronomers, professionals and amateurs, volunteers, and people from many other areas of knowledge. Public schools and the general public benefited from the competition through the various open or semiopen activities offered by partner institutes and universities. The public schools of Vassouras city and Vale do Café region also benefited from the training on usage of the telescopes that were donated to them. The 6th IOAA organisation, with Vassouras Town Hall and partners, promoted activities opened to public during the IOAA, in the context of a ”Semana da Astronomia de Vassouras” (Vassouras Astronomy Week), with expositions, talks, movies, cultural shows, and others. To teachers an EREA (Regional Meeting on Astronomy Education) was offered, a large meeting of teachers training organised by the Brazilian Olympiad on Astronomy and Astronautics (OBA). The Olympiad represents more than a competition among students, but also friendship, information exchange and cooperation in astronomy education among astronomers. Moreover, it motivates the participating countries to hold their own national (and even regional) level astronomy competition, leading to the popularisation of astronomy in their countries. The aim of this work is to present the organisers’ view of the execution of the VI IOAA in Brazil, as well as its consequences to the popularisation of sciences in the country through activities during the olympiad and the parallel, subsequent and ongoing activities. A great amount of experience to be shared with others was gained through the VI IOAA in Brazil in 2012. It is also considered a first step towards the realisation of the idea to host a ”Knowledge Competition” in Brazil in 2016. B 1 2 3 4 5 6 7 8 9 [email protected] UFRJ / Observatorio do Valongo - OV MCTI / Laboratorio Nacional de Astrofisica - LNA MCTI / Instituto Nacional de Pesquisas Espaciais - INPE MCTI / Museu de Astronomia e Ciências Afins - MAST MCTI / Observatorio Nacional - ON Fundação Planetario do Rio de Janeiro Agência Espacial Brasileira - AEB Universidade Federal do Estado do Rio de Janeiro - UNIRIO Universidade do Estado do Rio de Janeiro - UERJ 190 Short Talks Teaching & Outreach TO -2 The Latin American Journal of Astronomy Education (RELEA): contributions and perspectives Bretones, P. S.B1 ; Jafelice, L. C.2 ; Horvath, J. E.3 The goal of this work is to present an analysis of articles published by the Latin American Journal of Astronomy Education (RELEA) since its beginning (2004) to the present. We analyzed the 59 articles available on the website of the journal (http://www.relea.ufscar.br), published in 15 issues. The articles were classified by: year of publication, issue, author’s institutions, grade level, focus of the study and content. The results show that the number of articles is still small - although the journal has been initially qualified as B3 within the Journal Ranking scheme Qualis CAPES and in the latest ranking (current) advanced to the concept B1 in the Qualis, it is too early to expect an increase in the number of articles submitted. Among the main factors for the relatively low number of articles we can mention that the initially nominated Editorial Board did not succeed in a proper dissemination of the journal and call for papers, the ongoing absence of a “critical mass” of astronomy education researchers and the lack of publishing tradition in the area. Important aspects of the writing of articles submitted are also discussed, such as refereeing, acceptance rate of articles, participation of authors from countries other than Brazil and theoretical and methodological frameworks, as well as the recent editorial restructuration of the international Editorial Board of the RELEA and the nomination of Associate Editors from Brazil. Concluding, it is possible to note the contribution to the field up to the moment through citations in other works in the field. However, it is necessary to advance with regard to: publishing more articles, articles from greater variety of Latin American countries, training of the community for a minimum quality of the writing of articles submitted for publication in a journal aimed at education research. In this sense, additional analyses of the published papers would be desirable. Finally, it is pointed out the need for greater dissemination of the journal to increase the number of submissions, encouraging the diversification of contents and methods and increase the participation of authors in general and from Latin America in particular, aiming to greater academic contribution for astronomy education at various levels and places. B 1 2 3 [email protected] DME, UFSCar Depto. de Fı́sica, UFRN IAG, USP 191 192 Posters 193 Planetary Systems PS -1: #1 Stellar occultation by the trans-Neptunian object 2002 KX14 A. Alvarez-CandalB1,2 ; J. L. Ortiz2 ; N. Morales2 ; R. Duffard2 ; S. Littlefair3 ; V. S. Dhillon3 ; B. Sicardy4 ; S. Mottola5 ; S. Hellmich5 ; T. Marsh6 ; T. Shahbaz7 On the night of April 25, 2012 we observed a stellar occultation by the trans-Neptunian object (119951) 2002 KX14 . Astrometric predictions had shown that the shadow path would pass upon Earth’s north hemisphere and was potentially favorable for the south of Europe and even the Canary islands. Several professional and amateur telescopes/observers attempted to observe the event. We had a successful observation from the 4.2-m William Herschel telescope at the Roque de los Muchachos observatory, La Palma, Spain, where the visiting instrument Ultracam was used. The occultation light-curve has a depth of 1.98 mag and lasted 21.2 s, this implies a minimum diameter of (414 ± 4) km. There is no evidence of atmosphere from the light-curve. B 1 2 3 4 5 6 7 [email protected] Observatório Nacional Instituto de Astrofı́sica de Andalucı́a University of Sheffield LESIA/Observatoire de Paris DLR/German Aerospace Center Institute of Planetary Research Department of Physics, University of Warwick Instituto de Astrofı́sica de Canarias 195 Planetary Systems Posters PS -1: #2 Rotation of Multi-layered Super-Earths Nelson Callegari Jr.B1 Super-Earths are planets with possible terrestrial-like composition and mass compared to the Earth mass. Many numerical studies on internal structure of these planets show a diversity of differentiation whose configuration depends on the mass of the planet, the initial composition of each layer before the reaching of the equilibrium, densities and other parameters. Due to the fact that several of these planets have compact orbits with orbital period with order of magnitude of days or less, some works have shown recently the complexity of dynamics of rotation of some of them, as is the case of 55 Cnc e. In the referred papers, it is considered a single homogeneous planet. In view of the multi-layered models of Super-Earths, a more complete model of rotation of the planet, characterized by the motion of the outer layer, can be done. In this work we show an improvement of the homogenous model on the basis of the efforts which consider gravitational coupling between the solid-like layers of planets or regular satellites. The main motivations of these works are theoretical modeling the mantle-inner core torque coupling of the Earth. We have prepared a numerical code with the equations of motion of differential rotation of the inner core and mantle where a large variety of internal configurations can be constructed, i.e., different sub-layers of the mantle. We apply them to different hypothetical interior structure of many previously studied Super-Earths (55 Cnc e, GJ 876d, KOI-55b, GJ 3634b). Numerical exploration of the rotation phase space show that, depending on the initial conditions and physical parameters like the density of the sub-layers, the effects of the gravitational coupling on rotation of the outer mantle can be important. For instance, new structures on the spin-orbit phase space might appear. B 1 [email protected] Instituto de Geociências e Ciências Exatas, Unesp - Univ Estadual Paulista 196 Posters Planetary Systems PS -1: #3 Stable low-altitude orbits around Ganymede considering a disturbing body in a circular orbit Cardoso dos Santos, J.B1 ; Carvalho, J. P. S.2 ; Vilhena de Moraes, R.2 Ganymede is one of the four Jupiter’s moons which compose the Galilean satellite. It is one of the planetary satellites of greater interest at the present moment among the scientific community. There are some missions being planned to visit Ganymede and the jovian system. It is possible cite, for example, the Europa Jupiter System Mission (EJSM). This mission is a cooperation between NASA and ESA in which is planned the insertion of the spacecraft JGO (Jupiter Ganymede Orbiter) into Ganymede’s orbit. Another mission being planned for visiting Ganymede is the Jupiter IcyMoon Explorer (JUICE/ESA). Thus, there is a great necessity for having a better comprehension of the dynamics of the orbits around this planetary satellite. This comprehension is essential for the sucess of this type of mission. In this context, this work aims to perform a search for low-altitude orbits around Ganymede. An emphasis is given in polar orbits. These orbits can be useful in the planning of aerospace activities to be conducted around this planetary satellite, with respect to the stability of orbits of artificial satellites. The study considers orbits of an artificial satellite around Ganymede under the influence of the third-body perturbation (the gravitational attraction of Jupiter) and the polygenic perturbations. These last ones occur due to forces such as the non-uniform distribution of mass ( J2 and J3 ) of the main (central) body. A simplified dynamic model for these perturbations is used. The Lagrange planetary equations, which compose a system of nonlinear differential equations, are used to describe the orbital motion of the artificial satellite around Ganymede. The equations showed here are developed using expansions in eccentricity. B 1 2 [email protected] UNESP UNIFESP 197 Planetary Systems Posters PS -1: #4 Disk-planet interactions de Paula, L. A.B1 ; Michtchenko, T. A.1 The study of planetary migration is the purpose of the present project. Planet migration is the process by which a planet’s orbital radius changes in time. The main agent for causing migration is the gravitational interaction of the young planet with the gaseous disk from which it forms. The already developed models predict two main types of migration, I and II. The first one is characteristic of low-mass planets which are embedded in the gaseous disk. The type II is characteristic of the large-mass planets which clear gaps in the disk around their orbits. Some other kinds of migration are also known and their dynamics will be explored. The main objectives are (i) the supervised learning of the existing models of planet migration in order to acquire enough new experience; (ii) application of the models over a variety of physical parameters; (iii) numerical simulations of migration processes B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo. 198 Posters Planetary Systems PS -1: #5 Improvement of TNO’s Ephemerides in the context of stellar occultations Desmars, J.B1 ; Braga-Ribas, F.1 ; Vieira-Martins, R.1 ; Camargo, J. I. B.1 ; Assafin, M.2 Trans-Neptunian Objects (TNO) and Centaurs are distant and faint solar system objects (around magnitude 20). They are consequently difficult to observe and poorly known objects. Due to their slow motion around the Sun, their orbits are inaccurate. However, stellar occultations are currently, the only way to precisely determine some physical characteristics of these objects. Actually, it is possible to determine the size or the shape with kilometric accuracy, or to highlight binary or multiple objects, or an eventual atmosphere as tenuous as few nanobars. The prediction of stellar occultations requires both accurate astrometry of stars and accurate ephemeris. The current methods of prediction use a constant offset compared to an ephemeris. The ephemeris used comes from Jet Propulsion Laboratory (JPL) and is determined by fitting the observations or by numerical integration of the osculating elements. The offset is calculated from the most recent observations as the mean difference between the observed positions and the ephemeris. This method assumes that the offset remains constant over a certain period (1 or 2 years). In this study, we perform a new ephemeris with available observations and observations done for offset determination. In this context, we have developed a dynamical model of the motion of asteroids (NIMA), fitted it to observations and determined a new ephemeris and its accuracy. Comparing the NIMA and JPL ephemerides, we show that the difference between the two ephemerides is close to the offset at the date of observations but this difference then varies over time, according to a periodic one-year term (mainly due to the parallax) and a secular term. For some objects, the method of the offset may however remain accurate when the time between observations and occultation is short or when the offset’s variations remain small. However, for other TNOs, the difference sharply increases making inaccurate predictions in the future. Consequently, new ephemerides should be used to make predictions. Finally, occultations also provide accurate astrometrical positions and therefore new constraints on the TNO’s motion. We analyze the contribution of previous occultations in the improvement of TNO’S ephemerides and in prediction of future occultations. B 1 2 [email protected] Observatório Nacional/MCTI, Brazil Observatório do Valongo/UFRJ, Brazil 199 Planetary Systems Posters PS -1: #6 Study of Pluto’s atmosphere from stellar occultation B1,2 Alex Dias de Oliveira ; B. Sicardy1 ; J. I. B. Camargo2 ; R. Vieira-Martins2 ; M. Assafin3 ; F. Braga-Ribas1,2 ; A. H. Andrei2 ; D. N. da Silva Neto4 ; A. Doressoundiram1 ; E. Lellouch1 ; F. Roques1 ; T. Widemann1 ; F. Colas5 ; C. Dumas6 ; V. D. Ivanov6 ; J. H. Girard6 ; J. L. Ortiz7 ; R. Andres8 ; L. Espinoza8 ; L. Vanzi8 ; E. Meza9 With the soon arrival of NASA’s probe New Horizons the demand for physical and dynamic information about the Pluto system became even greater. As far as ground-based observations are concerned, stellar occultations constitute the only technique capable of providing the temperature and density profiles of Pluto’s tenuous nitrogen atmosphere. On July 18, 2012, a multi-chord occultation by Pluto was observed from three stations in Chile: European Southern Observatory ESO/Paranal, San Pedro de Atacama and Santa Martina (near Santiago). Due to the brightness of the star in the IR (H magnitude= 11.1), the event was recorded with high signal-to-noise ratio at the ESO 8.2 m Very Large Telescope equipped with the NACO instrument, at a rate of 5 frames per second, without adaptative optics. This event provides one of the best data set ever obtained during a Pluto stellar occultation. It allows to build an accurate profile of Pluto’s atmosphere and reveal local fluctuations possibly caused by gravity waves. Using images taken 20 minutes before the occultations, we can measure the separate fluxes of the star and the Pluto-Charon system. This provides measurement of the residual stellar flux in the range 0.008 resid during the occultation. A preliminary analysis shows that resid lies 0.018, relative to the full unocculted stellar flux. This flux is related to the temperature gradient in the lower part of the atmosphere that connects Pluto’s surface (at 35 upper part (at about 105K). Our value of 40K) to the isothermal resid indicates a temperature gradient in the range 8 for that atmospheric region. Improved values of resid 15 K · km 1 will be given and constraints to Pluto’s radius will be presented, as well as temperature profiles derived from inversions of the ingress and egress light curves. This data will be combine with past information and new data (obtained in 04 May 2013 occultation) to provide a analysis of Pluto’s atmosphere evolution. B 1 2 3 4 5 6 7 8 9 [email protected] LESIA, Observatoire de Paris/Meudon Observatório Nacional, MCTI Observatório do Valongo, UFRJ Centro Universitário Estadual da Zona Oeste IMCCE, Observatoire de Paris/Meudon European Southern Observatory Instituto de Astrofı́sica de Andalucı́a, CSIC Pontificia Universidad Católica de Chile (PUC) Facultad de Ciencias, Universidad Nacional de Ingenierı́a, UNI 200 Posters Planetary Systems PS -1: #7 Small asteroid fragments in earth-crossing orbits Duha, J.B1 ; Afonso, G. B.2 The meteorite that fell in Chelyabinsk, Russia, naturally made many people think it could be a smaller companion of the Asteroid 2012 DA14, which passed close to Earth on that same day. Some asteroid specialists discarded this hypothesis for two main reasons: The meteorite was too far away from the asteroid, because the collision happened sixteen hours before the asteroid passed close to Earth. Moreover, it was not traveling, similarly to asteroid DA14, from south to north. However the possibility of the meteorite being a companion of the Asteroid 2012 DA14 cannot be completely discarded, due to the followings reasons: The Asteroid 2012 DA14, with a diameter of 45 meters, is very small. It can be considered an asteroid’s fragment, which is usually accompanied by other smaller fragments, scattered in space, practically in the same orbit and possibly being separated from each other by long distances. Therefore, the meteorite could be a smaller fragment that was ahead of the larger fragment of the original asteroid. Assuming that 2012 DA14 is not an isolated asteroid, but the biggest remaining fragment from a previous impact, we developed a model to study the dynamics of an asteroid fragment, similar to DA14, and its companions, the smaller fragments. This dynamically interesting encounter with planet Earth is addressed by generating the appropriate ephemerides and impact parameters. The orbital changes that could explain the Chelyabinsk event are discussed. As a result we find that, there could be a collision of a meteorite before, during, or after the Asteroid 2012 DA14 passing by, the same way that happens with meteorite showers, which can last several days. Now, because of the meteorite that crashed into Russia, there will be a bigger search for asteroid fragments that pass close to Earth in the world. Therefore, it would be very interesting to look for them, also, close to the larger fragments, more easily found. B 1 2 [email protected] Federal Institute of Paraná - IFPR Federal Institute of Amazonas - IFAM 201 Planetary Systems Posters PS -1: #8 Use of Mathematica software in the study of planetary dynamics Natasha Fioretto AgueroB1 ; Tatiana A. Michtchenko1 This work presents a study on how techniques provided by the algebraic manipulation software Mathematica can be used in the planetary dynamics investigations. The discovery of extra-solar planets orbiting other stars has been one of the major breakthroughs in astronomy of the past decades, changing our view on the features of planetary systems, mainly drawn from the observation of the Solar System. Today, over 800 exoplanets are known and the Kepler satellite has recently identified over 3000 additional candidates, most of them still awaiting for confirmation. We have learned that exoplanets are much more diverse when compared to our own Solar System. Thus, the implementation of advanced manipulation techniques can be of great importance for the investigation of such unusual configurations of these new worlds. We chose Mathematica, a software that has been increasingly used worldwide due to its great analysis power. The solutions of transcendent equations (e.g., Kepler’s equation), which cannot be determined through elementary functions, can be analyzed using the functions and the programming techniques employed by this software. The case that we focus is the 2/1 mean-motion resonance in the two-planet systems. Based on the Mathematica platform, we present animations of the evolution of the stationary solutions configurations as functions of the energy and the angular momentum of the system. The visualization of this evolution is very important to understand the complicated dynamical proprieties of resonant planetary systems. B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas (IAG), Universidade de São Paulo (USP) 202 Posters Planetary Systems PS -1: #9 Finding new planets around solar twins using the HARPS/ESO spectrograph Freitas, C. F.B1 ; Meléndez, J.1 We are using long time series of stellar spectra gathered with the HARPS spectrograph at the La Silla ESO observatory in order to detect small planets around solar twins through radial velocity variations. There are instrumental limitations (about 1 m/s) as well as those due to both stellar oscillations and stellar activity. To get rid of the effects of oscillations, we average several observations within the time scale expected for stellar oscillations, increasing thus the precision of our radial velocities. We are also studying the stellar activity of solar twins, because it can induce radial velocity variations that could be confused with the presence of planets. Finally, we are studying which lines are more sensitive to stellar activity, so that in future studies we can eliminate them before obtaining the radial velocity for a given observation, allowing thus a better precision to improve the detection of low-mass planets. B 1 [email protected] Universidade de São Paulo 203 Planetary Systems Posters PS -1: #10 Asteroids in the quasi-Hilda comet group R. Gil-HuttonB1,2 With the aim to identify dormant or extinct comet nuclei among the Hildas, the orbital parameters of more than 4000 of these asteroids were analyzed to find outliers in the quasi-hilda region. Around 1000 objects were found in this zone using the orbital excitation parameter and the planes of the Lagrangian elements as tools to discriminate between Hildas and quasi-hildas objects. Several of these outliers were integrated backward in time to know their recent dynamical evolution and to better find comet candidates among them. Preliminary results of this research are shown in this work. B 1 2 [email protected] Complejo Astronómico El Leoncito - CONICET San Juan National University 204 Posters Planetary Systems PS -1: #11 Dust production of the small satellites immersed in the arcs/ring of Saturn Giuliatti Winter, S. M.B1 ; Sfair, R.1 Images sent by the Cassini spacecraft showed a new structure in the ring system of Saturn, small satellites immersed in arcs/ring. The satellites Anthe, Methone and Aegaeon are embedded in an arc, while Pallene shares its orbit with a complete ring. All four satellites are located between the orbits of Mimas and Enceladus. The arcs, composed of small particles, are in corotation resonance with Mimas. These small satellites can be the source for the arc and the ring particle. In this work we analysed the dust production generated by collisions of interplanetary objects on the surfaces of the satellites. Satellites smaller than 10km are more efficient at generating dust particles since they are large enough to present a large cross-section and small enough to not hold the impact ejecta. For example the satellite Aegaeon, located in the G-ring arc, has a radius smaller than 1km. This satellite could be responsible for the maintenance of the ring, and also the arc, by generating particles thought collisions with interplanetary objects onto its surface. We used the algorithm present in Sfair and Giuliatti Winter (2012) to calculated the mass production of these satellites. By assuming the typical mass flux at Saturn to be 1.8 ⇥ 10 16 kg/ms2 and the nominal parameters of the planet and the satellite, we could determine the ejecta yield (Y) and the mass production rate (M + ). These values are found to be Y = 21153.86 and M + = 5.9 ⇥ 10 6 kg/s for the satellite Aegaeon, which produce about 104 kg of dust particles in a 100years. We also present the mass production of Anthe, Methone and Pallene and discuss the dynamics evolved in these systems. B 1 [email protected] UNESP - Univ. Estadual Paulista 205 Planetary Systems Posters PS -1: #12 Astrometric positions for the irregular satellites of Jupiter, Saturn and Neptune Gomes Jr, A. R.B1 ; Assafin, M.1 ; Vieira Martins, R.2 ; Camargo, J. I. B.2 The irregular satellites are smaller than the regular ones. They are more distant from the central body and have more eccentric orbits that may also be retrograde. Explaining their existence is a very important topic of study in Orbital Dynamics, and gives clues to the formation and evolution of the solar system. However, their orbits are known with poor precision. Therefore, a more dedicated observational work is necessary. We have organized and reduced thousands of CCD images from 11 Jovian and Saturnian irregular satellites plus Nereid. They were observed with the 1.6m and 0.6m telescopes from the OPD (Pico dos Dias Observatory LNA - Itajuba, IAU code 874). More than 4 thousand images were retrieved from a database with about 80 thousand images obtained between 1992 and 2012. In this work, we present the organization and astrometric reduction of these images. We processed all the 80 thousand images searching the satellites, what means reduct images from almost 10 CCDs in 3 telescopes using 6 different filters. Many of the older images were corrupted or had missing coordinates in their FITS headers. A big effort was made to separate and correct the data. We used the astrometric reduction package PRAIA. The UCAC4 was adopted as the reference frame. Positive aspects of the OPD data set are the large time span and the great number of observed positions. We eliminated bad observations to improve the astrometric precision using a sigma-clip procedure. We analyze the differences between the current ephemeris and the satellites positions for a better understanding of their orbit status. The projection of the orbits in the plane of the sky, with vectors which represent the position offsets relative to the ephemeris, was an important analysis tool. It clearly shows the level of contribution for improving the orbits. A similar work was done by our group with data from the Observatoire HauteProvence. We compared the results from both sets. The OPD positions have 40 mas precision. For some of the satellites, there are clear improvements to be made to the orbits, mostly in inclination, after a new integration is made with our new observed positions. B 1 2 [email protected] Observatório do Valongo - UFRJ Observatório Nacional - MCT 206 Posters Planetary Systems PS -1: #13 Shape effects on the spectra of asteroids Gonzales, J.B1 ; Carvano, J. M.1 Asteroids are irregular solar system bodies, with surfaces composed of grains of different sizes and mineralogical compositions. Their superficial composition can be infered with the aid of semi-empirical models of the bidirectional reflectance, which are commoly used to interpret the integrated reflectance spectra of asteroid that can be observed by Earth-based telescopes. Such interpretation is dificult because the asteroid spectra are complex nonlinear functions of grain size, mineral abundance and composition. The two widely-used regolith reflectance models are: the isotropic multiple-scattering approximation (IMSA) of Hapke (1993), based on the radiative transfer equation and, the one-dimensional geometrical-optics model for spectral albedo of powdered surfaces, of Shkuratov et al. (1999). These two theories are modeled under the assumption of a medium stratified and parallel planes . The semiempirical reflectance equation of Hapke has several free parameters, these are: size of grain, abundance, porosity, rugosity, etc. These model parameters can be obtained by fitting the reflectance measurements, having the optical constants of the mineral presents on the surface, using as input optical constants derived from laboratory spectra of meteorites and minerals. The objective of this work is to study the role of the asteroid shape on its observed spectra. For this, we generate a sythetic spectrum for a nonplanar geometry and, compare it with a spectrum generated with the same optical parameters as the first but, assuming a planar geometry. The observed differences between of two spectra are describe in terms of (1) the slope of the spectrum, width and depth of the absorption band, (2) differenties relatives of abundances and grain size, obtained by a fitting the hapke reflectance equation. B 1 [email protected] Observatório Nacional-ON, Rio de Janeiro-Brazil. 207 Planetary Systems Posters PS -2: #14 Identification of families halos in a multi-domain space composed by proper elements M. E. HuamanB1 ; V. Carruba1 ; R. C. Domingos2 ; D. Nesvorný3 ; F. Roig4 ; D. Souami5,6 If the large families are not limited to what found by hierarchical clustering methods (HCM) in the domain of proper elements (a,e,sin(i)), that seems to be biased to find compact, relatively young clusters, but that there exists an extended population of objects with similar taxonomies and geometric albedo, that can extend to much larger regions in proper elements and frequencies domains: the family ”halo”. Numerical simulations can be used to determining a good estimate of the possible orbital extension of a family ”halo” and provide estimates of the age of the family that can then be compared with ages of the family obtained with other methods. Other autors have identified families halos by: i) an analysis in proper elements domains, ii) or by using SDSS-MOC4 multi-band photometry to infer the asteroid taxonomy, iii) or by a combination of the two methods. The limited number of asteroids for which geometric albedo was known, were restricted in the past the extensive use of this additional parameter, which is however of great importance in identifying an asteroid taxonomy. But now a new availability of geometric albedo data from the WISE mission for about 100,000 asteroids significantly increased the sample of objects for which such information, with some errors, is now known. In this work we proposed a new method to identify families halos in a multi-domain space composed by proper elements, SDSS- MOC4 (a’,i-z) colors, and WISE geometric albedo for the whole main belt . Assuming that most families were created by the breakup of an undifferentiated parent body, they are expected to be homogeneous in colors and albedo. The new method is quite effective in determining objects belonging to a family halo, with low percentages of likely interlopers, and results that are quite consistent in term of taxonomy and geometric albedo of the halo members. B 1 2 3 4 5 6 [email protected] Unesp, Univ. Estadual Paulista, Grupo de Dinâmica Orbital e Planetologia, Guaratingueta, Brazil INPE, Instituto Nacional de Pesquisas Espaciais, São José dos Campos, Brazil SWRI, SouthWest Research Institute, USA ON, Observatório Nacional, Brazil UPMC, Université Pierre et Marie Curie, France SYRTE, Observatoire de Paris, Systèmes de Référence, Temps Espace, France 208 Posters Planetary Systems PS -2: #15 A New Paradigm for Habitability in Planetary Systems: the Extremophile Zone Janot-Pacheco, E.B1 ; Bernardes, L.1 About a thousand exoplanets habe been discovered so far. Planetary surface temperature may strongly depend on its albedo and geodynamic conditions. We have fed exoplanetary data from the Encyclopedia database (Schneider, 2013) with a comprehensive model of Earth’s atmosphere and plate tectonics. As the main greenhouse effect is CO2, its partial pressure has been taken as a free parameter to calculate the surface temperature of some known planets. We also investigated the possible presence of ”exomoons“ belonging to giant planets capable of harbour dynamic stability and to retain atmospheric layers and keep geodynamic activity for long time spans. Collected information on biological data of earthly micro-organisms classified as “extremophiles” indicate that such kind of microbial species could dwell on the surface of many exoplanets and exomoons. We thus propose an extension of the mainly astronomically defined “Habitable Zone” concept into the more astrobiologically “Extremophile Zone”, taking into account other refined parameters allowing survival of more robust life forms. This contribution comes from an ongoing project developed by a French-Brazilian colaboration in Astrophysics and Biophysics to search for living fingerprints in astrobiologically interesting exoplanets. B 1 [email protected] IAG-USP 209 Planetary Systems Posters PS -2: #16 Close-in planets around giant stars Jones, M. I.B1 ; Jenkins, J. S.1 ; Rojo P.1 ; Melo, C. H. F.2 In 2009 we started a RV survey aimed at studying the population of planets in close-in orbits around giant stars. So far, we have collected multi-epochs spectra for a sample of 166 bright targets in the southern hemisphere, resulting in the discovery of several planets and binary systems. Additionally, many other substellar candidates in long-period orbits have emerged, which still have to be confirmed. In this talk I will present the goal of our project, the observing strategy and the reduction analysis. Finally I will present our results and I will discuss about the possible explanation for the lack of close-in planets orbiting post-MS stars. B 1 2 [email protected] Universidad de Chile ESO 210 Posters Planetary Systems PS -2: #18 Dynamical evolution of differentiated asteroid families Martins-Filho, W. S.B1 ; Carvano, J. M.1 ; Mothe-Diniz, T.2 ; Roig, F.1 The project aims to study the dynamical evolution of a family of asteroids formed from a fully differentiated parent body, considering family members with different physical properties consistent with what is expected from the break up of a body formed by a metallic nucleus surrounded by a rocky mantle. Initially, we study the effects of variations in density, bond albedo, and thermal inertia in the semi-major axis drift caused by the Yarkovsky Effect. The Yarkovsky Effect is a non-conservative force caused by the thermal re-radiation of the solar radiation by an irregular body. In Solar System bodies, it is known to cause changes in the orbital motions (Peterson, 1976), eventually bringing asteroids into transport routes to nearEarth space, such as some mean motion resonances. We expressed the equations of variation of the semimajor axis directly in terms of physical properties (such as the mean motion, frequency of rotation, conductivity, thermal parameter, specific heat, obliquity and bond albedo). This development was based on the original formalism for the Yarkovsky Effect (i. e., Bottke et al., 2006 and references therein). The derivation of above equations allowed us to closely study the variation of the semi-major axis individually for each physical parameter, clearly showing that the changes in semi-major axis for silicate bodies is twice or three times greater than for metal bodies. The next step was to calculate the orbital elements of a synthetic family after the break-up. That was accomplished assuming that the catastrophic disruption energy is given by the formalism described by Stewart and Leinhardt (2009) and assuming an isotropic distribution of velocities for the fragments of the nucleus and the mantle. Finally, the orbital evolution of the fragments is implemented using a simpletic integrator, and the result compared with the distribution of real asteroid families. B 1 2 [email protected] Observatório Nacional, ON/MCT, Rio de Janeiro, RJ, Brasil Observatório do Valongo, UFRJ, Rio de Janeiro, RJ. Brasil 211 Planetary Systems Posters PS -2: #19 The Evolution of the G Ring Arc under the Effects of the Resonance with Mimas and the Solar Radiation Force Mourão, D. C.B1 ; Giuliatti Winter, S. M.1 ; Sfair, R.1 The small satellite Aegaeon, less than 1km across, is embedded in an arc located in the G ring of Saturn. This satellite belong to a new class of structures imaged by the Cassini spacecraft, which is formed by small satellites immersed in arcs. Aegaeon is also locked in a 7:6 corotation resonance with the satellite Mimas. It has been proposed that Aegaoen, along with a set of large particles located in this arc, is responsible for the maintenaince of the G ring against dissipative forces. In this work, we study the orbital evolution of a sample of tiny particles (sizes ranging from 1 to 10µm) under the gravitational effects of Mimas and the solar radiation pressure. These particles were initially located in the arc about ±20km from the semimajor axis resonance of Aegaeon with ±30 in longitude. Our results show that, despite the particles are initially in a corotation resonance with Mimas, the effects of the solar radiation pressure remove the particles from the arc in a timespan of 50yrs. These particles stay confined in the G ring. B 1 [email protected] UNESP - Univ Estadual Paulista 212 Posters Planetary Systems PS -2: #20 Programa de observación de ocultaciones de estrellas desde el Observatorio Nacional de Llano del Hato O. NaranjoB1 ; G. Navas2 ; P. Rosenzweig1 ; E. Guzmán1 ; R. Alvarez1 ; L. Zerpa1,2 ; J. Villarreal1,2 ; N. Villa La observación de ocultaciones de estrellas por objetos del Sistema Solar permite el estudio de la posible atmosfera presente en el objeto que oculta a la estrella, su forma, tamaño y verificar la existencia de posibles satélites asociados al mismo. Recientemente, hemos comenzado la observación de ocultaciones de estrellas por objetos del Sistema Solar, usando los telescopios Reflector f/5; f/21 de 1-m y el telecopio Refractor de 0.65-m del Observatorio Nacional de Llano del Hato, Mérida. En ambos telescopios se ha acoplado una cámara CCD en su foco. Hasta el presente se ha observado ocultaciones de estrellas por planetas menores, objetos cercanos a la Tierra, cometas y el satélite Titan de Saturno. Algunas de estas ocultaciones observadas no coinciden con las predicciones de su trayectoria. En este trabajo se presentan algunos resultados de estas observaciones. B 1 2 [email protected] Universidad de los Andes, Facultad de Ciencias, Departamento de Fı́sica, Grupo de Astrofı́sica Teórica. Mérida-Venezuela Centro de Investigaciones de Astronomı́a (CIDA) 213 Planetary Systems Posters PS -2: #21 Observación de objetos cercanos a la Tierra (Observation of Neos) O. Naranjo1 ; G. NavasB2 ; P. Rosenzweig1 ; E. Guzmán1 ; L. Zerpa1,2 ; R. Alvarez1 ; J. Villarreal1,2 ; D. Collazo1 El estudio de objetos cercanos a la Tierra es importante por cuanto permite conocer sobre las propiedades fı́sicas de estos objetos, su origen y las condiciones existentes en el sistema solar durante su formación. Además, por la ubicación única de nuestro observatorio cercano al ecuador terrestre, nos permite el monitoreo de objetos moviéndose norte y sur y viceversa. Estas observaciones fueron realizadas usando el telescopio Reflector f/5; f/21 de 1-m del Observatorio Nacional de Llano del Hato, junto con el sistema de filtros BVRI. La astrometrı́a y fotometrı́a realizada sobre cada objeto nos permitió determinar su posición en la órbita, su color y curva de luz. Se presentan resultados obtenidos de la observación de varios objetos cercanos a la Tierra. Palabras Claves: Objetos cercanos a la Tierra, planetas menores, atmósferas, astrometrı́a, fotometrı́a B 1 2 [email protected] Universidad de los Andes, Facultad de Ciencias, Departamento de Fı́sica, Grupo de Astrofı́sica Teórica. Mérida-Venezuela Centro de Investigaciones de Astronomı́a (CIDA) 214 Posters Planetary Systems PS -2: #22 The Behavior of Regular Satellites during the Nice Model’s Planetary Close Encounters Nogueira, E. C.B1,2 ; Gomes, R. S.2 ; Brasser, R.3 The behavior of the regular satellites of the giant planets during the instability phase of the Nice model needs to be better understood. In order to explain this behavior, we used numerical simulations to investigate the evolution of the regular satellite systems of the ice giants when these two planets experienced encounters with the gas giants. For the initial conditions we placed an ice planet in between Jupiter and Saturn, according to the evolution of Nice model simulations in a ‘jumping Jupiter’ scenario (Brasser et al. 2009). We used the MERCURY integrator (Chambers 1999) and cloned simulations by slightly modifying the Hybrid integrator changeover parameter. We obtained 101 successful runs which kept all planets, of which 24 were jumping Jupiter cases. Subsequently we performed additional numerical integrations in which the ice giant that encountered a gas giant was started on the same orbit but with its regular satellites included. This is done as follows: For each of the 101 basic runs, we save the orbital elements of all objects in the integration at all close encounter events. Then we performed a backward integration to start the system 100 years before the encounter and re-enacted the forward integration with the regular satellites around the ice giant. These integrations ran for 1000 years. The final orbital elements of the satellites with respect to the ice planet were used to restart the integration for the next planetary encounter (if any). If we assume that Uranus is the ice planet that had encounters with a gas giant, we considered the satellites Miranda, Ariel, Umbriel, Titania and Oberon with their present orbits around the planet. For Neptune we introduced Triton with an orbit with a 15% larger than the actual semi-major axis to account for the tidal decay from the LHB to present time. We also assume that Triton was captured through binary disruption (Agnor and Hamilton 2006, Nogueira et al. 2011) and its orbit was circularized by tides during the ⇠500 million years before the LHB. B 1 2 3 [email protected] Universidade Federal Fluminense, Brasil Observatório Nacional, Brasil Institute for Astronomy and Astrophysics, Academia Sinica, Taiwan 215 Planetary Systems Posters PS -2: #23 Small-body colors from the UV to the IR: bringing together all space and ground-based observations Penteado, P.B1 ; Trilling, D.1 The main current asteroid taxonomical systems are defined from ground-based observations, limited to 3100-10600 Å (Tholen, Zellner et al. (1985)), and 4400-9200 Å (SMASS, Bus and Binzel (2002))). This narrow wavelength range does not include several regions useful to determine asteroid properties, such as: 1) the well-known spectral features in the near-IR (20000-50000 Å) that differentiate between common asteroid and meteorite minerals and indicate the presence of water, methane or other volatiles; 2) the far IR, which probes the bodies’ emission, thermal inertia and albedo; 3) the UV, where the degree of darkening probes the surface grain properties and space weathering. The few existing studies using multiple instruments from the UV to the IR (ground, Earth-orbit and flyby observations) have been limited to targeted observations of special-interest bodies (Perna et al., 2013, Kueppers et al. 2013, Müller et al. 2012, to name just the most recent). We aim to obtain UV to IR colors of a large sample of bodies, to study how they are distributed and how these colors differentiate among bodies with similar spectra on the standard taxonomies. The data are being gathered from archives of multiple space- and ground-based instruments: GALEX, HST, SDSS, 2MASS, Spitzer, WISE and Herschell. Such a combined use of multiple archived observations is commonly done for fixed (non-Solar System) astronomical targets, which can be easily found by their RA and Dec. To obtain such data for Solar System bodies, we built a database to index all archive observations of each known body. We used their orbits, integrated into the past, to build an index in the Time/RA/Dec domain, where we locate each archive footprint to determine if it contains a known Solar System body. We present a preliminary cluster analysis, using a small sample of objects identified in multiple instruments, as well as the magnitude distributions on different colors, for a larger sample of objects, which were not matched among the different instruments. In the future we will expand the database to include more observations (more instruments and more bodies), and the populations we identify will be compared to spacecraft UV to IR spectra of those few bodies observed in close passes and with high resolution spectra. B 1 [email protected] Department of Physics and Astronomy, Northern Arizona University 216 Posters Planetary Systems PS -2: #24 The most common habitable planets – atmospheric characterization of the subgroup of fast rotators Pinotti, R.B1 The current search for habitable planets has focused on Earth-like conditions of mass, volatile content and orbit. However, rocky planets following eccentric orbits, and drier than the Earth, may be a more common phenomenon in the Universe. For the subgroup of fast rotators, it is suggested that their atmospheric thermal capacitance, subject to the radiative forcing of their parent stars, may provide researchers in the near future with a simple method for the determination of a robust lower limit of atmospheric thickness. This technique, together with the spectroscopic analysis of resolved planets from their stars, both allowed by planned spaceand ground-based observatories with thermal infrared capabilities, would enable us with a better understanding of the habitability of this class of planets. The technique works better for shorter orbital periods, but since the tidal-lock radius ofMdwarfs encompasses their Habitable Zone (HZ), the optimum targets would be planets around K dwarf stars. The atmospheric thermal capacitance could also expand the range of HZs for shorter orbits, particularly for planets around M dwarf stars, since the higher frequency of the periodic radiative forcing dampens the surface temperature variation considerably. B 1 [email protected] Observatório do Valongo, Universidade Federal do Rio de Janeiro, UFRJ 217 Planetary Systems Posters PS -2: #25 Asteroids Atiras: study of stability and dynamical analysis of the region Ribeiro, A. O.B1 ; De Prá, M. N.1 ; Roig, F.1 ; Carvano, J. M.1 The Near Earth Asteroids (NEAs) are a dynamic group of asteroids with perihelium q < 1.333 UA. Dynamical studies show that the NEAs are an unstable population, and that the Main-Belt is the main source for replenishing asteroids in that region. The NEAs are divided in four subgroups: Amor, Apollo, Aten e Atira. In the literature, objects with aphelium Q < 0.983 UA are usually called Atiras, Inner Earth Object (IEO), and sometimes Apohele. Being extremely difficult to observe due to it’s proximity to the Sun, only 12 Atiras are presently known, while dynamical arguments and extrapolation from the known polulation suggests an expected population of around 375 asteroids in this region. An important aspect of the objects in this region is the threat they may represent, since several dynamic mechanism (as, for example captures by secular resonances and/or close encounters with Venus and Mercury) may reinject these objects em Earth crosser orbits. This work proposes a dynamical study of the region of Atiras asteroids. A grid with 2500 test particles with semi-mayor axis between 0.2UA and 0.38 UA; eccentricity between 0 and 0.8, were equidistantly distributed. All particles have orbital inclination of 0.05o and the remaining orbital elements were fixed with the mean value of the observed Atiras asteroids. For each point in the grid, the orbit diffusion coefficient is calculated and a map of the diffusion in the region is made. The results show a region of stability between 0.2 UA and 0.3 UA in semi-mayor axis for eccentricity until 0.4. It is possible to identify the 9:7 resonance with Mercury, this temporarily stabilizes the objects a increase the eccentricity. This region of stability found can help to design more target surveys and improve the odds of detecting new Atiras B 1 [email protected] Observatório Nacional, Rua General José Cristino 77, Rio de Janeiro, 20921-400, Brazil 218 Posters Planetary Systems PS -2: #26 Spin-Orbit Resonances in Super-Earth Systems Close to Mean-motion Commensurabilities Ribeiro, F. B.B1 ; Callegari Jr., N.2 There is a great deal of planets in close-in orbits and low mass on order of magnitude less than 10 Earth mass. Valencia et al. (2006) call them by Super-Earths. Recently, several efforts have been done in order to understand the dynamical of rotation of these planets, including spin-orbit resonance and spin tidal evolution. In the referred papers, it is considered a single planet whose motion around the star is governed by the rules of the two-body problem. However, many Super-Earths are present in system where other terrestrial or giant planets are present, and that problem must be checked. In this work we study the dynamical effects of mean-motion commensurabilities on rigid body rotation and spin-orbit resonances. Emphasis is given in the cases of the multi-planetary systems Kepler-11, KOI-55 and KOI-961, where the mean motions of several pairs of planets are commensurable. In some cases we have observed that the period associated to a particular commensurability is close to the period of the free libration of the rotation of one of the super-Earths. Thus, we investigate the role of the mean motion resonance on the synchronous rotation. Depending on the initial conditions inside the synchronous domain, the stable librations induced by the torque of the central star on the figure of the planet can lead to instabilities on its rotation which is not expected in such regular regions of rotational phase space. This phenomenon has been observed in the cases of Kepler-11 b (disturbed by Kepler-11 c), KOI-55 b (disturbed by KOI-55 c), KOI-961c (disturbed by KOI-961b and KOI-961d). B 1 2 [email protected] UNESP, Physics Department, Rio Claro, SP, Brazil UNESP, Demac, Rio Claro, SP, Brazil 219 Planetary Systems Posters PS -3: #27 V-type asteroids among the Mars crosser population 1 B1 Ribeiro, A. O. ; Roig, F. ; Cañada-Assandri, M.2,3 ; Carvano, J. M.1 ; Jasmin, F. L.1 ; Alvarez-Candal, A.1,4 ; Gil-Hutton, R.2,3 We search for asteroids belonging to the V taxonomic class which have not been detected up to now among the populations of Mars crossing asteroids. This is motivated by the fact that the Mars crossing regime is a path to deliver asteroids from the Inner Main Belt to the Earth crossing space, and both the Inner Main Belt and the population of Earth crossing asteroids contains a significant fraction of V-type bodies. We selected 18 candidate V-type asteroids in the Mars crossing region using observations contained in the Sloan Digital Sky Survey Moving Objects Catalog. Then, we observed 4 of these candidates to take their visible reflectance spectra using the Southern Astrophysical Research Telescope (SOAR). We also performed the numerical simulation of the orbital evolution of the observed asteroids. We confirmed that 3 of the observed asteroids belong to the V class, and one of them follows a path that drives it to an Earth collision in a few tens of million years. B 1 2 3 4 [email protected] Observatório Nacional, Rio de Janeiro, Brazil Universidad Nacional de San Juan, San Juan, Argentina Complejo Astronómico El Leoncito - CONICET, San Juan, Argentina Instituto de Astrofı́sica de Andalucı́a - CSIC, Granada, Spain 220 Posters Planetary Systems PS -3: #28 Photometry and Spectroscopy of Asteroids Rich in Volatils of the Type Main Belt Comets (MBC) Rondón, E.B1 ; Carvano, J. M.1 ; Lorenz-Martins, S.2 Nine asteroids of the main belt have shown cometary activity. These objects have been called Main Belt Comets (MBC). The physical source of their activity can be diverse; among the possible causes are collision and sublimation. In this work we use a dust distribution model associated with the asteroid coma to study the photometric and spectroscopic properties of these objects, from which we can estimate the parameters associated with position of the particle in the coma, the size of the grain and with the velocity distribution, and thus simulating a collision in the asteroids. We study the influence of grain size on the spectrum of asteroids, using the Hapke model for the sun light reflected at the surface asteroids and attenuated by the coma, and using the monte carlo method for the sun light scattered by the coma into the line of sight of the observer, following the approach of Carvano & Lorenz (2010) which modeled the effects of a faint dust coma on the asteroid (5201) Ferraz-Mello spectra and other objects. This model was capable to produce an increase in the reflectance in the shorter wavelength, and they show that the presence of a faint coma produces unusual reflectance. In our model, we study other distribution for the grains and we added the effect of the solar phase angle on the spectra. B 1 2 [email protected] Observatório Nacional (COAA), Rua Gal. José Cristino 77, São Cristóvão, CEP 20921-400 Rio de Janeiro RJ, Brazil Universidade Federal do Rio de Janeiro/Observatório do Valongo. Ladeira do Pedro Antônio, 43 - 20080-090 Rio de Janeiro, Brazil 221 Planetary Systems Posters PS -3: #29 The IMPACTON project: rotational properties of NEAs B1 Silva J. S. ; Lazzaro D.1 ; Rodrigues T.1 ; Carvano J. M. F.1 ; Roig F.1 ; Dos Santos E.1 ; Jasmin F. L.1 ; Gonzales J.1 ; Ribeiro A. O.1 ; Hasselmann P. H1 ; Nascimento M.1 The main scientific goal of the IMPACTON project is to characterize the physical properties, of the largest possible number of NEOs discovered by other search projects (Lazzaro et al. 2012). In the present paper we will report about the rotational properties of a set of NEAs. The observations were carried on at the 1m telescope of the Observatório Astronômico do Sertão de Itaparica (OASI, MPC code Y28), located in the North-eastern part of Brazil. The photometric observations were obtained between March and June, 2012, using a 1024 x 1024 pixels CCD, with a 13 x 13 micron size, and the R filter (Johnson). Among the observed NEAs we computed the rotational period for (85818) 1998 XM4, , (312473) 2008 SX245, (330825) 2008 XE3, being 5.8, 3.4 and 4.0 hours, respectively. For other objects only strong indications on the rotational period were obtained, among these are: (154007) 2002 BY, (112221) 2002 KH4, (326732) 2003 HB6, 2006 VY13, 2011 YV15. B 1 [email protected] Observatório Nacional 222 Posters Planetary Systems PS -3: #30 Connecting the Circumstellar Habitable Zone to the Galactic Habitable Zone Sime, M. K.B1 ; Friaça, A. C. S.1 The circumstellar habitable zone (CHZ) is the region around a star where a planet can exhibit liquid water on its surface, which is essential for the life as we know it. The outer boundary of the CHZ is sensitive to the amount of greenhouse effect. The main greenhouse gases are water vapor, carbon dioxide and methane. Therefore, if there is a larger availability of carbon, the greenhouse effect due to carbon dioxide as methane increases. In the present work we explore the carbon connection which links galactic evolution models and the extension of the CHZ. The galactic habitable zone (GHZ) is the region of the Galaxy within which the probability of life arises and survives is higher. The boundaries of the GHZ are determined by the survival probability against catastrophic events (Sne, GRBs), the probability of the formation of Earth-like planets and long timescales for Darwinian Evolution. We perform calculations of the GHZ using a chemical evolution model for the Galaxy. A novelty of the present work is that we focus on the evolution of carbon to derive a constraint between biomass (heavily dependent on the carbon abundance) and the extension of the CHZ, reflection the amount of greenhouse effect, which, in turn, is dependent on the carbon abundance. B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo 223 Planetary Systems Posters PS -3: #31 Stellar occultations by trans-Neptunian objects Vieira-Martins, R.B1 ; Braga-Ribas, F.1 ; Camargo, J. I. B.1 ; Assafin, M.2 ; Sicardy B.3 The discovery of the trans-Neptunian objects (TNOs) since 1992 led to the development of new models about the giant planets’ initial evolution, giving rise to new insights on the formation of the solar system. The consolidation of these models depends on a more detailed knowledge of the physical properties of TNOs such as mass, density, shape, albedo and atmosphere’s detection. The goal of our work concerns the determination of these parameters for a significant number of objects. As their distances do not allow a good determination of their physical parameters, we use the technique of stellar occultations. It consists of observing the star’s light variation when an object passes between the star and the observer. This technique allows obtaining the TNOs’ sizes with accuracies of few kilometers which combined with other data provides the physical parameters above. Almost 10 years ago we associated to a large international collaboration that develops a important effort in order to observe stellar occultations by outer solar system objects. Today this collaboration is being led by three groups based in Paris, Granada and Rio. They perform the predictions of short and long-term occultations, the organization of observational campaigns, the reductions and analysis of data. In particular, the Rio Group has developed a process for long-term predictions (up to 2015) for 50 TNOs, which involved the construction of a catalog of 20 million stars down to 20th magnitude with positions that have astrometric precisions better than 50 mas. This catalog was obtained from observations made with the wide-field camera (WFI) of the 2.2-meter telescope at La Silla/ESO. In order to refine de previsions our group started in the Brazilian Laboratório Nacional de Astrofı́sica a systematic program of astrometric observations of stars and objects involved in some future occultations. We constructed a web page to inform the observers, which is updated several times a week with the refinements of the predictions, and we are organizing in Brazil an observer network involving professional and amateur astronomers. We have also actively worked in the reductions and analysis of the light curves resulting from occultations. All this work has given rise to several articles in journals with our participation. At this meeting we will present an overview on the main results achieved in our occultations’ works. Details of these results will be presented in other communications in this meeting. B 1 2 3 [email protected] Observatório Nacional Observatório do Valongo/UFRJ Observatoire de Paris/Meudon 224 Posters Planetary Systems PS -3: #32 Morphological analysis of the tail structures of comet 1P/Halley 1910 II Voelzke, M. R.B1 ; Izaguirre, L. S.2 Eight hundred and eighty six images from September 1909 to May 1911 are analysed for the purpose of identifying, measuring and correlating the morphological structures along the plasma tail of 1P/Halley. These images are from the Atlas of Comet Halley 1910 II (Donn et al., 1986). A systematic visual analysis revealed 304 wavy structures along the main tail and 164 along the secondary tails, 41 solitary waves (solitons), 13 Swan-like tails, 26 disconnection events (DEs), 166 knots (regions of higher density of matter) and six shells. While the wavy structures denote undulations or a train of waves, the solitons refer to the formations usually denominated kinks. In general, it is possible to associate the occurrence of a DE and/or a Swan-Tail with the occurrence of a knot, but the last one may occur independently. It is also possible to say that the solitons occur in association with the wavy structures, but the reverse is not true. The 26 DEs documented in 26 different images allowed the derivation of two onsets of DEs, i.e., the time when the comet supposedly crossed a frontier between magnetic sectors of the solar wind (Brandt and Snow, 2000). Both onsets of DEs were determined after the perihelion passage with an average of the corrected velocities Vc equal to (57 ± 15) km s 1 . The mean value of the corrected wavelength c measured in 70 different wavy structures is equal to (1.7 ± 0.1) ⇥ 106 km and the mean amplitude A of the wave (measured in the same 70 wavy structures cited above) is equal to (1.4 ± 0.1) ⇥ 105 km. The mean value of the corrected cometocentric phase velocity Vpc measured in 20 different wavy structures is equal to (168 ± 28) km s 1 . The average value of the corrected velocities Vkc of the knots measured in 36 different images is equal to (128 ± 12) km s 1 . There is a tendency for A and c to increase with increasing cometocentric distance. The results of this work agree with the earlier research from Voelzke and Matsuura (1998), which analysed comet P/Halley’s tail structures in its last apparition in 1986. B 1 [email protected] Cruzeiro do Sul University 225 Planetary Systems Posters PS -3: #33 Contributions of geomorphology for the understanding of landscape evolution in rocky planets of the Solar System Alexandre, S. T.B1 ; Nunes, N. A.1 ; Guerra, A. J. T.1 The combination of endogenous, exogenous and dynamic processes is responsible for the way landforms are shaped on Earth. The application of geomorphology, a branch of science dedicated to understanding the land-surface in connection with the processes that created it, with sophisticated planetary imaging technologies, is improving our knowledge on the formation and evolution of surface features in different contexts. Using Mars as model-object, this study aims to apply the knowledge of geomorphology and related sciences for understanding the processes and evolution of the Martian relief. Using mapping techniques of Jmars and Jearth, we attempt to draw connections between morphostructure and morphology of an area on Mars, Candor Chasma, and an area on Earth related to the feature of canyons. The comparison of the two bodies can provide valuable clues on similarities and differences on the evolution of these planets. B 1 [email protected] Laboratory of Environmental Geomorphology and Soils Degradation, Federal University of Rio de Janeiro. 226 Posters Planetary Systems PS -3: #34 Finding ’jumps’ in light curves using change-point algorithms Boufleur, R. C.B1 ; Emilio, M.2 ; de la Reza, J. R.1 ; Janot-Pacheco, E.3 In the search for extra solar planets using the transit method, astronomers are concerned in to obtain the maximum information of the photons received from the stars. Such transits produce characteristic effects in the light curves which allow to determine some physical parameters of the planet candidate. The incidence of high-energy particles and the consequent hot pixels generation, or even thermal variations of the instrument, cause sudden changes in the light curves at short time intervals. Thereby an algorithm for the identification and treatment of such phenomena in data is as important as a good transit search due to bias introduced. A set of techniques known as change-point are commonly employed in various fields of knowledge to detect abrupt variations in observations at short intervals of time. In an extensive comparison Reeves et al. (2007) shows that there is not an unique improved algorithm which covers all the cases. The decision on which to use depends on various characteristics of the time series analyzed, including the range and the occurrence frequency of these breaks in the series. On the other hand, Jann (2000) studied the occurrence of multiple change-point time series. We develop in this work a methodology using change-point algorithms dedicated to the detection and location of jumps in the light curves. The statistics we used to do the calculations involved the standard homogeneity test. We show that our preliminary results are satisfactory and as events of abrupt change does not appear periodically opposed to transit ones they meet with the future objectives of the project that aims at the same time to detects the change-points and transits based on the probability density results. B 1 2 3 [email protected] ON - MCTI. Rio de Janeiro, Brasil UEPG. Ponta Grossa / PR. Brasil IAG/USP. São Paulo. Brasil 227 Planetary Systems Posters PS -3: #35 Towards understanding the late evolution of protoplanetary disks Caceres, C.B1 Understanding the evolution of circumstellar disks around young stellar objects is crucial for theories of star and planet formation. Most young stellar objects are either accreting classical T Tauri stars with “full” disks or non-accreting weak-line T Tauri stars (WTTSs) with bare stellar photospheres, which suggests that the transition phase between the two states must be very short. Currently, the only mechanism able to consistently explain the rapidly vanishing disks is photoevaporation. However, the photoevaporation rates predicted by current models differ by several orders of magnitude which makes modelling of protoplanetary disk evolution a rather difficult exercise. We use ALMA cycle 0 observations of a large sample of WTTS in Lupus to conclusively distinguish primordial photoevaporating disks from young debris disks. We derive mass limits for all the disks in our sample which puts tight constraints on current photoevaporation models. B 1 [email protected] Universidad de Valparaiso 228 Posters Planetary Systems PS -3: #36 Finding minor Bodies with the JPAS/J-PLUS photometric surveys De Prá, M. N.B1 ; Carvano J. M. F.1 ; Lazzaro D.1 ; Roig F.1 ; Mothé-Diniz T.2 ; Alvarez-Candal, A.1 ; J-PAS Team The JPAS/J-PLUS is a joint Spanish-Brazilian project that aims to map an area of the sky of 8000 square degrees, in order to measure, with unprecedented accuracy, the redshifts of a large sample of extragalactic objects up magnitude 23. It involves the installation of two telescopes on the Javalambre Mountains, in Spain. The T250 telescope will have an aperture of 250cm and will be equipped with a camera with a 3 square degree field of view and will use a set of 56 filters (54 narrow band + 2 wide band) covering the 0.31.0 micron range, while the T80 telescope (presently on commissioning phase) will have a camera with 2 square degree field of view and will use a set of 12 narrow and intermediate band filters covering the same wavelength range. During its execution, the surveys will also observe a large number of minor Solar System bodies. Here we will discuss the expected efficiency of the J-PLUS survey in finding minor bodies. B 1 2 [email protected] Observatório Nacional Observatório do Valongo 229 Planetary Systems Posters PS -3: #37 Transit Timing Variations analysis in exoplanet host stars B1 Petrucci, R. ; Jofre, E.2 ; Schwartz, M.1 ; Cúneo, V.1 ; Martı́nez, C.2 ; Saker, L.2 ; Ferrero, L.2 ; Artur, E.2 ; Gómez, M.2 ; Mauas, P.1 In June of 2011 we started a continuous photometric monitoring of transiting planets host stars in the southern hemisphere, with the aim of searching for periodic variations in their mid-transit times. Such variations (or TTVs) are produced by the gravitational action of other bodies in the system that disturb the semimajor axis and therefore the orbital period of the transiting planet. The smaller the mass of the disturber the lower the amplitude of the variation and therefore high precision (tens of seconds) is required to measure the central transit times. In this paper, we present a full analysis of TTVs of one of the objects with transits observed from 2011 to the present. B 1 2 [email protected] Instituto de Astronomı́a y Fı́sica del Espacio, Argentina Observatorio Astronómico de Córdoba, Argentina 230 Posters Planetary Systems PS -3: #38 About Hohmann Transfer with Orbital Plane Change Ángel RincónB1 ; Patricio Rojo1 We analitically studied the generalized Hohmann orbital transfer by considering non coplanar and elliptical orbits instead of planar and circular. It was done in order to find the transfer orbit that minimizes the energy and therefore missing mas of a satellite through the application of two non-tangetial impulses. We found an analytical expression that leads to minimize the fuel cost after assuming some reasonable physical constraints. Finally, we discuss some possible configurations and applications to our model. B 1 [email protected] Astronomy department, Universidad de Chile 231 Planetary Systems Posters PS -3: #39 Palaeogeographic reconstruction of Minchin palaeolake system, South America: the influence of astronomical forcing Andrea Sánchez-Saldı́asB1 ; Richard A. Fariña2 Current palaeoclimatic reconstructions for the Rı́o de la Plata region during the latest Pleistocene (30,000 to 10,000 years BP) propose dry conditions, with rainfall at the Last Glacial Maximum amounting to onethird of today’s precipitation. Despite the consequential low primary productivity inferred, an impressive megafauna existed in the area at that time. Here we explore the influence of the flooding from a huge extinct system of water bodies in the Andean Altiplano as a likely source for wet regimes that might have increased the primary productivity and, hence, the vast number of megaherbivores. The system was reconstructed using specifically combined software resources, including Insola, Global Mapper v13, Surfer and Matlab. Changes in water volume and area covered were related to climatic change, assessed through a model of astronomical forcing that describes the changes in insolation at the top of the atmosphere in the last 50,000 years BP. The model was validated by comparing its results with several proxies (CH4, CO2, D, 18O) from dated cores taken from the ice covering Antarctic lakes Vostok and EPICA Dome C. It is concluded that the Altiplano lake system drained towards the southeast in the rainy seasons and that it must have been a major source of water for the Paraná-Plata basin, consequently enhancing primary productivity within it. B 1 2 [email protected] Universidad de la República, Facultad de Ciencias, Departamento de Astronomı́a, Iguá 4225, 11400 Montevideo, Uruguay Universidad de la República, Facultad de Ciencias, Laboratorio de Paleobiologı́a, Iguá 4225, 11400 Montevideo, Uruguay 232 Posters Planetary Systems PS -3: #40 Photometry of Hot-Jupiters Type Exoplanets in Transiting Systems Hickel, G. R.1 ; Siqueira, M. F. F. T.B2 The current project aims find candidates for temporal high resolution and multiband photometry at SOAR (Southern Astrophysical Research Telescope) of exoplanets such as Hot-Jupiters in transiting planetary systems. The number of exoplanets discovered in transiting planetary systems significantly expanded in the last 3 years, due the great performance of COROT and KEPLER satellites. Many of these discovered exoplanets are Hot-jupiters type, gas giants like the jovian prototype, orbiting their host star with lesser distances than Mercury does in relation to the sun. Most of them need follow-up in transiting observations to refine orbital and physical parameters. The temporal high resolution photometry (exposure time < 1% transiting time) with small photometric erros (S/R > 1000) can be obtained on SOAR using the SOI and SPARTAN imagers. The multiband transiting photometry can even provide evidences of the exoplanet’s high atmosphere features. B 1 [email protected] Universidade Federal de Itajubá 233 234 Stars & Stellar Systems SSS -1: #41 The BIOSUN project:an astrobiological approach to study the origin of life in the context of the young Sun/solar stellar analogs Abrevaya, X. C.B1 ; Hanslmeier, A.2 ; Leitzinger, M.2 ; Odert, P.2 ; Horvath, J. E.1 ; Ribas, I.3 ; Galante, D.1,4 ; Porto de Mello, G. F.5 During the early ages of the Earth the magnetic activity of the young Sun was much stronger than the observed from the present Sun, in particular causing proportionally higher amounts of radiation emitted below 1700 Å. Such enhanced particle/high-energy radiation fluxes play a role in the evolution of planetary atmospheres and therefore on their surface conditions. Moreover, it is supposed that life arose on the Earth in this environment, therefore it is thought that radiation could have had an important role in the origin and evolution of life. Interestingly, solar stellar analogs could provide some relevant information about the characteristics of the Young Sun (age < 0.8 Gyr) which could allow the investigation of the radiation environment of the early Earth among other planetary bodies. The objective of this project is to focus on the radiation emission features of the young Sun through solar stellar analogs (mainly based on the data obtained by “The Sun in Time” project) to characterize the radiation environment of the early Earth and other planetary bodies of the Solar System that are or could have been potentially inhabited by life as we know it, in particular considering Venus, Earth, Mars and Europa and their early evolution. The next step will be to reproduce this radiation environment under laboratory conditions to explore: 1) Whether cells could survive at that level of radiation on the early Earth confronting that with the hypothesis that first cells could have arose around 3.8-3.5 Gyr ago according to the microbial fossil record. Additionally, the environments of Mars and Europa will be tested; 2) The possibility of “transfer” of microorganisms between Earth, Mars and Venus at that time; 3) The formation, inflow and outflow of some prebiotic molecules in the early planetary conditions. The experimental approach will be carried out exposing microorganisms to simulated environments according to the data obtained previously. The irradiation sources will be a solar simulator for UV radiation and a synchrotron accelerator for X-rays. Microorganisms selected are cyanobacteria (the oldest entries in the fossil record, found in stromatolites) and halophilic archaea (UV-tolerant features, also found in modern stromatolites analogs of the older stromatolites on the Earth, the fact of their apparent longevity since they were found in evaporites from Permian and Triassic and its link to martian evaporites). B [email protected] Research Unit in Astrobiology (NAP-Astrobio), Institute of Astronomy, Geophysics and Atmospheric Sciences, Universidade de São Paulo, São Paulo, Brazil 2 Institute of Physics, Karl-Franzens-Universität Graz, Graz, Austria 3 Institut de Ciencias de l’Espai , CSIC, Spain 4 Brazilian Center for Research in Energy and Materials (CNPEM) / Brazilian Synchrotron Light Source (LNLS), Campinas - SP, Brazil 5 Observatorio do Valongo, Universidade Federal do Rio de Janeiro, Rio de Janeiro, Brazil 1 235 Stars & Stellar Systems Posters SSS -1: #42 A long-term study of the Be star Mu Centauri in the L-band Aguayo, G.B1,2 ; Martayan, C.2 ; Mennickent, R. E.1 ; Baade, D.3 ; Rivinius, T.2 ; Stefl, S.4 ; Fabregat, J.5 We present 10 L-band spectra of the Be star Cen obtained with the VLT ISAAC distributed along 1 year during an epoch of relative photometric quiescence. We observe significant changes in emission line strength of Bracket- and Pfund- lines relative to Humphreys lines. We interpret this variability as monotonic changes in the opacity of the circumstellar envelope, moving from an optically thin to an optically thick condition. This behavior is observed just prior to the triggering of a major outburst. B [email protected] Universidad de Concepción, Departamento de Astronomı́a, Casilla 160-C, Concepción, Chile. 2 European Organisation for Astronomical Research in the Southern Hemisphere, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile. 3 European Organisation for Astronomical Research in the Southern Hemisphere, Karl-Schwarzschild-Str. 2, D-85748 Garching b. Muenchen, Germany. 4 ESO/ALMA, The European Organisation for Astronomical Research in the Southern Hemisphere/The Atacama Large Millimeter/Submillimeter Array, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile. 5 Observatorio Astronómico de Valencia, edifici Instituts d’investigació, Poligon la Coma, 46980 Paterna Valencia, Spain 1 236 Posters Stars & Stellar Systems SSS -1: #43 Determination of Li abundance in Solar type stars of intermediate brightness Eliana Maritza Amazo-GómezB1 ; Bosco Hernandez-Aguila2 ; Miguel Chavez Dagostino2 ; Emanuele Bertone2 ; Victor de la Luz2 The determination ofthe Li abundance (ALi) in stellar atlnospheres is of fundamental importance in multiple contexts of contemporary astrophysics. On one hand, the Li present in stars with global subsolar chemical abundances provides a strong restriction on the abundance of this clement as a result of primordial nueleosynthesis. On the other hand, Li is one of the few age indicators for field stars with convective envelopes. Additionally, Li abundance appear to be correlated with the presence of sub-stellar companions, perhaps even more correlated than global chemical composition. We present preliminary results of a project aimed at determining the Li abundances of an extended sample of solar like stars (spectral type G and lulninosı̀ty class V) of intermediate brightness. High resolution spectroscopic data (R=65000) were obtained with the CANHiS Echelle Spectrograph on the 2.11n telescope of the Guillermo Haro Observatory in Cananea, Sonora, Mexico. Measured equivalent Widths and appropiate model atmopsheres for each star have been incorporated into the LINEWIDTH the program to detelmine the abundance of Li. B 1 2 [email protected] Universidad Nacional de Colombia Instituto Nacional de Astrofı́sica, Óptica y Electrónica INAOE 237 Stars & Stellar Systems Posters SSS -1: #44 H accretion disc maps of V2051 Oph along outburst: additional evidence in favor of the mass-transfer instability model Andrade, E.B1 ; Baptista, R.1 Dwarf novae (DNs) are mass-exchanging binaries showing repeated outbursts, lasting from days to weeks and recurring on timescales from weeks to years, in which their accretion discs brighten by factors 20-100 either because of a thermal-viscous instability cycle in the accretion disc (the DI model) or as a consequence of an instability in the mass-donor star leading to a burst of enhanced mass-transfer (the MTI model). While the issue seemed to be settled in favor of the DI model, the last decade has progressively provided compelling evidence in support of the idea that there is a group of DN the outbursts of which are powered by MTI. V2051 Oph is one of the DNs yielding stronger evidence in favor of the MTI (Baptista et al. 2007). Here we report eclipse mapping analysis of velocity-resolved (|v| = 400 1000 km/s) H light curves of V2051 Oph on 4 consecutive nights along its 2002 July outburst, based on spectroscopy collected with the 1.5 m ESO telescope. The outburst starts with a ring of enhanced emission at the circularization radius, which spreads inwards and outwards with velocities of 0.89 km/s and +0.16 km/s, respectively, to form an extended bright disc in less than a day. The outburst maximum disc shows two asymmetric arcs reminiscent of the spiral arms seen in other outbursting dwarf novae. The disc cools along the decline phase, with a cooling wave that accelerates from 0.12 km/s (at ' 0.3 RL1 ) to 0.42 km/s (at ' 0.2 RL1 ) as it moves towards the inner disc regions. The results are at odds with predictions of the DI model (cooling front deceleration), but are in good agreement with the expected response of a viscous disc to a burst of dense, enhanced massaccretion through its sparse outer regions. B 1 [email protected] Universidade Federal de Santa Catarina 238 Posters Stars & Stellar Systems SSS -1: #45 Fast and slow radiation-driven wind solutions using ZEUS-3D Araya, I.B1 ; Curé, M.1 ; ud-Doula, A.2 ; Santillán, A.3 Currently, the theory of radiation–driven winds of massive stars posses three known solutions for the velocity and density profiles of the stellar winds, namely: the fast, ⌦–slow and –slow solutions. In order to confirm their stability we use a time–dependent numerical hydrodynamic code called ZEUS-3D, and then we compare their results with the stationary solutions from our numerical hydrodynamic code. ZEUS-3D needs an initial trial solution to start to integrate, for this we use the stationary solution (from our code) or a –law for the velocity field. In both cases we obtain the same results. Fast and both slow stationary solutions are attained in ZEUS-3D and are all stables. Furthermore, there is a very good agreement with the velocity and density fields from ZEUS-3D and our code, having differences between the terminal velocities lower than 3%. In addition, we found that ZEUS-3D is very sensitive to the boundary conditions (base density and velocity profile), in some cases we obtain kinks in the velocity profiles, similar to the ones obtained by Madura et al. (2007) for stars with high rotation. We conclude that these kinks are because the initial trial solution is “far” from the stationary solution. Currently, we are exploring the effects of small perturbation at the base of the wind in order to study possible transitions or oscillations between –slow and fast solutions. B 1 2 3 [email protected] Universidad de Valparaı́so, Chile Penn State Worthington Scranton, USA Universidad Nacional Autónoma de México, México 239 Stars & Stellar Systems Posters SSS -1: #46 Effects of enhanced neutrino emission on the evolution of low-mass stars Arceo-Diaz, S.B1 ; Schroeder, K-P.2 ; Zuber, K.3 With a laboratory limit of 3.2 ⇥ 10 11 µB , provided by Beda et. al. (2011), almost ten times larger than the one currently predicted by Astrophysics, the neutrino magnetic dipole moment is a property out of the standard model that remains unverified. Its existence has a important impact on the evolution and internal properties of stars, as it has been already discussed by several authors, as it enhances the emission of neutrinos, via plasmon decay, that can take energy away from dense stellar matter. We use the well tested Eggleton code for stellar evolution to analyze the consequences of this enhanced neutrino emission in the evolution of low mass stars, (internal structure and observable parameters) from main sequence to the horizontal branch. We focus, on particular, on the possible differences in tip-RGB luminosity for stellar models of around one solar mass and different metallicities, for different rates of enhanced neutrino cooling, at the eve of the Helium flash. To calculate the plasma-neutrino emissivity we use the currently most accurate fitting formula, Kantor et. al. (2007), and consider the prescription of Raffelt et. al. (1992) for the nonstandard contribution to the neutrino vector current. Finally, we comment on the impact of nonstandard neutrino emission on the calibration of the Reimmers mechanism for not dust-driven mass loss in red giants and the possibility that standard ingredients of stellar theory, as chemical abundances and rotation of the stellar core, can be responsible for the changes attributed to nonstandard neutrino emission. B 1 [email protected] Departamento de Astronomia, Universidad de Guanajuato, Mexico. 240 Posters Stars & Stellar Systems SSS -1: #47 Wind study of B supergiants stars Arcos, C.B1 ; Curé, M. 1 ; Kanaan, S.1 The estimation of the stellar and wind parameters of the B supergiants stars, give us important information to understand the evolution of these. In recent years, different codes have been developed based on the radiation-driven wind theory to estimate such parameters. It is known from previous studies that the A nonrotating (or slow rotation) supergiant stars can have two types of solution: one fast and one slow. Here we study the two types of solutions for the B supergiant star: HD41117, using the FASTWIND code with beta law and then modified-FASTWIND code that use the hydrodynamics from HYDWIND code). B 1 [email protected] Universidad de Valparaı́so, Chile. 241 Stars & Stellar Systems Posters SSS -1: #48 On magnetic fields in barotropic stars Armaza, C.B1 ; Reisenegger, A.1 ; Valdivia, J. A.2 ; Marchant, P.1,3 Although barotropic matter does not constitute a realistic model for magnetic stars, it would be interesting to confirm a recent conjecture that states that magnetized stars with a barotropic equation of state would be dynamically unstable (Reisenegger 2009). In this work we construct a set of barotropic equilibria, which can eventually be tested using a stability criterion. A general description of the ideal MHD equations governing these equilibria is summarized, allowing for both poloidal and toroidal magnetic field components. A new finite-difference numerical code is developed in order to solve the so-called Grad-Shafranov equation describing the equilibrium of these configurations, and some properties of the equilibria obtained are briefly discussed. B [email protected] Instituto de Astrofı́sica, Facultad de Fı́sica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile 2 Departamento de Fı́sica, Facultad de Ciencias, Universidad de Chile, Casilla 653, Santiago, Chile 3 Argelander Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, D-53121, Bonn, Germany 1 242 Posters Stars & Stellar Systems SSS -1: #49 Searching for cyclical period variations in cataclysmic variable stars Bernardo BorgesB1 ; Raymundo Baptista2 ; Alexandre de Oliveira3 Cataclysmic variables (CVs) are close binary systems where the late-type star (the secondary) overfills its Roche lobe and transfers matter to a white dwarf (the primary) via an accretion disc. In this poster we report some results of the search of cyclical period variations in three cataclysmic variables: UU Aqr, V2051 Oph and VZ Scl (orbital periods of 3.9, 1.5 and 3.5 hours, respectively). These systems were monitored from 2008 to 2013 at Observatório do Pico dos Dias (OPD/LNA, Brazil) as part of long-term project to detect/characterize cyclical period variations in CVs. Times series of high speed CCD photometry were obtained using the 0.6 m and 1.6 m telescopes at OPD. We measured new white-dwarf mid-eclipse timings and combined them with published measurements to construct updated observed-minus-calculated (O-C) diagrams. The UU Aqr OC diagram covers 24 years of observations and presents a 26 yr modulation with semi-amplitude of 47 s. The V2051 Oph data cover 35 years of observations and the new timings show significant deviations from the published linear plus sinusoidal ephemeris (22 yr modulation with a semi-amplitude of 17 s), indicating that the variation is not strictly periodic. We are unable to detect period changes in VZ Scl due to short coverage (less than one decade). We discuss the observed modulations in UU Aqr and V2051 Oph in context of the two current explanations for the phenomenon: magnetic activity in the secondary star and the presence of a third body in the system. B 1 2 3 [email protected] UFSC/Araranguá,Brazil UFSC, Brazil UNIVAP, Brazil 243 Stars & Stellar Systems Posters SSS -2: #50 Unveiling Type IIb Supernova Progenitors Bufano, F.B1 Type IIb Supernovae are the final evolutionary stage of massive stars that were able to retain only a thin (< ⇠1 M ) H/He external envelope at the time of the explosion. The mechanism of mass-loss that made such final structure possible and the nature of such progenitor stars are still open issues. We present the preliminary results obtained from the study of a sample of Type IIb SNe. In particular, we present SN 2011hs, a IIb SN with peculiar properties: very high velocities measured from the spectroscopic lines and a faint and narrow bolometric light curve, pointing to a low-mass He core progenitor star, as confirmed by the comparison with hydrodinamical models. Finally, we obtain evidences for a progenitor with a radius of the order of 500-600 R , corresponding to an extended star as in the case of SNe 1993J and 2011dh. B 1 [email protected] Universidad Andres Bello, Chile 244 Posters Stars & Stellar Systems SSS -2: #51 Detailed differential chemical analysis of a poor metal star: new evidences about planet formation Carlos, M. G. C. C.B1 ; Meléndez, J.2 ; Milone, A. C.1 The present project emphasizes on the study of metal-poor stars, with and without planets, to investigate the existence (or not) of a connection between anomalies in the chemical composition and the presence of planets by inspecting the high resolution spectra (R = 65 000), in order to derive chemical abundances with high precision using the differential technique. In this method, measurements of equivalent widths of the target star are compared to a standard star with predetermined photospheric parameters that are similar to those of the target star (effective temperature, surface gravity and metallicity). Therefore, we have compared the star HD111232 (standard) with HD020794, such that the first holds a hot Jupiter-type planet and around the second one there are three super-Earths. These solar-type stars are moderately metal-poor and had their spectra collected with the MIKE spectrograph at the 6.5m Magellan telescope in the Las Campanas Observatory. Among the main results, we have derived the classical photospheric parameters and chemical abundances of refractory and volatile elements with such a high precision, particularly with errors about 0.01 dex, which is essential for the study of chemical connection between planets and star. We have also added to the differential method the spectral synthesis of molecular bands and atomic lines to recover abundances of volatile elements such as carbon, nitrogen, oxygen, and potassium. We thus present the parameters effective temperature, surface gravity, metallicity [Fe/H], microturbulence velocity and differential elemental abundances. For some elements, we have performed comparisons of the abundances measured by spectral synthesis with those obtained directly through measurements of equivalent widths. B 1 2 [email protected] Instituto Nacional de Pesquisas Espaciais Universidade de São Paulo 245 Stars & Stellar Systems Posters SSS -2: #52 Characterization and search for periodicities on coronal mass ejections (CME) occurrence Cecatto, J. R.B1 ; Guedes, M. R. G.1 It is well known that coronal mass ejections (CME) are solar phenomena corresponding to huge amounts of gas being ejected from solar atmosphere to the interplanetary space. Typical velocities of several hundred to few thousand km/s have been measured to ejected CME with an average of about 470 km/s. In principle, the CME rate of occurrence should accompany the solar cycle activity. However, a distinct behavior has been observed since the decay phase of the 23rd cycle. We studied CME start times recorded by LASCO experiment on board Soho satelite, during the period from 1996 up to 2012, to investigate and characterize their occurrence. This period enclose since the beggining of 23th solar cycle till actual maximum phase of cycle 24. Also, we search for periodicities on CME occurrence. Yet, we suggest possible interpretations to the unexpected high rate of CME occurrence during the period of 2005-2008. B 1 [email protected] Astrophysics Division, National Institute for Space Research 246 Posters Stars & Stellar Systems SSS -2: #53 On the origin of the wind variability of 55 Cyg M. Haucke1 ; M. Kraus2 ; R. Venero1 ; S. Tomic2 ; L. CidaleB3 ; M. Cure4 The hot supergiant star 55 Cyg shows strong spectroscopic variability. Drastic changes in the P Cygni profiles of hydrogen lines take place in a matter of hours. In order to understand the origin of this variability, we study an extensive sample of spectroscopic observations taken at the Observatory of Ondrejov (Czeck Republic). We model the wind of 55 Cyg with FASTWIND code and derive the relevant parameters. Then we discuss the mechanisms that could lead to the variable nature of the wind. B 1 2 3 4 [email protected] Facultad de Ciencias Astronomicas y Geofı́sicas, UNLP, La Plata, Argentina Observatory of Ondrejov, Czeck Republic Instituto de Astrofı́sica de La Plata, CCT-La Plata, CONICET-UNLP, Argentina Departamento de Fı́sica y Meteorologı́a, Facultad de Ciencias, Universidad de Valparaiso, Chile 247 Stars & Stellar Systems Posters SSS -2: #54 The Study of Physical Parameters of Unclassified Stars with the B[e] Phenomenon M. Boges Fernandes1 ; Cesar A. H. CondoriB1 During the last years, the models of stellar evolution have had huge advances, obtaining a good agreement with the observations, thanks to the inclusion of ingredients like rotation, mass loss and different metallicities. However, despite these advances, there are some phases for stars of different masses that are short and with few objects already identified, which are still poorly known. They are called transition phases and as an example, we have the stars with the B[e] phenomenon. This phenomenon occurs in objects of different evolutionary stages, as pre-main sequence stars of intermediate mass (Herbig Ae/Be), evolved stars of low and high mass (compact planetary nebulae and supergiant stars) and symbiotic objects. However, most of the stars with the phenomenon B[e] in the galaxy still have their physical parameters unknown, being called of unclassified B[e] stars (unclB[e]). In this work, we will present the results of the analysis of high resolution spectra obtained with the ESO/FEROS for a sample of 6 galactic unclB[e] stars. We obtained spectral atlas for all of these objects, deriving radial velocities, equivalent widths, and also estimating their physical parameters and distance, allowing us a better knowledgement of the nature of these stars. B 1 [email protected] Observatório Nacional/MCT 248 Posters Stars & Stellar Systems SSS -2: #55 The VVV Templates Project B1 R. Contreras Ramos 1 ; M. Catelan ; R. Angeloni1 ; I. Dékány1 ; C. Navarrete1 ; F. Gran1 ; A. Jordán1 ; J. Alonso-Garcı́a1 ; R. K. Saito1 ; J. Borissova2 ; The VVV Templates Team Until now, stellar variability in the near-IR has been a relatively ill-explored research field: in particular, the number of high-quality light curves was very limited and, even worse, many variability classes have not yet been observed in a sufficiently extensive way in the near-IR, so that good light curves are entirely lacking for some such classes. Since VVV is the first ever large survey dedicated to stellar variability in the near-infrared, the first problem we had to face has thus been the construction of a proper statistically significant database of high-quality (i.e., template) near-IR light curves for a significant sample of stars taken to be representative of the different variability classes under study. The main purpose of the VVV Templates Project is thus to build a large database of well-defined, high-quality, near-IR light curves for variable stars of different types, which will form the basis of the VVV automated classification algorithms. B 1 2 [email protected] Pontificia Universidad Católica de Chile Universidad de Valparaı́so, Chile 249 Stars & Stellar Systems Posters SSS -2: #56 Extensive MultiConfiguration calculations of oscillator strengths useful for Astrophysics Applications Cruzado, A.B1 ; Di Rocco, H. O.2 ; Marchiano, P. E.3 The goal of this work is to obtain oscillator strengths (gf ) of spectral lines of astrophysical interest. On the one hand, by using appropiate codes, we theoretically obtain the gf values. This involves: i) calculation of radial functions by means the Hartree-Fock (HF) method or some of its different approximations, ii) calculation of radial integrals, iii) calculation of atomic energy levels, and iv) obtaining of the spectrum, which means, wavelengths, gf values, and transition probabilities of the lines. On the other hand, we empirically obtain the gf values. This implies: i) obtaining of line wavelengths from laboratory experiments, ii) calculation of atomic energy levels, and iii) obtaining of gf values and transition probabilities of the lines. The comparison of the gf values obtained theoretically by adopting different approximations to the general HF method, among themselves and with the empirical values, is itself a goal of our work. In addition, we aim to estimate the effects of the uncertainties associated with obtaining gf values in the calculation of stellar abundances. In the atmospheres of chemically peculiar stars, it is critical the accurate determination of the abundance of some chemical elements, as well as their possible variations with the time. With this in mind, we begin our analysis with spectral lines observed in the spectrum of He-weak, Hestrong, HgMn, and Ap stars. B 1 2 3 [email protected] Facultad de Ciencias Astronomicas y Geofisicas, Universidad Nacional de La Plata, Argentina Instituto de Fisica de Arroyo Seco, Universidad Nacional del Centro de la Provincia de Buenos Aires, Argentina Facultad de Ciencias Astronomicas y Geofisicas, Universidad Nacional de La Plata, Argentina 250 Posters Stars & Stellar Systems SSS -2: #57 A new method to disentangle the rotational velocities of stars: application to main-sequence field Stars Curé, M.B1 ; Rial, D. F.2 ; Cassetti, J.3 ; Christen, A.4 The projected rotational velocity v sin i is a fundamental observable quantity. In order to obtain the rotational velocity distribution of a sample of v sin i, Chandrasekhar & Münch (1950) developed a formalism to obtain this distribution under the assumption that rotational axes are uniformly distributed, but this method is not usually applied due to an intrinsic numerical problem associated to the derivative of an Abel’s integral. An alternative iterative method was developed by Lucy (1974) to disentangle the distribution function of this kind of inverse problem, but this method has no convergence criteria. Here we presented a new method to disentangle the distribution of rotational velocities, based on Chandrasekhar & Münch (1950) formalism. We obtain the cumulative distribution function (CDF) of the rotational velocities from projected velocities (v sin i) under the standard assumption of uniform distributed rotational axes. Through simulations the method is tested using a) theoretical Maxwellian distribution functions for the rotational velocity distribution and b) with a sample of about 16.000 main-sequence field stars. Our main results are: The method is robust and in just one step gives the cumulative distribution function of rotational velocities. When applied to theoretical distributions it recovers the CDF with very high confidence. When applied to real data, we recover the results from Carvalho et al. (2009) proving that the velocity distribution function of main–sequence field stars is non–Maxwellian and are better described by Tsallis or Kaniadakis distribution functions. B 1 2 3 4 [email protected] Universidad de Valparaı́so, Chile Universidad de Buenos Aires, Argentina Universidad Nacional de General Sarmiento, Argentina Pontificia Universidad Católica de Valparaı́so, Chile 251 Stars & Stellar Systems Posters SSS -2: #58 Self-consistent physical parameters for 5 intermediate-age SMC stellar clusters from CMD modelling Dias, B.B1,2 ; Kerber, L.1,3 ; Barbuy, B.1 ; Santiago, B.4 ; Ortolani, S.5 ; Balbinot, E.4 Stellar clusters in the Small Magellanic Cloud are fundamental pieces to study the chemical and dynamical evolution of this neighbouring dwarf galaxy, enabling inspection of a large period covering ⇠10 Gyr. The main goals of this work are the derivation of age, metallicity, distance modulus, reddening, core radius and central density profile for each cluster, and place them in the context of the Small Cloud evolution. The studied clusters are: AM 3, HW 1, HW 34, HW 40, Lindsay 2, and Lindsay 3, where HW 1, HW 34, and Lindsay 2 are studied for the first time. Optical colour-magnitude diagrams (V, B-V CMDs) and radial density profiles were built from images obtained with the 4.1m SOAR telescope, reaching V ⇠ 23. The determination of structural parameters were carried out applying King profile fitting. The other parameters were derived in a self-consistent way by means of isochrone fitting, which uses the likelihood statistics to identify the synthetic CMDs that best reproduce the observed ones. Membership probabilities were determined comparing the cluster and control field CMDs. Completeness and photometric uncertainties were obtained performing artificial star tests. The results confirm that these clusters (except HW 34, identified as a field fluctuation) are intermediate-age clusters, with ages between ⇠1 and ⇠5 Gyr. Their metallicities follow the age-metallicity relation by Pagel & Tautvaisiene (1998), with some spread as described by Parisi (2009) and Piatti (2011). In particular HW 1, Lindsay 2, and Lindsay 3 are located in a region that we called West Halo. (Based on paper by Dias et al. 2013, submitted to A&A). B 1 2 3 4 5 [email protected] IAG, Universidade de São Paulo European Southern Observatory, Chile Universidade Estadual de Santa Cruz Universidade Federal do Rio Grande do Sul University of Padova 252 Posters Stars & Stellar Systems SSS -3: #59 V/R variations in Be shell stars Escolano, C.B1 ; Carciofi, A. C.1 ; Rivinius, Th.2 ; Stefl, S.2 Be stars are rapidly rotating non-supergiant B type stars surrounded by a circumstellar disk. Both theoretical and observational evidences converge toward the model of viscous decretion disk to describe their physics. In that model, a geometrically thin disk - orbiting at Keplerian velocities - is formed by viscous diffusion of the material ejected episodically from the central star. From their build-up to their decay and even their disappearance, Be disks experience various dynamical processes, on timescales of years. One of the most obvious indicator of their strong activity is the so-called V /R variability, i.e. the quasi-cyclic variations of the violet and red emission peaks intensity observed in neutral hydrogen lines. Such variability is generally explained by a global oscillation of the disk, forming a one-armed spiral density perturbation precessing around the central star. Some Be stars exhibit sharp absorption troughs in their Balmer and metallic lines; they are classified as shell stars. Shell lines are usually found in Be stars observed with their disk edge-on, suggesting that the difference between ’normal’ and ’shell’ Be stars might be purely geometric. Interestingly, shell lines also exhibit variations of their width and depth as the disk rotates. Those variations, as well as the V /R variations evoked previously, are the spectroscopic translation of the structure and dynamics of Be disks. As a matter of fact, studying shape variations of various lines, formed in different regions, might provide valuable informations about the physics of the disk. I will present the results of an analysis performed with the fully-3D radiative transfer code HDUST. The analysis is focused on V/R variations of hydrogen Balmer lines in shell stars. By applying Gaussian fits to the line profiles computed with HDUST, we are able to quantify their width, their height and their degree of asymmetry, all indicative of the physical conditions in their formation region. The same treatment will be applied to the observed spectra of ⇣ Tau and 48 Lib - two well-known shell stars vastly studied by our group and compared to simulations. B 1 2 [email protected] Institute of Astrophysics and Geophysics (IAG), São Paulo University (USP), Brasil ESO, Santiago, Chile 253 Stars & Stellar Systems Posters SSS -3: #60 Classical Cepheids from long-baseline interferometry: diameters, distances, circumstellar envelopes and binarity Gallenne A.B1 ; Kervella P.2 ; Mérand A.3 ; Breitfelder J.2,3 ; Gieren W.1 Optical interferometry is the only technique giving access to milli-arcsecond resolution at infrared wavelengths. For Cepheids, this is a powerful and unique tool to measure distances in a pseudo-geometric way, and probe the close circumstellar environment. While the mean angular diameter allow us to probe the pulsation mode, its angular and linear variation can provide the distance to the star. Independent distance measurements are particularly interesting because classical Cepheids are used as primary distance indicator in the local group. Interferometry also enables to probe the close environment of these stars, and so study their circumstellar envelope (CSE) and the companions. The characterization of these CSEs is particularly important as they give access to the present mass-loss rate of Cepheids. These CSEs were probably formed through past or ongoing mass loss, possibly generated by shock waves in the pulsating atmosphere of the Cepheid. Their presence can also biased the distance estimate in the Baade-Wesselink method. Finally, when Cepheids are in binary system, we can investigate their age and evolution, estimate the mass and distance, and constrain theoretical models. However, most of the companions are located too close to the Cepheid (⇠ 1 40 mas) to be observed with a 10-meter class telescope. The only way to spatially resolve such systems is to use long-baseline interferometry. B 1 2 3 [email protected] Universidad de Concepción, Departamento de Astronomı́a, Casilla 160-C, Concepción, Chile LESIA, Observatoire de Paris, CNRS UMR 8109, UPMC, Université Paris Diderot, 5 Place Jules Janssen, F-92195 Meudon, France European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Santiago 19, Chile 254 Posters Stars & Stellar Systems SSS -3: #61 A Study on the Universality and Linearity of the Leavitt Law in the LMC and SMC Galaxies A. Garcı́a-VarelaB1 ; B. E. Sabogal1 ; M. C. Ramı́rez-Tannus1 The universality and linearity of the Leavitt law are hypotheses commonly adopted in studies of galaxy distances using Cepheid variables as standard candles. In order to test these hypotheses, we obtain slopes of the Leavitt law using linear regressions of fundamental-mode Cepheids observed by the Optical Gravitational Lensing Experiment project in the Magellanic Clouds. We find that the slopes in V I-bands and in the Wesenheit index behave exponentially, indicating non-linearity. We also find that the slopes obtained using long-period Cepheids can be considered as universal in the V I-bands, but not in the Wesenheit index. B 1 [email protected] Universidad de los Andes, Departamento de Fı́sica, Cra. 1E No. 18A-10, Edificio Ip, A.A. 4976, Bogotá, Colombia 255 Stars & Stellar Systems Posters SSS -3: #62 High-frequency quasi-periodic oscillations in X-ray binaries: clues from their amplitude and coherence Claudio GermanàB1 The twin-peak high-frequency quasi-periodic oscillations observed in the power spectra of several Low Mass X-ray Binaries (LMXBs), display central frequencies typical of the orbital motion time-scale close to the compact object. Thus, such modulations could arise from the energy released by accreting clumps of matter interacting with the strong gravitational field of the compact object. HF QPOs are characterized by their central frequency ⌫, root mean square amplitude (rms) and coherence Q = ⌫/ ⌫, where ⌫ is the width of the peak. Here we investigate on the characteristic behavior of both the rms and Q observed in several sources and highlight mechanical proprieties of the accreting material. B 1 [email protected] Departamento de Fı́sica, Universidade Federal do Maranhão, São Luı́s, Brazil 256 Posters Stars & Stellar Systems SSS -3: #63 Rotational Properties of A-Type Stars Monica GrossoB1 ; Hugo Levato1 El objetivo de este trabajo es presentar un analisis estadıstico completo y detallado de la rotacion de la mayor muestra posible de estrellas A del Bright Star Catalogue (BSC) , utilizando mediciones de la rotacion realizadas mediante la aplicación de una tecnica precisa y simple para medir las velocidades de rotacion proyectada habida cuenta de las falencias senaladas en gran parte de la literatura sobre las dificultades para medir vsini (velocidad de rotación proyectada). Para ello se han observado más de 800 estrellas de tipo espectral A mas brillantes que magnitud V=6.5. Se han reducido los datos usando las tecnicas usuales de IRAF y se ha medido el parámetro vsini usando el método DiGoLeG de Dıaz et al.(2011) que hace uso de la Transformada de Fourier del máximo de la Funcion de Correlacion Cruzada para medir vsini. Se amplı́a la muestra con los datos de Royer et al.(2002ab) y se analiza estadı́sticamente la muestra ampliada de 1900 objetos presentando las distribuciones observadas de las velocidades de rotacion axial para las distintas clases de luminosidad y las distribuciones de la velocidad de rotación verdadera V que surge de deconvolucionar la distribucion de vsini. El trabajo presenta datos de la rotacion para 223 estrellas cuyos valores de rotación se desconocı́an previamente. Tambien cabe mencionar que durante la investigación se detectaron 13 binarias espectroscópicas a las cuales se les calculo la rotacion a cada componente. B 1 2 [email protected] Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE) CONICET-UNSJ 257 Stars & Stellar Systems Posters SSS -3: #64 Comparison of optical/near-infrared light-curve properties of the Cepheid Instability Strip pulsating variables Hajdu, G.B1 ; Dékány, I.1 ; Catelan, M.1,2 The ongoing ESO public survey, the Vista Variables in the Vı́a Lactea (VVV) maps about 520 square degrees of the Galactic bulge and the disc in five near-infrared bands. Besides providing us with an unprecedented map of the bulge and the disc, it also conducts a multi-epoch survey in the K band aimed at discovering and characterizing hundreds of thousands of variable stars, many of which belongs to the classical Cepheid Instability Strip classes ( and Type II Cepheids, RR Lyrae stars). For the first time, VVV data will enable us to trace the structure of the spiral arms behind the bulge. This task will be largely depend on the Cepheid variables, but a careful, robust distinction between them and the Type II Cepheids has to be made. Although the period-luminosity relationships of these classes are accurately calibrated, no established classification scheme of variables depending solely on the near-infrared light curves have been published yet. We use a sample of variable stars discovered in the bulge by the optical microlensing surveys (OGLE, MACHO, EROS), common with the VVV survey to systematically compare the optical and K-band light-curve properties of different classes pulsating variable stars. Knowing these parameters allow us to properly classify individual stars (based solely on VVV data), to map the regions of the Galaxy behind the Bulge. We pay special attention to stars pulsating simulatenously in multiple modes (bump and beat Cepheids, RRd stars), as the modeling of pulsations can provide accurate stellar parameters for these variables. B 1 2 [email protected] Instituto de Astrofı́sica, Pontificia Universidad Católica de Chile - Santiago, Chile The Milky Way Millenium Nucleus, Santiago, Chile 258 Posters Stars & Stellar Systems SSS -3: #65 White dwarfs in the Javalambre Physics of the Accelerating Universe Survey A. KanaanB1 ; Navarro, E. A.2 ; Daflon, S.3 ; Pereira, C. B.3 ; Borges, M.3 ; Villegas, T. A.3 ; Gonçalves, D. R. G.4 ; Martins, S. L.4 ; Marcolino, W.4 ; Ribeiro, T.5 ; Ederoclite, A.6 ; JPAS Collaboration White dwarfs are the end state of all main sequence stars less massive than 8M , which means that 98% of all stars will end up as white dwarfs. First and foremost, J-PAS will allow us to discover many new white dwarfs. It will go deeper than SDSS; most of SDSS spectroscopically confirmed white dwarfs have a magnitude below 20.5, while J-PAS will be complete (5 detections) down to 22.5 in each filter. So we should see white dwarfs 2.5 times farther than SDSS and therefore the total volume will be (2.53 - 1 = 14.6 times larger. By definition every object in J-PAS will be spectroscopically observed, while in SDSS only chosen objects had their spectra taken, so our white dwarf sample will also be much more complete than SDSS. We expect to increase the total number of white dwarfs from approximately 20,000 to 300,000. Among our goals are the study of the white dwarf luminosity function and the mass distribution. B 1 2 3 4 5 6 [email protected] Departamento de Fı́sica, Universidade Federal de Santa Catarina Instituto de Astrofı́sica de Andalucı́a Observatórion Nacional, Ministério de Ciência e Tecnologia Observatório do Valongo, Universidade Federal do Rio de Janeiro Universidade Federal de Sergipe Centro de Estudios de Fisica del Cosmos de Aragón 259 Stars & Stellar Systems Posters SSS -3: #66 Line Identification in the Sun’s Spectrum Kitamura, J. R.B1 ; Martins, L. P.1 Synthetic stellar spectra are extensively used for many different applications in astronomy, from determining atomic parameters of new observed stars to the study of the stellar populations of galaxies. One of the inputs for the codes that generate these synthetic spectra are atomic and molecular lines lists, which contain the atomic parameters of the absorption lines that should appear in each spectrum. Although these lists contain million of lines, very few of them were actually measured in laboratory. The consequence is that for many lines the errors in the parameters can be as large as 200%. Besides that, we do not know all the lines that appear in the stars. Even for the Sun, our closest and most studied star, the synthetic spectra misses many lines. This is one of the main reasons we still cannot reproduce the spectrum of observed stars. In this project we will develop a careful strategy to compare the synthetic and observed spectrum of the Sun to try to identify and quantify the lines still missing in the models. We will also try to identify lines with large errors in the atomic parameters, as for example, lines in which the central wavelength is wrong. B 1 [email protected] Universidade Cruzeiro do Sul 260 Posters Stars & Stellar Systems SSS -3: #67 Pre-main sequence evolutionary tracks and isochrones in color-magnitude diagrams Landin, N. R.B1 ; Mendes, L. T. S.2 ; Vaz, L. P. R.3 Evolutionary tracks are widely used to estimate masses of stars. Isochrones are specially used in determining ages of stars in binary systems and in stellar clusters. We present non-gray, pre-main sequence evolutionary tracks and isochrones in theoretical and observational Hertzsprung-Russel diagram for Johnson-Cousins (UBVRI), Johnson-Glass (JHKL) and CTI/CTIO. Theoretical evolutionary tracks from fully convective configuration to a given configuration in main sequence were generated by ATON 2.4 code for a range of masses and chemical compositions. By using color-temperature relations and bolometric corrections available in literature, we converted theoretical pre-main sequence evolutionary tracks and isochrones to their counterparts in color magnitude diagrams. We obtained grids of tracks and isochrones for low-mass stars with different values of metallicity (Fe/H), including the solar one. We present a comparasion between tracks and isochrones in the color-magnitude diagram obtained with different color-temperature relations and bolometric corrections. Finally, we used our new evolutionary tracks and isocrhones in color-magnitude diagram to estimate masses and ages of the pre-main sequence stars of the NGC 2264 young cluster. The resulting mass distribution of the bulk of NGC 2264 population is in the range 0.1-0.6M and the mean age of stars’ cluster is 3.5 Myr, which is in agreement with other works. B 1 2 3 [email protected] Universidade Federal de Viçosa - Campus UFV Florestal Departamento de Fı́sica, Universidade Federal de Minas Gerais Departamento de Engenharia Eletrônica, Universidade Federal de Minas Gerais 261 Stars & Stellar Systems Posters SSS -4: #68 Unveiling optical properties of the high mass X-ray binary XMMU J054134.7-682550 from spectroscopy Lopes de Oliveira, R.B1 ; Placco, V. M.2,3 XMMU J054134.7-682550 is an X-ray source located in the Large Magellanic Cloud. Based on its X-ray properties, and from optical and near-infrared photometry, it was assumed to be a Be/X-ray binary. In this work we present the characterization of its optical counterpart from an optical medium-resolution spectrum acquired with the 3.6-m New Technology Telescope. Photospheric lines along with strong emission lines from the H and several transitions of iron show that the optical counterpart is a Be star with a dense or large circumstellar disk. Thus, it is now conclusive that the system is indeed a Be/X-ray binary. Additionally, we present an ongoing program which aims to improve the characterization of the system from optical and X-ray observations. B 1 2 3 [email protected] Universidade Federal de Sergipe, Brazil NOAO, USA Universidade de São Paulo, Brazil 262 Posters Stars & Stellar Systems SSS -4: #69 In search of precise isochronal ages: Monte Carlo and Bayesian Approach Diego Lorenzo-OliveiraB1 ; Gustavo F. Porto de Mello1 Obtaining accurate ages for FGK stars is important to understand the Galactic structure and evolution as well as the evolution of exoplanetary systems. We build a dense grid of isochrones and evolutionary tracks aimed to identify, in several spectroscopic surveys, which are the most stellar reliable ages based on solid statistics. For this, we calculate their probability distributions of isochronal age and fundamental parameters such as mass, radius, radius (at ZAMS) and surface gravity through Monte Carlo simulations and Bayesian inference. From these determinations, we will be able to derive a sample of MS and subgiant stars with very accurate isochronal ages covering an extensive domain of ages, masses and metallicities. This sample will be very useful for future observational follow-ups and, moreover, when applied to age-activity-rotation relationships will enable the construction of robust age calibrations for solar-type stars. Such calibrations of age and activity might contribute towards the establishment of firmer relations governing the evolution of angular momentum in solar-type stars. B 1 [email protected] Observatório do Valongo, Universidade Federal do Rio de Janeiro 263 Stars & Stellar Systems Posters SSS -4: #70 El Catalogo Bibliografico de Velocidades Radiales Malaroda, S.B1 ; Levato, H.1 ; Galliani, S.1 ; Vega, L.1 Se presenta la ultima version, la numero 24, hasta el 31 de diciembre de 2012, del Catalogo Bibliografico de Velocidades Radiales, iniciado por el grupo en 1991. Se analiza el incremento a lo largo de estos años de los datos observacionales provenientes de grandes contribuciones instrumentales como el RAVE y el BRAVA. El numero de entradas de la presente version supera las 300.000. B 1 [email protected] Instituto de Ciencias Astronomicas, de la Tierra y el Espacio. ICATE-CONICET, San Juan, Argentina 264 Posters Stars & Stellar Systems SSS -4: #71 Atmospheric stratificatfication in NLTE of He and He in the Bp star a Cen 3 4 Maza, Natalia L.B1 ; Nieva, M. Fernanda2,3 ; Levato, Hugo1 Chemically peculiar stars offer unique conditions to investigate difussion processes in stellar atmospheres. The analysis of their spectra is, however, quiet challenging. Such stars present not only several hundred of additional lines in comparison with normal stars due to abundance anomalies. Also, because of diffusion processes, a stratification of the chemical species can affect the stellar atmosperic structucture and the spectral line formation. We have analyzed a high-resolution and high-S/N UVES spectrum of the Bp star a Centauri (He- variable) by means of state-of-the-art non-LTE spectral synthesis. Atmospheric paramteres were determined in an iterative way via ionization equilibria of OI/II and FeII/III and the matching of several Balmer lines simultaneously. Because of chemical stratification and the presence of 3 He, the He lines are not matched with a standard model atmosphere. A new He model atom accounting for the 3 He isotope and an empirically solution for the He stratification in the line-formation calculations allow us to characterise for the first time the He lines of this star in a more realistic manner than do classical models. This non-trivial step is necessary to perform a consistent spectral analysis of trace species, which will be done next. B 1 2 3 [email protected] Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE), San Juan, Argentina Remeis-Sternwarte & ECAP, University of Erlangen-Nuremberg, Germany Institute of Astro- and Particle Physics, University of Innsbruck, Austria 265 Stars & Stellar Systems Posters SSS -4: #72 Stellar models of low-mass, rotating pre-main sequence stars and the effects of an imposed parametric magnetic field Mendes, L. T. S.B1,3 ; Landin, N. R.2,3 ; Vaz, L. P. R.3 Rotating, pre-main sequence stellar models of low-mass stars have been computed with the ATON 2.3 stellar evolutionary code, in which the effects of a large-scale, radially-varying parametric magnetic field are taken in account. Those effects have been modeled according to method proposed by Lydon & Sofia (1995), in which the magnetic field is treated as perturbation that changes the stellar structure equations. Here we report preliminary results on some stellar properties of those models, such as their position in the H-R diagram and the resulting lithium burning. B 1 2 3 [email protected] Departamento de Engenharia Eletrônica, Escola de Engenharia, UFMG, Brazil Departamento de Fı́sica, UFV, Brazil Departamento de Fı́sica, UFMG, Brazil 266 Posters Stars & Stellar Systems SSS -4: #73 Estimating the slope of average rotational axes stars in open cluster Pleiades Dayvid de Sousa MirandaB1,2 ; Bráulio Batista Soares2 ; José Ronaldo Pereira da Silva2 The true rotational velocity of star, V , can be measured from the radius and period of the star. However, determination of the angle of inclination of the rotational axis with the sight line i, is possible only in special cases (eg, star or measured rotation period in binary systems with rotation and translation synchronized). Often, the average equatorial speed, hV i, for a sample of stars is usually estimated by the ratio between the projected average speed, hV sin ii, and the sine of the angle of inclination, hsin ii. The latter is assumed to always equal to ⇡/4 = 0, 79 chance of random distribution of rotational axes irrespective of the particular stellar population or sample. While this procedure has rarely led to discrepancies between theoretical models and the data observations. This work uses the radius star and the period of rotation to determine the equatorial velocity actual best fit with the curve of distribution of velocities equatorial actual procedure by which to determine the index q Tsallis entropy which allows to estimate the average hsin ii based on a sample of radius, rotation periods and projected. This method is used to estimate the average hsin ii of a database containing 217 stars in the Pleiades open cluster, whose rotation periods are available. The result shows an excellent agreement with the observational data. B 1 2 [email protected] Instituto Federal do Maranhão Universidade Estadual do Rio Grande do Norte 267 Stars & Stellar Systems Posters SSS -4: #74 Near-IR Period-Luminosity relations for variable stars in omega Centauri Navarrete, C.B1,2 ; Catelan, M.1,2 ; Alonso-Garcı́a, J.1,2 ; Contreras, R.1,2 ; Dékány, I.1,2 The VISTA Variables in the Vı́a Láctea (VVV) is an ESO public near-infrared variability survey expecting to discover ⇠ 106 new variable sources. In order to perform an automated classification of those sources, welldefined Ks light curves are needed to be used as templates (VVV Templates Project, Catelan et al. 2011). Under this context, omega Centauri is the most suitable globular cluster due to its large amount of known variables. More than 30 hrs of VISTA observations and PSF photometry were used to derive the Ks light curves for ⇠ 300 of known variable stars in omega Centauri (including RRab, RRc, SX Phoenicis, type II Cepheids, Eclipsing Binaries and others) with almost complete phase coverage (more than 100 epochs), in the majority of the cases for the first time in the near-IR. The Period-Luminosity (PL) relation is a remarkable property of pulsating stars. At infrared wavelengths, it has more advantages than the ones derived at visible bands: the interstellar extinction is lower and the infrared luminosities are less sensitive to temperature changes (instability strip is narrower), so PL relations are tighter, with low rms-dispersion. Considering that, PL relations in the near-infrared J and Ks bands were derived for RR Lyrae, type II Cepheids and SX Phoenicis (more than 50 belonging to the cluster) omega Cen variable stars. Each type was analyzed in order to find, if present, different pulsation modes, PL color or metallicity dependence. Our preliminary PL relations for each type, the PL slope behaviour and the possibility to determine the omega Centauri distance modulus will be analyzed. B 1 2 [email protected] Instituto de Astrofı́sica, Facultad de Fı́sica, Pontificia Universidad Católica de Chile, Santiago, Chile The Milky Way Millennium Nucleus, Santiago, Chile 268 Posters Stars & Stellar Systems SSS -4: #75 High-ionization accretion signatures in compact binary candidates from SOAR Telescope observations Oliveira, A. S.B1 ; Rodrigues, C. V.2 ; Cieslinski, D.2 ; Jablonski, F.2 ; Gomes da Silva, K. M.2 ; Almeida, L. A.2 Exploration of transient astrophysical phenomena has been improved by the new generation of synoptic surveys and will soon receive a major impact when large synoptic surveys, like LSST, become available. Meanwhile, the increasing number of surveys made by small robotic telescopes represents a unique opportunity for the discovery of new variable objects and also for the improvement of the samples of many classes of variables. Here we show the results of our work on the search for spectroscopic signatures of high-ionization mass accretion on variable objects of uncertain classification, using spectra obtained in 2012 with the Goodman High Throughput Spectrograph on the SOAR Telescope. Our goal is the discovery of new polars, a subclass of magnetic Cataclysmic Variables (mCVs) with no accretion disk, and Close Binary Supersoft X-ray Sources (CBSS), strong candidates to Type Ia Supernova progenitors. Both are rare objects and probe interesting accretion scenarios. Most of the candidates we observed came from the Catalina Real-Time Transient Survey (CRTS), which incorporates data from 3 wide-field telescopes, in both hemispheres, reaching down to 21 mag. Finding spectral features associated to high-ionization mass accretion, like HeII and inverted Balmer decrement, constrains the CBSS or magnetic CV nature for the candidates, expanding the hitherto small samples of these classes (specially CBSS) and allowing for detailed observational follow-up. B 1 2 [email protected] Univap INPE 269 Stars & Stellar Systems Posters SSS -4: #76 In the wake of ultraviolet sources observed by the Swift satellite Pereira Santos, J.B1 ; Lopes de Oliveira, R.1 ; Luna, G. J. M.2 We present an ongoing project which aims to reveal the nature of the brightest unknown UV sources identified in observations carried out with the Ultraviolet/Optical Telescope onboard Swift. Our sample comprises 60 fields of 17’⇥17’ around symbiotic stars which were the main targets of Swift observations conducted by our group during the past four years. Here we detail the pipeline procedure developed to identify UV sources and search for variability in their flux, and the first results from the five fields already studied. The UV sources identified are likely associated with cataclysmic variables, white dwarfs, and active stars. Additionally, we present the complementary part of this investigation that intends to include optical spectroscopic followup, and mining of X-ray and infrared databases to support the characterization of UV sources. B 1 2 [email protected] Universidade Federal de Sergipe, Brazil IAFE/UBA, Argentina 270 Posters Stars & Stellar Systems SSS -5: #77 Abundance Analysis of CEMP RR Lyrae Stars H. ReggianiB1 ; S. Rossi2 ; C. Kennedy3 ; T. C. Beers4 Among the stellar populations of the Galactic halo are a class of stars known as carbon-enhanced metal-poor (CEMP) stars. These are metal-poor ([Fe/H] < 1.0) stars whose atmospheres exhibit large overabundances of carbon ([C/Fe] +0.7). The frequency of these stars increases with decreasing metallicity, and so by studying their abundance patterns, one can begin to uncover details of the origins of the elements. There exist a number of different classes of CEMP stars (Beers & Christlieb 2005) with specific abundance characteristics; one of them is the CEMP-s class, which exhibit evidence of s-process element enrichment, widely belivied to be resultant of mass transfer from a companion low-metallicity asymptotic giant branch (AGB) star, where the production of carbon and s-process elements occurs. Recent spectroscopic observations of metal-poor RR Lyrae stars have revealed that their typical abundance patterns are consistent with very metal-poor (VMP) and extremely metal-poor (EMP) giants and dwarfs studied in the halo system of the Milky Way. Of particular interest is the recent discovery of a VMP RR Lyrae that has large overabundances of carbon and the s-process elements. In this work, we will show preliminaries results obtained with WiFeS observations 2.3m Siding Spring Observatory telescope of a set of newly-identified CEMP stars that are known RR Ly stars. We seek to confirm classes of these likely CEMP-s stars and, eventually, test their abundances against new stellar evolution simulations of CEMP stars. B 1 2 3 4 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo Research School of Astronomy & Astrophysics, Australian Natinal University National Optical Astronomy Observatory 271 Stars & Stellar Systems Posters SSS -5: #78 Accretion and Activity on the PostCommonEnvelope Binary RR Cae Ribeiro, T.B1,2 ; Baptista, R.3 ; Kafka, S.4 ; Dufour, P.5 ; Gianninas, A.5,6 ; Fontaine, G.5 Context. Current scenarios for the evolution of interacting close binaries – such as Cataclysmic Variables (CVs) – rely mainly on our understanding of low mass stars angular momentum loss (AML) mechanisms. The coupling of stellar wind with its magnetic field i.e., magnetic braking, is the most promising mechanism believed to drive AML in these stars. There are basically two properties thought to drive magnetic braking; stellar magnetic field and wind. Therefore understanding the mechanisms that drives AML requires a compressive understanding of both. Aims. RR Cae is a well known nearby (d = 20pc) eclipsing DA+M binary with an orbital period of P = 7.29h. The system harbors a metal rich cool DA white-dwarf (WD) and a highly active M dwarf locked in synchronous rotation. The metalicity of the WD suggest that wind accretion is taking place, thus providing a good opportunity to obtain the mass loss rate of the M dwarf component. We aim to reach a better understanding of the AML mechanisms in close binaries by characterizing the relevant properties of the M dwarf component of this system. Methods. We analyzed multi-epoch time-resolved high-resolution spectra of RR Cae in search for traces of magnetic activity and accretion. We selected a number of well known chromospheric activity indicators and studied their phase-dependence and long- term behavior. Indirect imaging tomographic techniques were also applied in order to provide the surface brightness distribution of the magnetically active M dwarf. The blue part of the spectrum was modeled using state of the art atmosphere model to constrain the WD properties and its metal enrichment. The latter was used to improve the determination of the mass accretion rate from the M dwarf wind. Results. Doppler imaging of the M dwarf component of RR Cae reveals a polar feature similar to those observed in fast rotating solar-type stars. Analysis of tomographic reconstruction of the H↵ emission line reveals the presence of two components, one traces the motion of the M dwarf and is likely due to chromospheric activity while the other clearly follows the motion of the WD. The presence of metals in the WD spectrum suggests that this component arises from accretion of the M dwarf wind. A model fit to the WD spectrum provides Te↵ = (7260 ± 250)K and log g = (7.8 ± 0.1)dex with a metallicity of < log[X/X ] accretion rate of Ṁacc = (7±2)⇥10–16M · yr B 1 2 3 4 5 6 1 (-2.8 ± 0.1)dex. This maps into a mass onto the surface of the WD. [email protected] SOAR Telescope Universidade Federal de Sergipe Universidade Federal de Santa Catarina Department of Terrestrial Magnetism Département de physique - Université de Montréal C.P. 6128, Succ. Centre-Ville, Montréal, Quebec H3C 3J7, Canada Homer L. Dodge Department of Physics and Astronomy University of Oklahoma, 440 W. Brooks St., Norman, OK, 73019, USA 272 Posters Stars & Stellar Systems SSS -5: #79 High-resolution spectroscopic of red giants stars in NGC 2360 Sales Silva, J. V.B1 ; Pereira, C. B.1 Open clusters can be used to study the disk metallicity distribution and the radial abundance gradient of the Galactic disk because they are among the few objects on the disk where the distances are well determined, making the study of open clusters important to bring us consistent answers regarding the formation and evolution of the two components of the disk (thick and thin disk). Moreover, open clusters are excellent laboratories to test our knowledge of stellar structure and evolution, since the stars present the same age and distance, thus reducing the uncertainties associated with field stars of the Galaxy. NGC 2360 is an open cluster with 0.85 Gyr, with galactocentric distance equal to 9.28 Kpc and height equal to 30 pc (Salaris, et al., 2004). We determine to 16 stars in the NGC 2360 using high resolution spectroscopy the atmospheric parameters and the chemical composition for Fe, Ni, Cr, Ca, Mg, Si, Ti, Na, Al, Ba, Y, Zr, La, Ce and Nd with measures of equivalent widths of absorption lines, and spectral synthesis for C, O and N. The spectra of our stars were obtained with FEROS at the 2.2m ESO telescopes at La Silla (Chile). Atmospheric parameters and abundances were determined using the local thermodynamic equilibrium atmosphere models of Kurucz and the spectral analysis code MOOG. The spectroscopic study of NGC 2360 allowed us to confirm that the binary stars NGC 2360-51 and NGC 2360-52 are belong to NGC 2360 and the discovery of one red straggler star (NGC 2360-96). We also observed a slight overabundance of the elements generated by the s-process in NGC 2360 with respect to field stars of the disk. According Mallorca et al. (2011) the overabundance of the elements generated by the s-process occurs in young open clusters and may be linked to high-efficiency of these nucleosynthesis in low-mass stars (< 1.5M ). However, this high-efficiency has not been explained by the stellar evolutionary models. Additional observations and spectroscopic analysis of intermediate-age open clusters (like NGC 2360) are necessaries to confirm the slight overabundances of s-process elements with relation to field stars of the disk. B 1 [email protected] Observatório Nacional, Rio de janeiro, Brazil 273 Stars & Stellar Systems Posters SSS -5: #80 Mapping of the Physicochemical Conditions of the Planetary Nebula Menzel 1 Santos, P.B1 ; Monteiro, H.1 We prensent a study of the physicochemical conditions of the planetary nebula Menzel 1 using the method of spatially resolved spectrophotometric mapping. The data used in this study were collected in the Cerro Tololo Inter-American Observatory (CTIO) 0.9 m telescope. Observations were made with traditional longslit spectroscopy with exposures taken for multiple parallel positions along the object in order to map it. The separation of the 4” slits were of 4”. Initially, a data cube was created with the spectra obtained for each position of the slit. We used MPFIT - a software package that aims to find parameters that best fit the data to a function - to fit gaussians to the emission lines observed in each pixel of the spatial direction, for each slit in the data cube. We then reconstructed the image of the nebula for each a given emission line extracted from the data cube, interpolating between observed slit positions. With these maps, we obtained the interestelar extition from the H↵/H ratio pixel by pixel. We obtained the density map from the [SII]671.7nm/673.1nm ratio and the temperature map from the [NII](654.8+658.4)nm/575.5nm ratio. Using the code NEAT (Nebular empirical analysis tool), the maps of the chemical abundance were calculated from the flux maps. These maps provide a spatially resolved overview of the physicochemical conditions found in this object. From the maps, we calculated mean values for the main diagnostics, which compared well with values from the literature, showing that we retrieved results from observations without spatial resolution. This method allows the study of planetary nebulae in more detail than conventional methods. B 1 [email protected] Universidade Federal de Itajubá 274 Posters Stars & Stellar Systems SSS -5: #81 Accretion disc mapping of the shortest period eclipsing binary SDSS J0926+36 Wagner SchlindweinB1 ; Raymundo Baptista1 AM CVn stars are ultracompact binaries (Porb < 65 min) where a hidrogen-deficient low-mass, degenerate donor star overfills its Roche lobe and transfers matter to a companion white dwarf via an accretion disc. SDSS J0926+36 is currently the only eclipsing AM CVn star and also the shortest period eclipsing binary known. Its light curve displays deep (⇠ 2 mag) eclipses every 28.3 min, which last for ⇠ 2 min, as well as ⇠ 2 mag amplitude outbursts every ⇠ 100 200 d. Superhumps were seen in its quiescent light curve in some occasions (Copperwheat et al. 2011), probably as a reminiscence of a (in some cases undetected) previous outburst. Its eclipsing nature allows a unique opportunity to disentangle the emission from several different light sources, and to map the surface brightness distribution of its hidrogen-deficient accretion disc with the aid of maximum entropy eclipse mapping techniques. Here we report the eclipse mapping analysis of optical light curves of SDSS J0926+36, collected with the 2.4 m Liverpool Robotic Telescope, covering 20 orbits of the binary over 5 nights of observations between 2012 February and March. The object was in quiescence at all runs. Our data show no evidence of superhumps nor of orbital modulation due to anisotropic emission from a bright spot at disc rim. Accordingly, the average out-of-eclipse flux level is consistent with that of the superhump-subtracted previous light curves. We combined all runs to obtain an orbital light curve of improved S/N. The corresponding eclipse map shows a compact source at disc centre (Tb ' 16000 K) and extended emission (Tb ' 4000 K) along the gas stream trajectory and the disc rim at R ' 0.44 a (a is the orbital separation), suggesting gas stream penetration without bright spot formation. B 1 [email protected] Universidade Federal de Santa Catarina 275 Stars & Stellar Systems Posters SSS -5: #82 Envelopes of Evolved Stars: Galactic and Magellanic Clouds B[e] Supergiants Daiane Breves SeriacopiB1 ; Antonio M. Magalhães1 ; Alex C. Carciofi1 ; Antonio Pereyra2 ; Marcelo Borges2 ; Armando Domiciano de Souza3 ; Francisco Araujo2 ; Jon Bjorkman4 ; Rocı́o Melgarejo Yrupailla1 B[e] Supergiants (B[e]SG) are massive stars with high rotation velocity and a non-spherical circumstellar envelope. This envelope generates a net polarization observed in the light emitted from these objects. Spectropolarimetry is a powerful tool for mapping the structure of the envelope, since emission, absorption and scattering processes are imprinted on the polarized flux. We present preliminary results of spectropolarimetry of Galactic Magellanic B[e]SG obtained with the 4 m Blanco telescope at Cerro Tololo and with the 8.2 m VLT/UT1 telescope at Paranal. For data reduction, we used routines developed by the Polarimetry Group at IAG-USP for the IRAF environment. Results of modeling R82 in the LMC are shown. B 1 2 3 4 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas (IAG/USP) - Brasil Observatório Nacional (ON) - Brasil Université de Nice Sophia (UNICE) - France University of Toledo - USA 276 Posters Stars & Stellar Systems SSS -5: #83 Time-dependent nonextensivity arising from the rotational evolution of solar-type stars Silva, J. R. P.B1 ; Nepomuceno, M. M. F.1 ; Soares, B. B.1 ; de Freitas, D. B.2 The nonextensive formalism is a generalization of the Boltzmann-Gibbs Statistics. In this formalism the entropic index q is a quantity characterizing the degree of nonextensivity, and is interpreted as a parameter of long-memory or long-range interactions between the components of the system. Since its proposition, in 1988, by Tsallis, this formalism has been applied to investigate a wide spectrum of natural phenomena. In stellar astrophysics, theoretical distribution function based on Tsallis nonextensive formalism (q-distributions) has has been successfully applied to reproduce the distribution of V sin ⇠ i data for stars from different stellar populations. In this paper, we investigate the time variation of the entropic index q obtained from the distribution of rotation, V sin ⇠ i, for a sample of 254 rotational data for solar-type star from 10 open clusters aged between 12.9 Myr and 2.6 Gyr. We have found that (1) there is an anti-correlation between the entropic index q and the age of the clusters, and that the distribution of rotation V sin ⇠ i for solar-type stars becomes extensive for an age of about 600 Myr; (2) the distribution of rotation V sin ⇠ i as a function of age is well described by the nonextensive magnetic braking law derived by de Freitas & De Medeiros (2013). Assuming that the parameter q is associated with long-memory effects, we also suggest that the memory of the initial angular momentum of solar-type stars can be scaled by the entropic index q. B 1 2 [email protected] Universidade do Estado do Rio Grande do Norte Universidade Federal do Rio Grande do Norte 277 Stars & Stellar Systems Posters SSS -5: #84 Abundâncias de Zinco em estrelas do bojo Galáctico B1 Silveira, C. R. ; Barbuy, B.1 ; Hill, V.2 ; Zoccali, M.3 ; Minniti, D.3 ; Renzini, A.4 ; Ortolani, S.5 ; Gómez, A.6 ; Dutra, N.1 O Zn é um dos elementos mais pesados da famı́lia do Fe e seu interesse ocorre por duas razões. Primeiro, mostra uma caracterı́stica secundária em estrelas pobres em metal (Cayrel et al. 2004), sendo parcialmente produzido pela adição de nêutrons, e traçar sua abundância ajuda a entender a sua nucleossı́ntese. Segundo, e o mais importante, o Zn é o principal elemento de referência para derivar a metalicidade a partir das linhas de absorção em quasares. Portanto, o estudo de sua abundância como uma função da metalicidade, permite a comparação direta de sua abundância como função da distância e tempo das nuvens presentes entre nós e os quasares. Dispomos de 55 espectros obtidos com o espectrógrafo UVES do VLT, com uma resolução R = 45000, na faixa de comprimento de onda de 480 680nm, que nos permite derivar as abundâncias de Zn das linhas de ZnI em 481.0nm e 636.2nm. Podemos notar que tanto a abundância do zinco ([Zn/Fe]) da nossa amostra como os valores de Reddy et al. (2003, 2006), Nissen et al. (2011) e Cayrel et al. (2004) crescem com metalicidade decrescente, ou seja, de um valor alto em estrelas pobres em metais, chegando ao valor solar em metalicidades maiores. B 1 2 3 4 5 6 [email protected] Universidade de São Paulo, IAG Université de Sophia-Antipolis, Observatoire de la Côte d’Azur Universidad Catolica de Chile, Departmento de Astronomia y Astrofisica Observatorio Astronomico di Padova, Vicolo dell’Observatorio Università di Padova, Dipartimento di Astronomia Observatoire de Paris-Meudon 278 Posters Stars & Stellar Systems SSS -5: #85 An study of v sin i distribution of Be stars Camila Maria SitkoB1 ; Eduardo Janot Pacheco2 ; Marcelo Emilio1 In this work we present the distribution of v sin i of 268 Be’s stars from BeSS (Be Star Spectra) database. We used two tecniques, the Fourier method and the FWHM (Full Fidth at Half Maximum) method and compared our result between the methods and with the literature. For the analysis we made use of three absortion lines of helium, they are 4026Å, 4388Å and 4471Å. We also estimate corrections for turbulance through an minimization technique of our distribution results with the values found at literature. The correction was applied for the values of v sin i not found at the literature. We concluded that the Fourier method give more consistent values of the projected rotational velocities up to 400km/s. B 1 2 3 [email protected] UEL IAG-USP ON 279 Stars & Stellar Systems Posters SSS -6: #86 Theoretical distribution function for rotations of field evolved stars Soares, B. B.B1 ; Silva, J. R. P.1 ; Silva, M. P.1 The present study we compare the different distributions of V sin i, carried out on a large sample for field evolved stars, obtained for different B V intervals with the named q-Maxwellian distribution model. Results show a decreasing trend of the q parameter with increasing color-index B V . Thus, q-Maxwellian appears to be a more suitable instrument to scrutinize the rotational behavior of evolved stars. B 1 [email protected] Department of Physics, State University of Rio Grande do Norte 280 Posters Stars & Stellar Systems SSS -6: #87 Stellar Parameters and Metallicities of a Sample of M dwarfs Hosting Planets Souto, D.B1 ; Cunha, K.1 ; de la Reza, R.1 ; Ghezzi, L.1 ; Smith, V.2 M-dwarfs are an important component in both radial-velocity and transit searches for exoplanets, thanks to the enhanced detectability of small planets due to low stellar masses, low luminosities, and small stellar radii, as well as the fact that they are the most numerous stars in the Galaxy. The determination of stellar parameters and chemical abundances of M-type dwarfs is challenging and remains relatively unexplored. We present results for stellar parameters and metallicities for a sample of planet hosting M-dwarf stars from a spectrum synthesis analysis of high-resolution spectra observed with CRIRES on the VLT between 1.588 and 2.33 microns. B 1 2 [email protected] Observatório Nacional - MCT NOAO/ HQ,US 281 Stars & Stellar Systems Posters SSS -6: #88 SN 2009N: Another Supernova between the Normal and Faint Type II-P SNe Takats, K.B1 Type II supernovae are core-collapse SNe that are classified based on the presence of hydrogen in their spectra. Among them, type II-P SNe represent the most numerous class by far. Those within the subgroup of subluminous II-P events are typified by fainter absolute magnitudes, lower expansion velocities and smaller ejected Ni-mass than the majority of SNe II-P. However, only a couple of SNe falling into the ”gap” between the subluminous and the normal SNe II-P populations have been discovered so far. We present ultraviolet, optical and near-infrared photometric and spectroscopic observations of such object, SN 2009N in NGC 4487. The observed characteristics of SN 2009N (plateau length, spectral evolution, expansion velocity, ejected Ni-mass) are compared to those of subluminous SNe and to those of another intermediate-luminosity object, SN 2008in. We estimate the physical parameters of the progenitor at the explosion (explosion energy, progenitor radius, ejected mass) through hydrodynamical modelling of the main observables and discuss the results. B 1 [email protected] Universidad Andres Bello 282 Posters Stars & Stellar Systems SSS -6: #89 Differential chemical abundances of heavy elements in solar twins Tucci Maia, M.B1 ; Melendez, J.1 In this work we present differential chemical abundances of neutron-capture elements (Z > 30) in solar twins. We have obtained high resolution (R = 60, 000) and high S/N (> 100) spectra of solar twins in the ultraviolet region (310-400nm) with the UVES spectrograph at the VLT/ESO. In the same configuration we also observed that the Sun, that is our reference for the differential analysis, thus obtaining results with high accuracy and precision. In the ultraviolet there is a large number of atomic transitions of heavy elements, which allows the detailed study of the r and s processes. Our sample of solar twins covers a wide range of ages, so it will be possible to study the temporal evolution of the neutron capture elements. B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas (IAG/USP) 283 Stars & Stellar Systems Posters SSS -6: #90 Stellar differential rotation using planetary transits of starspots Adriana ValioB1 When a planet transits its host star, spots and other features on the surface of the host star may be occulted, causing small variations in the star light curve. Detailed analysis of these variations during planetary transits provides a wealth of information about starspot properties such as size, position, temperature (i.e. intensity), and magnetic field. By observing multiple transits, it may be possible to detect the same spot on different transits and thus determine the stellar rotation. Assuming a rotation profile of the star with latitude, for example similar to the Sun, the stellar differential rotation may be estimated. This study is performed using the light curves of known planets detected by the CoRoT and Kepler satellites. Results from the analysis of these lightcurves yields the stellar rotation and differential rotation that are presented here. B 1 [email protected] CRAAM - Mackenzie University 284 Posters Stars & Stellar Systems SSS -6: #91 Infrared accretion disc mapping of the dwarf nova V2051 Ophiuchi in outburst and in quiescence Wojckiewicz, E.B1 ; Baptista, R.1 Dwarf novae are compact binary systems where a late-type star (the secondary) fills its Roche lobe and transfers matter to a companion white dwarf (the primary) via an accretion disc. They show outbursts which recur on timescales of weeks to years, where the accretion disc brightens by factors 20 to 100 either due to a thermal-viscous instability in the disc (DI model) or due to an instability in the secondary which causes a burst of enhanced mass-transfer (MTI model). A DI-driven outburst requires temperatures high enough to < ionize hydrogen Thot > ⇠ 10000K at outburst maximum, and Tcool ⇠ 7000K when the disc is in quiescence, whereas in an MTI-driven outburst there is no temperature constraint. Here we present time-series of fast photometry of the dwarf nova V2051 Oph in the J and H bands, obtained with the CAMIV at the 1.6 m telescope of Observatório Pico dos Dias/Brazil, during the decline of an outburst in 2005 June, and in 2008 when the object was in quiescence. We modelled the ellipsoidal variations caused by the secondary to infer its contribution to the J and H fluxes, and fitted stellar atmosphere models to find a photometric parallatic distance of d = (111± 14)pc. At this short distance, the corresponding disc temperatures in outburst are too cold to be explained by the DI model, underscoring the suggestion of Baptista etal. (2007) that the outbursts of this system are powered by MTI. We also present and discuss J and H eclipse maps tracing the evolution of the disc surface brightness distribution during the decline from the 2005 June outburst. B 1 [email protected] Grupo de Astrofı́sica, Univerisade Federal de Santa Catarina 285 Stars & Stellar Systems Posters SSS -6: #92 VVV Survey search for distant Cepheids in the inner Milky Way Elenna CapoteB1,2 ; Istvan Dékány2 ; Dante Minniti2,3 The VVV Survey has been monitoring the inner disk and bulge of the Milky Way in the near-infrared since 2010. We are building a variability database that would contain a billion point sources in these regions. Using the available data, we have started a search for distant Cepheid variable stars. The multicolor ZYJHKs photometry allows us to estimate the individual reddenings, and the periods yield the intrinsic luminosities, from which accurate distances can be obtained. The main aim of this project is to map the structure of the Milky Way out to longer distances than has been possible before. We report initial results of this search in bulge and disk fields which contain more than two dozen epochs of observations to date. B 1 2 3 [email protected] Massachusetts Institute of Technology Instituto de Astrofisica, Pontificia Universidad Catolica de Chile The Vatican Observatory 286 Posters Stars & Stellar Systems SSS -6: #93 Stelar Activity in stars with planets from CASLEO spectra Flores, M.B1 ; Buccino, A.2 ; Saffe, C.3 ; Mauas, P.4 ; González, F.5 In this work, we study the activity of a sample of stars with planets like nearby Jupiters (0.40<Mp<11 and a<1 UA). We did a study at long-term from the index of Mount Wilson (S). For this, a set of espectra of high resolution was taken and obteined between the years 2002 and 2010 with the spectrograph REOSC of the telescope 2.15 m of CASLEO. In this study, we analyze the stars’ activity at long-term and its dependence with several orbital parameters of the planet. Also, we compare these levels of activity with the asociated at stars of equal type, espectral class and luminosity that don’t have planets. B 1 2 3 [email protected] Institute of Astronomical Sciences, Earth and Space University of Buenos Aires Institute of Astronomy and Space Physics 287 Stars & Stellar Systems Posters SSS -6: #94 Chemical abundances and physical parameters of evolved stars with planets Jofre, E.B1 ; Petrucci, R.2 ; Saker, L.1 ; Artur, E.1 ; Saffe, C.3 ; Gomez, M.1 ; Mauas, P.2 In this contribution we report homogeneous spectroscopic determinations of the effective temperature, surface gravitiy, metallicity, projected rotational velocity and individual abundances for a large sample of evolved stars with planets, as well as for a control sample of evolved stars not known to host planets. Among other empirical relationships between planets and their host stars, we investigate the connection between the chemical abundances of these evolved stars and the presence of giant planets. Implications for the primordial and the self-enrichment hypotheses are also discussed. B 1 2 3 [email protected] Observatorio Astronómico de Córdoba, Argentina Instituto de Astronomı́a y Fı́sica del Espacio, Argentina Instituto de Ciencias Astronómicas, de la Tierra y del Espacio, Argentina 288 Posters Stars & Stellar Systems SSS -7: #95 Modeling Blue Horizontal Branch Stars Santos, R. G.B1 ; Martins, L.1 The stars of the Blue Horizontal Branch (BHB) are characterized by having being through most of their evolutionary process and lost part of their external layers, leaving only a thin layer of hydrogen and a burning Helium nucleus. This makes these stars very blue and hot, although old. They are present in many stellar population systems (e.g. stellar clusters and elliptical galaxies), and their presence can induce errors in the age determination of these objects using integrated spectra. The stellar population analysis technique using integrated spectra is a very powerful tool nowadays, however stellar population models do not account for the BHB stars. Because of that, the presence of these stars induces to the determination of younger ages than expected for these systems. In this project we will create synthetic spectra for the BHB stars that can be incorporated to the stellar population models to be used in spectral synthesis. Here we present an study of the atmospheric parameters of these stars that will be used to create the synthetic spectra. B 1 [email protected] NAT - Universidade Cruzeiro do Sul, Brasil 289 Stars & Stellar Systems Posters SSS -7: #96 An observational overview of the rotation in binary systems Mattiuci, A. C.1 ; Santos, H. B. S.B1 ; Soares, B. B.1 ; Silva, J. R. P.1 Theoretical models of stellar angular momentum evolution predict that the distribution of stellar rotational velocity can be altered by the presence of a binary companion. In the early stages of stellar formation, the binary companion can decrease the time of magnetic star-disk coupling and influence the rate of rotation which the star reaches the main sequence. After the stellar formation, the binary companion can produce tidal torques that alters the angular momentum of the star. As a result, the evolution of the angular momentum of the binary stars are different from the one of the single stars. In this context, the accuracy of the models of stellar angular momentum evolution is constantly increased by comparing it with the observational data. In the last few years, new technologies in the development of new instrumentation, and observational techniques have considerably increased the number of catalogs of stellar rotation. In this work we use rotational data for about 3.000 binary stars from the literature to obtain an overview about the evolution of the stellar rotational velocity in binary systems. We analyze the relationship between rotation and stellar radius, X-ray luminosity, and the synchronization process in different stages of stellar evolution. B 1 [email protected] Universidade do Estado do Rio Grande do Norte 290 Posters Stars & Stellar Systems SSS -7: #97 Mass loss from massive stars Setia Gunawan, D. Y. A.B1 ; Cure, M.2 Massive stars in galaxies transfer huge amount of processed matter and energy into the interstellar medium through their hot, dense and fast stellar wind, and through their often explosive ending. These processed matter and energy in the interstellar medium will in turn influence further star formations. Knowledge about the evolution and characteristic massive stars is therefore crucial in understanding the evolution of galaxies and universe as a whole. The fast dense wind from massive star is line-driven radiatively and is in-homogen/clumped. Models predicted that the clumping is stratified. We will briefly discuss the evidence of inconsistencies of result of massloss rate measurements derived using different diagnostics due to clumping, leading to over-estimation (by up to a factor of ten) of the currently accepted mass-loss rate of massive stars. This is followed by discussion on efforts to constrain the clumping stratification to establish the real mass-loss rates of massive stars. B 1 2 [email protected] ALMA JAO, Chile Universidad de Valparaiso, Chile 291 Stars & Stellar Systems Posters SSS -7: #98 Spectroscopy of the open cluster remnant candidate ESO429-SC02 Angelo, M. S.B1 ; Corradi, W. J. B.1 ; Santos Jr., J. F. C.1 ; Maia, F. F. S.1 In this study we intend to assess conclusively the physical nature of the open cluster remnant (OCR) candidate ESO429-SC02. In a previous work, the method of characterization devised by Pavani & Bica (2007) failed to characterize the object as an OCR or as an asterism, classifying it as a possible OCR. To perform our anal0 ysis, we carried out multi-object spectroscopy of 31 stars in its inner area (r < ⇠ 4 ) using GMOS/GEMINI-S (resolution R ⇡ 2000). We have cross-correlated (IRAF’s FXCOR task) our science spectra with 1962 templates from ELODIE library and obtained heliocentric radial velocities, spectral types and metallicities. In our research, we have employed 2MASS JHKs photometric data and retrieved proper motions from UCAC4. We have derived individual distances via spectroscopic parallax and reddening values for our science stars. In a star-by-star analysis we used the dispersion of the derived parameters as a measure of the star’s physical connection. Preliminary results indicate that five stars are at approximately the same distance from the Sun (hdi = 1.81 ± 0.05 kpc (s.d.)), have nearly solar metallicities (h [Fe/H]i = 0.039 ± 0.064) and quite consistent heliocentric radial velocities (hVr i = 21.9 ± 9.6 km/s), although only three of them share common proper motions (hµ↵ cos i = 0.77± 1.4 mas/yr; hµ i = 2.1 ± 2.5 mas/yr). Three other bright stars (J < 12.m 4) present in ESO429-SC02 central field, but without observed spectrum, have proper motions components values similar to these mean ones and, together with the other five candidate member stars identified, they possibly form a coeval aggregate well fitted by a log (t/yr) = 8.8, Z = Z Padova isochrone (Bressan et al. 2012) with (m M )0 = 11.m 2 and E(B V ) ⇡ 0.m 1. Our nest step will be to cross-correlate our spectra with synthetic spectra libraries in order to cover ELODIE’s “gaps”, in parameters space, specially in metallicity. This way we aim to better constrain the list of probable members of ESO429-SC02. B 1 [email protected] ICEx/Physics Department, Universidade Federal de Minas Gerais 292 Posters Stars & Stellar Systems SSS -7: #99 Collisions between Globular Clusters Belloni, D. T.B1 ; Rocha-Pinto, H. J.2 The study of globular clusters plays an important role on our understanding of the Universe since these systems are true laboratories for theories of stellar dynamics and evolution. Although the common, traditional astronomical knowledge about these systems picture them as homogeneous polytropes, made of single stellar populations, the detailed photometrical study and chemical tagging of their constituent stars suggest that some are far from being homogeneous systems. The discrepancies from the canonical picture include double (or even triple) main sequences and/or red giant branches, larger than expected internal chemical abundance scatter and unusual horizontal branch showing simultaneously extremely blue and red stars. Some of these non-canonical clusters are now being seen as remmants of the nuclei of former satellite galaxies of the Milky Way. A similar awkward extragallactic globular cluster (Scl-dE1 GC1) in the Sculptor Group dwarf elliptical galaxy Scl-dE1 (Sc22), studied by Da Costa et al. has a half-light radius of 21.8 pc, an absolute magnitude of MV = 6.7 and the cluster stellar population appears indistinguishable from that of the parent galaxy. Da Costa et. al suggest that this object might have formed through the merging of star clusters. This scenario for the formation of Scl-dE1 GC1 was succesfully reproduced by Assmann et al. with a particle-mesh code. Since the globular cluster configuration correspond to a relatively small, relaxed gassfree stellar system supported by velocity dispersion, it is likely that a number of different objects, by means of their formation path, could end up as globular-like systems, including some globulars formed by early collisions of other globulars. We here study the outcomes of collisions between globular clusters under the gravitational influence of a larger disk galaxy. We use the NBODY6 direct N -body code by Aarseth to check under which conditions a close encounter of two globulars could disrupt them or lead to a merged, larger globular. We check whether merged globulars have a peculiar luminosity profile right after the merger and how much time it takes for a new relaxation. B 1 2 [email protected] Valongo Observatory, Federal University of Rio de Janeiro Valongo Observatory, Federal University of Rio de Janeiro 293 Stars & Stellar Systems Posters SSS -7: #100 Study of clustering in the stellar abundances space Boesso, R.B1 ; Rocha-Pinto, H. J.1,2 The study of the stellar populations provides us with an understanding of the origin and evolution of the Milky Way. The chemo-evolutionary history of the Galaxy is still preserved in the stellar abundance distributions. Since stars are formed from the interstellar medium and inherit these chemical abundances, it is expected that the stars we observe today can be classified in chemical groups, in an analogous way to the classification of biological species. The aim of this study is to find structures in the stellar abundances space, obtaining stellar groups that had a similar chemo-evolutionary history, through the use of tree clustering technique. We built tree classifications for large and classic abundance surveys in the literature: Edvardsson et al. (1993); Fulbright (2000); Gratton et al. (2003a); Reddy et al. (2003); Reddy et al. (2006); Takeda et al. (2008); Neves et al. (2009); Adibekyan et al. (2012). In this technique, the data are grouped hierarchically, so that initially the number of clusters is identical to the number of observations and, by recursive clustering of data by similarity, the number of clusters progressivelly decreases. This method allows us to analyze large samples of stars and to obtain information about the enrichment history of the Galaxy. In this study we also made use of a second tool, the PCA (Principal Component Analysis) method, and we apply this tool to stellar abundances to analyze the history of star formation and the main processes of nucleosynthesis. B 1 2 [email protected] Observatório do Valongo, Universidade Federal do Rio de Janeiro LIneA, Laboratório Interinstitucional de e-Astronomia 294 Posters Stars & Stellar Systems SSS -7: #101 Old open clusters in the VVV Survey Borissova, J.B1 ; et al. We will report the discovery and analysis of new old infrared open cluster candidates projected in the bulge area covered by VISTA Variables in the Via Lactea (VVV) ESO Large Public Survey. For relatively well populated cluster candidates we derived the fundamental parameters such as reddening, distance and age by fitting the solar-metallicity Padova isochrones on the color-magnitude diagrams and spectroscopic parallaxes. Some important existing distributions such as distance of the cluster to the galactic center vs. age distribution, open clusters age histogram, distance of the open clusters to the Sun vs. reddening, etc. are complemented with the new sample and re-derived. B 1 [email protected] Universidad de Valparaiso, Chile 295 Stars & Stellar Systems Posters SSS -7: #102 Phase Mixing in Popping Star Clusters Candlish G. N.B1 ; Smith R.1 ; Fellhauer M.1 ; Gibson B. K.2 ; Kroupa P.3 ; Assmann P.1 As star clusters are expected to form with low star formation efficiencies, the gas in the cluster is expelled quickly and early in their development: the star cluster “pops.” This leads to an unbound stellar system. Previous N-body simulations have demonstrated the existence of a stepped number density distribution of cluster stars after popping, both in vertical position and vertical velocity, with a passing resemblance to a Christmas tree. Using numerical and analytical methods, we investigate the source of this structure, which arises due to the phase mixing of the out-of-equilibrium stellar system as it evolves in a background analytical potential. Considering only the vertical motions, we construct a theoretical model to describe the time evolution of the phase space distribution of stars in a Miyamoto-Nagai disk potential and a full Milky-Way type potential comprising bulge, halo and disk components, which is then compared with Nbody simulations. Using our theoretical model, we investigate the possible observational signatures and the feasibility of detection. B 1 2 3 [email protected] Departamento de Astronomia, Universidad de Concepción, Chile Jeremiah Horrocks Institute, University of Central Lancashire, Preston, UK Argalander Institut fur Astronomie, Universitat Bonn, Bonn, Germany 296 Posters Stars & Stellar Systems SSS -7: #103 Checking the consistency of physical parameters of open clusters: the case of NGC188 and M67 de Souza, C. C.B1 ; Kerber, L. O.1 Open cluster are fundamental pieces to calibrate the stellar evolutionary models, especially in the regime of solar metallicity. Despite the large number of determinations of physical parameters for open clusters, there is a lack of consistency tests to check these results. In this work we investigate this consistency in two classical open clusters: NGC 188 and M 67. It is done by means of isochrones fitting in multiband colour-magnitude diagrams, from optical (BVI) to the near-infrared (JHK). For this purpose we apply a numerical-statistical method based on the likelihood statistics to find the best solutions. Our results point to the existence of a sensitive dependence on the values of age, distance, reddening and metallicity depending on the choice of wavebands as well as the adopted stellar evolutionary models. In particular we find differences in age that can exceed 40%, even comparing results for the optical bands. B 1 [email protected] Universidade Estadual de Santa Cruz 297 Stars & Stellar Systems Posters SSS -8: #104 Proper motion determination of the optically visible open clusters based on the UCAC4 catalogue Dias, W. S.B1 ; Monteiro, H.1 ; Caetano, T. C.1,2 ; Lepine, J.2 ; Assafin, M.3 We present a catalog of mean proper motion and membership probability of individual stars for optically visible open clusters determined using the data from the UCAC4 Catalogue in a homogeneous way. The mean proper motion of the cluster and the membership probabilities of the stars in the region of each cluster were determined by applying the statistical method of Uribe & Brieva (1994) in a modified fashion. In this study, we applied a new technique based on the Cross-Entropy global optimization procedure to fit the observed distribution of proper motions with two overlapping normal bivariate frequency functions, inclusively considering the individual proper motion’s errors. For 724 clusters, this is the first determination of proper motion and for all we present results with a much larger number of identified astrometric member stars. B 1 2 3 [email protected] IFQ, UNIFEI IAG, USP OV, UFRJ 298 Posters Stars & Stellar Systems SSS -8: #105 An psf-fitting pipeline for VVV-ESO: The star cluster Pismis 24 R. A. DiasB1 This work presents a DAOPHOT-based pipeline to perform PSF-fitting pho-tometry of “VISTA Variables in the Via Láctea” (VVV) ESO Public Survey data.The main feature of the pipeline is to avoid user interaction keeping photometric accuracy and deepth, in fact it reached accurate photometry for the faintest stars (J, H, K) and reliable photometry to stars more than one magnitude fainter than the detectable in other techniques. Although getting less accurate data for the brightest stars, the pipeline proved to be the most appropriated approach, since we aim to work with young open clusters, where the pre-main sequence is of major relevance. Moreover, we can apply 2MASS/VVV matching to replace the VVV’s saturated stars. B 1 [email protected] Universidade Federal do Rio Grande do Sul - UFRGS 299 Stars & Stellar Systems Posters SSS -8: #106 Proper motions of pre-main sequence stars B1 Ferreira, A. C. S. ; Teixeira, R.1 ; Ducourant, C.2 ; Galli, P. A. B.1 ; Le Campion, J. F.2 ; Fidêncio, M.1 The kinematic study of young stars is an important tool to discuss the early stages of star formation. In this context, proper motions allow us to detect moving group structures of young stars to which they belong. Individual distances to moving group members can be inferred from proper motion and radial velocity data using the convergent point strategy. The main objective of this work is to determine proper motions of premain sequence stars in nearby star-forming regions. This work represents an improvement of an existing database by including more pre-main sequence and refining the astrometry for stars with poor proper motion information in the literature. We calculate the stellar proper motions from observations performed with the CCD meridian circles located at the Abrahão de Moraes Observatory (Valinhos, SP) and the Bordeaux Observatory, and also use data from the literature. Here we discuss the accuracy of our results and compare with published astrometric catalogs. B 1 2 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo, Brasil Observatoire de Bordeaux, France 300 Posters Stars & Stellar Systems SSS -8: #107 The nature of X-ray sources associated to young clusters around Sh2-296 Gregorio-Hetem, J.B1 ; Fernandes, B.1,2 ; Montmerle, T.2 Aiming to unravel the star formation activity in the Canis Major R1 (CMaR1) star-forming Galactic region, we have studied the young (< 5 Myr) clusters associated to the arc-shaped ionized nebula Sh2-296. Based on our X-ray data complemented by optical and near-IR data, we discovered, near to GU CMa, a stellar cluster that is older by at least a few Myr than the previously known cluster, around Z CMa, where star formation is still very active. We suggest that the CMa R1 region has undergone at least two distinct star formation episodes. Multi-object optical spectroscopy of our X-ray sources nearby Z CMa and GU CMa has been performed with Gemini telescopes to confirm the existence of a mixed population from both older and younger clusters around the edge of Sh2-296. In the present work we show the results obtained for the stellar clusters located to the East of Z CMa, where we acquired spectra for optical counterparts candidates of 45 X-ray sources. Spectral-type determination was based on comparison with standard spectra library for late-type stars and fitting the continuum and TiO bands. Most of our sample is low-mass young stars, having K7 to M0 spectral types. Typical features of young stars were inspected to confirm the nature of the sample that is mainly classified as T Tauri stars (TTs), since their spectra show the Li I (670,8 nm) line, one of the indicators of youth. The equivalent width of H↵ measured at 10% of the total flux was used to separate Classical TTs (CTTs) from weak-line TTs (WTTs). Among 51 optical counterparts candidates, 38 are young stars: 24% of them are classified as CTTs and 76% are WTTs or post-TTs. One object is classified as Herbig Be star and 9 are emission-line stars, which nature remains to be revealed. The few number of CTTs among our sample is consistent with the mixing of populations that we discovered previously. However the present results correspond to a small fraction (⇠15%) of the entire sample of X-ray sources we have detected with XMM-Newton around Sh2-296. In order to have a more representative set of spectra, additional GMOS observations have been performed. Another ongoing project (see Santos-Silva et al.) is dedicated to study the relation of the X-ray properties of our sample compared to the optical spectral classification obtained in the present work. B 1 2 [email protected] Universidade de São Paulo, IAG Institut d’Astrophysique de Paris 301 Stars & Stellar Systems Posters SSS -8: #108 Stellar parameters and metallicity in Orion Association F and G stars Rafael Fraga GuerçoB1 The chemical abundance distribution in the young associations of the Milky Way are important in understanding the chemical evolution of the Galaxy and how it formed and evolved. In particular, the chemical abundances of young stars in association are important to define the present day abundance and address cosmic scatter. B 1 [email protected] Observatório Nacional 302 Posters Stars & Stellar Systems SSS -8: #109 Using MASSCLEAN to Describe Stellar Clusters Found in the Vista Variables in the Via Lactea (VVV) Survey Bogdan Popescu1 ; M. M. HansonB1 ; J. Borissova2 ; R. Kurtev2 ; V. D. Ivanov3 ; M. Catelan4 ; S. S. Larsen5 ; D. Minniti4 ; P. Lucas6 The important parameters of age, mass and distance of resolved or partially resolved stellar clusters are most accurately determined by using color-magnitude diagrams (CMD). However, when the main sequence turnoff is not available or clearly identifiable, large errors in all parameters result when using simple isochrone fitting, particularly when observations are limited to near-infrared bands. We used the MASSCLEAN package to perform 5 million Monte Carlo simulations of stochastically sampled stellar clusters in order to generate CMD templates for a variety of cluster masses and ages and which mimic the observational photometric errors. This results in the creation of tens of thousands of n-dimensional stellar density maps (templates) in numerous color planes as a function of age and mass. We use these MASSCLEAN CMD templates to refine and sharpen traditional isochrone fitting to analyze the newly discovered stellar clusters/cluster candidates from the Vista Variables in the Via Lactea (VVV) Survey. Our MASSCLEAN templates are also being used to design and optimize search algorithms for stellar clusters in broad-band surveys. B 1 2 3 4 5 6 [email protected] University of Cincinnati, USA Universidad de Valparaiso, Chile ESO, Santiago, Chile Pontificia Universidad Catolica, Santiago, Chile Radboud Universiteit Nijmegen, The Netherlands University of Hertfordshire, UK 303 Stars & Stellar Systems Posters SSS -8: #110 NIP of Stars: early results and new eclipsing binaries B1 Jaque Arancibia, M. ; Barba, R. H.2 ; Morrell, N.3 ; Roman Lopes, A.2 ; Torres Robledo, S.2 ; Gunthardt, G.4 ; Soto, M.5 ; Ferrero, G.6 ; Arias, J.2 ; Gamen, R. 7 ; Fernadez Lajus, E.7 We have performed a near-infrared photometric monitoring of 39 galactic youngstar clusters and star-forming regions, known as NIP of Stars, between the years 2009–2011, using the Swope telescope at Las Campanas Observatory (Chile) and the RetroCam camera, in H- and Y-bands. This monitoring program is complementary to the Vista Variables in the Vı́a Láctea (VVV), as the brightest sources observed in NIP of Stars are saturated in VVV. The objective of this campaign is to perform a census of photometric variability of such clusters and star-forming regions, with the main goal of discovering massive eclipsing binary stars.In this work, we present a preliminary analysis of this photometric monitoring program with the discovery of tens of candidates for variable stars, among which include candidates for massive eclipsing binaries. We included also to the analysis of variability, a small set of images obtained in the Ks with the VISTA telescope in the framework of VVV survey (Minniti et al. 2010). In special, we announce the infrared discovering of four massive eclipsing binaries in the massive young cluster NGC 3603. The stars have been classified spectroscopically as O-type stars, and one of them, MTT 58, has a rare star with a spectral type of O2 If*/WN6, as one of its components. We present a preliminary analysis of the light-curves of these binaries. B 1 2 3 4 5 6 7 [email protected] ICATE-CONICET, Argentina Universidad de La Serena, Chile Las Campanas Observatory, Chile Observatorio de Cordoba, Argentina STScI, USA FCAGLP, Universidad Nacional de la Plata, Argentina IALP-CONICET, Argentina 304 Posters Stars & Stellar Systems SSS -8: #111 Mass segregation for the young star clusters Jincheng Y. U.B1 Mass segregation of the young star cluster is one of the dynamical properties which is an important tool to investigate the star forming process and dynamical evolution of star clusters. The origin of this mass segregation has been suggested as either “primordial”, that is, it is a result of the star formation process in which stars form mass segregated from their parent molecular cloud, or dynamical, i.e., resulting from fast dynamical evolution. Recent N-body simulations suggest initially dynamically cool and sub-structured star clusters can be mass segregated within very short timescale. However, the effects of different initial conditions are still not well understood. Therefore, we investigate the influence of different initial parameters to further constrain our theoretical model for young-mass segregated star clusters. In particular, we focus on the correlation between the morphology and the degree of mass segregation of the early evolution of young star clusters. B 1 [email protected] Institute of Astrophysics, Pontificia Universidad Catolica de Chile 305 Stars & Stellar Systems Posters SSS -8: #112 Present-day Mass Function of Four LMC Star Clusters with Multiple Stellar Populations Luque, E. F.B1 ; Kerber, L. O.1 We determined the present-day mass functions (PDMFs) of four intermediate-age clusters NGC 1751, NGC 1783 NGC 1806 and NGC 1846 in the Large Magellanic Cloud (LMC) based on observations with HST/ACS. These clusters present a remarkable feature in their colour-magnitude diagrams: an extend Main Sequence Turn-Off, which is commonly interpreted as a signature of multiple stellar population with differences in age of about a few Myr. The global PDMFs for all clusters are well fitted by power-laws with exponent similar to the Salpeter one ( = 1.35) ranging from = 1.28 ± 0.19 (NGC 1846) to = 1.62 ± 0.23 (NGC 1783). Our preliminary radial analysis indicates that all systems present some evidence of mass segregation, but at different degrees. B 1 [email protected] Universidade Estadual de Santa Cruz 306 Posters Stars & Stellar Systems SSS -9: #113 Photometric analisys of Galactic Stellar Clusters in VVV Survey Mauro, F.B1 ; Moni Bidin, C.2 ; Cohen, R.1 ; Geisler, D.1 ; Villanova, S.1 ; Chené, A.-N.3 We’ll show the results of the photometric analysis of several interesting Galactic star clusters (known, new and candidate) in the “VISTA Variables in the Via Lactea” (VVV) Survey, one of the six ESO Public Surveys operating on the new 4-meter Visible and Infrared Survey Telescope for Astronomy (VISTA). VVV is scanning the Milky Way bulge and an adjacent section of the disk, where absorption is high, making difficult the observations in the visible. The data are obtained with the new automatic VVV-SkZ pipeline photometric pipeline, that permits to have photometry more accurate and with a wider range of magnitudes respect to other techniques (generally from Ks=9-10 to 18) to study the parameters of the star clusters. B 1 2 3 [email protected] Universidad de Concepcion Universidad Catolica del Norte Gemini Observatory 307 Stars & Stellar Systems Posters SSS -9: #114 The local dark matter density Moni Bidin, C.B1 ”Weighting” the Galactic disk by means of the kinematics and spatial distribution of its stars is a classical method of measuring the gravitational mass enclosed in a given volume. Unfortunately, the huge information required for this measurements has so far limited all the investigations to a one-dimensional approximation within 1 kpc from the Galactic plane. Applying a fully three-dimensional formulation to three kinematical data sets from the literature, extending up to 4 kpc from the plane, we found a surprising lack of dark matter at the solar position, at variance with previous measurements and with the expectations of the most accepted dark matter halo models (Moni Bidin et al. 2012, ApJ, 751, 30). Bovy & Tremaine (2012, ApJ, 756, 89) later defied those results, but we recently demonstrated (Moni Bidin et al. 2013, ApJ, submitted) that their criticism is not a viable explanation of our puzzling results. In this contribution, we will show our most recent advances in our ongoing studies, based on both synthetic data and an extended SDSS sample of more than 13000 stars, aimed to understand the origin of the unexpected lack of dark matter previously found. B 1 [email protected] Universidad Catolica del Norte, Antofagasta, Chile 308 Posters Stars & Stellar Systems SSS -9: #115 The Origin and Chemical Evolution of the Exotic Globular Cluster NGC 3201 Muñoz, C.B1 ; Geisler, D.1 ; Villanova, S.1 NGC 3201 is a globular cluster (GC) which shows very peculiar kinematic characteristics including an extreme radial velocity and a highly retrograde orbit, strongly suggesting an extragalactic origin. Our aims are to study NGC 3201 in the context of multiple populations (MPs), hoping to constrain possible candidates for the self-enrichment by studying the chemical abundance pattern, as well as adding insight into the origin of this intriguing cluster. We present a detailed chemical abundance analysis of eight red giant branch stars using high-resolution spectroscopy. We measured 29 elements and found [Fe/H] = -1.53±0.01; we cannot rule out a metallicity spread of ⇠0.12 dex, and an ↵-enhancement typical of halo GCs. However, significant spreads are observed in the abundances of all light elements except for Mg. We confirm the presence of an extended Na-O anticorrelation. n-capture elements generally are dominated by the r-process, in good agreement with the bulk of Galactic GCs. The total (C+N+O) abundance is slightly supersolar and requires a small downward correction to the isochrone age, yielding 11.4 Gyr. Kinematically, NGC 3201 appears likely to have had an extragalactic origin but its chemical evolution is similar to most other, presumably native, Galactic GCs. B 1 [email protected] Universidad de Concepción. Chile. 309 Stars & Stellar Systems Posters SSS -9: #116 Detección de cúmulos abiertos en regiones extensas del cielo usando parámetros astrométricos Paı́z, L. G.B1 ; De Biasi, M. S.1,2 ; Orellana, R. B.1,2 Se desarrolló un método no paramétrico para identificar cúmulos abiertos en regiones extensas del cielo utilizando datos precisos de posición y movimiento propio estelar. Se establecieron dos códigos binarios a partir del análisis de las funciones empı́ricas de densidad de probabilidad en posición y en movimiento propio, luego de eliminar la contaminación producida por las estrellas de campo en la región estudiada. Estos códigos definen para cada estrella un parámetro que indica la pertenencia de la misma a una zona de sobredensidad espacial y sobredensidad en movimiento propio. Se probó la validez del método aplicándolo a la región comprendida entre 7h 8m  ↵  7h 28m y - 33   -29 , que contiene a los cúmulos abiertos Collinder 140 y Collinder 132. Los datos utilizados fueron obtenidos del catálogo astrométrico UCAC4 hasta magnitud R=11 para asegurar pequeños errores en movimientos propios. Se detectaron 6 sobredensidades espaciales, de las cuales un nuevo análisis mostró que 3 podrı́an ser cúmulos abiertos. Se calcularon las coordenadas medias (¯ ↵, ¯), radio r y componentes medias de movimiento propio (µ̄↵ cos ¯, µ̄ ) de los 3 candidatos. Uno de ellos es Collinder140, y sus parámetros obtenidos (¯ ↵, ¯)=(110.8 , -32.0 ); r ⇡ 12’; (µ̄↵ cos ¯, µ̄ )=(-3 mas/año, +3 mas/año) muestran un buen acuerdo con la literatura consultada (Kharchenko et al. 2005, De Biasi & Orellana 2008). Los otros dos posibles cúmulos, con estrellas en su mayor parte de magnitud más débil que 10.0, no se encuentran en la literatura. Collinder132 no pudo ser detectado debido a que no tiene suficientes miembros brillantes (Orellana et al. 2010). B 1 2 [email protected] Facultad de Ciencias Astronómicas y Geofı́sicas, UNLP Instituto de Astrofı́sica de La Plata (CCT La Plata – CONICET) 310 Posters Stars & Stellar Systems SSS -9: #117 Galactic Embedded Clusters with 2MASS infrared photometry Pavani, D. B.B1 ; De Araújo, P. P.; Bica, E.; Bonatto, C. Star clusters and associations are born in general embedded within giant molecular clouds (GMCs). Because of this, during their formation and early evolution they are often only visible at infrared wavelengths, being heavily obscured by dust. Studies have indicated that less 5% of embedded clusters survive beyond the first million years to become opens clusters. In this work we employed the Two Micron All Sky Survey (2MASS) photometry to analyze, for the first time, 10 Galactic embedded clusters. We investigated the nature and derived fundamental parameters for the clusters by applying a field-star decontamination algorithm developed by our group. The method has been systematically used in our publications and have shown how the effective it is. As a result, this research will bring new information about the history of formation and evolution of the system of embedded and open clusters and their connection with the properties of the Galactic disk. B 1 [email protected] Department of Astronomy, Institute of Physics, Federal University of Rio Grande do Sul/UFRGS 311 Stars & Stellar Systems Posters SSS -9: #118 Probing accretion on the high-magnetized polar RX J1007.5-2017 Rodrigues, C. V.B1 ; Cieslinski, D.1 ; Ribeiro, T.2 ; Silva, K. M. G.1 ; Baptista, R.3 ; de Oliveira, A. S.4 ; Costa, J. E. R.1 ; Campbell, R.5 RX J1007.5-2017 is a polar: a compact binary system in which matter flows from a low-mass main-sequence star to a magnetized white dwarf without the formation of an accretion disk. RX J1007.5-2017 has some observational peculiarities: conspicuous optical cyclotron harmonics; a very soft X-ray spectrum; and no polarization in R and I bands. These characteristics may be related to extreme conditions at the accretion flow: a very strong white-dwarf magnetic field (around 100 MG on surface) and a low accretion rate. To study the accretion, from the secondary to the white dwarf, we obtained time-resolved spectroscopy using the Goodman spectrograph at the SOAR telescope in observing runs distributed around the first semester of 2012. We found the object in different brightness states. In the low state, we gathered data with two spectral resolutions (219 km/s and 170 km/s). In a brighter state, the spectral resolution was approximately 170km/s. The low (high) spectral resolution data cover the spectral region from 360 to 760 nm (435 to 700 nm). The continuum varies in both states and the cyclotron humps are visible in some orbital phases. The orbital dependence of the cyclotron emission were modelled using the Cyclops code, which adopts a 3D representation of the accretion column. In the low state, the secondary spectral features are seen as well as the Balmer emission lines. The spectra in the bright state show Balmer, HeI, and HeII emission lines. The Balmer and HeII lines components could be separated: in bright state the lines are broader and have three components. In the low state, the lines are narrower and two components are distinguished in some phases. These data were analyzed using Doppler tomography. This enables to study the origin of components and their changes as a function of the brightness state of the object. B 1 2 3 4 5 [email protected] Instituto Nacional de Pesquisas Espaciais, Brazil Universidade Federal de Sergipe, Brazil Universidade Federal de Santa Catarina, Brazil Universidade do Vale do Paraı́ba, Brazil Humboldt State University, USA 312 Posters Stars & Stellar Systems SSS -9: #119 Discriminating Local Group embedded star clusters from older ones using near-IR photometric indexes Santos Jr., J. F. C.B1 ; Dottori, H.2 ; Grosbol, P.3 Several grand-design spiral galaxies show a bimodal distribution of their system of star clusters and star forming complexes in JHK diagrams. In a comparison with stellar population models, the (J H) vs (H Ks) diagram revealed that embedded clusters, still immersed in their parental clouds of gas and dust, have in general a redder (H Ks) colour than older clusters, whose gas and dust have already been ejected. This bimodal behavior is also evident in the CMD MK vs (J Ks ), where the brightest clusters split into two sequences separating younger from older clusters. In addition, the reddening-free index Qd = (H 0.884 (J Ks ) - H) was shown to correlate with age for the young clusters and thus provided an effective way to differentiate the embedded clusters from the older ones. In the present work, the aforementioned photometric indices were explored for star cluster systems in the Local Group. In particular, we investigate the effectiveness of the Qd index in sorting out clusters of different ages at their early evolutionary stages. Surface photometry on 2MASS images was carried out for populous clusters younger than approximately 100 Myr and whose ages are available. The integrated magnitudes and colors extracted from the surface photometry of the most populous clusters/complexes in the Local Group showed the same bimodal distribution in JHK diagrams as that found for more distant galaxies, suggesting that the phenomenum is universal. In particular, we confirm the index Qd as a powerful tool to distinguish clusters younger than about 7 Myr from older clusters. B 1 2 3 [email protected] Universidade Federal de Minas Gerais Universidade Federal do Rio Grande do Sul European Southern Observatory 313 Stars & Stellar Systems Posters SSS -9: #120 ALS 2883: Analysis of spectroscopic features Silva, A. R.B1 ; Levenhagen, R. S.1 ; Künzel, R.2 ; Leister, N. V.3 Be stars are by definition objects that show or have shown, at least once in its living time, emission in their Balmer lines. ALS 2883 is a well-known Be-Pulsar system with all its spectroscopic features in emission, without any direct signature from its photosphere. This emission is a common hallmark among many Be stars, and this effect is thought to be due to the presence of a circumstellar environment. Also, the presence of X-ray emissions in this system is nowadays well established, which is often attributed to the presence of an orbiting compact object. In this study, we present the observations in the visible range of ALS 2883, performed at MCT/LNA in April 2011. In order to derive fundamental physical parameters and chemical abundances of the Be star, we solved the radiative transfer equation. B 1 2 3 [email protected] UNIFESP IF-USP IAG-USP 314 Posters Stars & Stellar Systems SSS -9: #121 Revisiting TW Hydrae in light of new astrometric data B1 Teixeira, R. ; Ducourant, C.2 ; Galli, P. A. B.1 ; Le Campion, J. F.2 ; Zuckerman, B.3 ; Krone-Martins, A. G. O.4 ; Chauvin, G.5 ; Song, I.6 TW Hydrae is a very important and interesting target to study star and planet formation due to its youth and proximity. Nevertheless, it is remarkable the lack of good observational data making the determination of individual stellar parameters and the membership status for many association members more difficult. In our work we have measured the proper motion and trigonometric parallax for 15 possible members of TWA Hydrae that associated to those astrometric, photometric and spectroscopic data from the literature allow us to refine and improve the previous description and understanding of this association. In this work we identify a core moving group of 25 stars using our new and improved convergent point search method, and then derive the dynamical age of the association by applying a traceback technique. We compare the dynamical age of the association with the age estimate as derived from theoretical evolutionary models and discuss the properties of individual stars. B 1 2 3 4 5 6 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, USP Observatoire de Bordeaux, Université de Bordeaux, LAB Department of Physics & Astronomy, UCLA Departamento de Fı́sica, Fac. Ciências da Universidade de Lisboa Laboratoire d’Astrophysique, Observatoire de Grenoble Department of Physics & Astronomy, University of Georgia 315 Stars & Stellar Systems Posters SSS -9: #122 On the sensitivity of extrasolar mass–loss rate ranges: HD 209458b a case study C. Villarreal D’AngeloB1,2 ; M. Schneiter1,2,3,4 ; A. Costa1,2,3,4 ; P. Velázquez5 ; A. Raga5 We present a 3D hydrodynamic study of the effect that different stellar and planetary wind conditions have on the calculated Ly↵ absorptions during transit. We concentrate, as a case study, on the known HD 209458b case. By comparing the numerically obtained Ly↵ absorption with the observations, we find that the planetary mass loss rate does not change dramatically for large changes in stellar wind speeds [400 s 1 1200] km . Several models with anisotropic evaporation profiles for the planetary escaping atmosphere were carried out, showing that both, the escape through polar regions, resembling the emission associated with reconnection processes, and through the night side, produced by a strong stellar wind that compresses the planetary atmosphere and inhibits its escape from the day hemisphere, yields larger absorptions than an isotropic planetary wind. B 1 2 3 4 5 [email protected] Instituto de Astronomı́a Teórica y Experimental (IATE), Córdoba, Argentina Fellow of Consejo Nacional de Investigaciones Cientı́ficas y Técnicas (CONICET), Argentina Member of the Carrera de Investigador Cientı́fico (CONICET), Argentina Profesor Faculty of Ciencias Exactas, Fı́sicas y Naturales Universidad Nacional de Córdoba, Argentina Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, DF, México 316 Posters Stars & Stellar Systems SSS -9: #123 Abundances and Kinematics of the Galactic Bulge [VVV] Zoccali, M.B1 I will present the latest results of a spectroscopic survey of bulge K giants, in 25 fields spread across the bulge area covered by VVV. B 1 [email protected] Instituto de Astrofı́sica, Pontificia Universidad Católica de Chile 317 Stars & Stellar Systems Posters SSS -9: #124 White dwarf-main sequence binaries from SDSS DR8: unveiling the cool white dwarf population A. Rebassa-Mansergas1,2 ; C. Agurto-GangasB2 ; M. R. Schreiber2,3 ; B. T. Gansicke4 ; D. Koester5 The spectroscopic catalogue of white dwarf main-sequence (WDMS) binaries from the Sloan Digital Sky Survey (SDSS) is the largest and most homogeneous sample of compact binary stars currently known. However, because of selection effects, the current sample is strongly biased against systems containing cool white dwarfs and/or early-type companions, which are predicted to dominate the intrinsic population. In this study, we present colour selection criteria that combines optical (ugriz DR 8 SDSS) plus infrared (yjhk DR 9 UKIRT Infrared Sky Survey, JHK Two Micron All Sky Survey and/or w1w2 Wide-Field Infrared Survey Explorer) magnitudes to select 3419 photometric candidates of harbouring cool white dwarfs and/or dominant (M dwarf ) companions. We demonstrate that 84 per cent of our selected candidates are very likely genuine WDMS binaries, and that the white dwarf effective temperatures and secondary star spectral types of 71 per cent of our selected sources are expected to be below < ⇠ 10000 15000K, and concentrated at ⇠ M 2 M 3, respectively. We also present an updated version of the spectroscopic SDSS WDMS binary catalogue, which incorporates 47 new systems from SDSS DR 8. The bulk of the DR 8 spectroscopy is made up of mainsequence stars and red giants that were targeted as part of the Sloan Extension for Galactic Understanding and Exploration (SEGUE) Survey, therefore the number of new spectroscopic WDMS binaries in DR 8 is very small compared to previous SDSS data releases. Despite their low number, DR 8 WDMS binaries are found to be dominated by systems containing cool white dwarfs and therefore represent an important addition to the spectroscopic sample. The updated SDSS DR 8 spectroscopic catalogue of WDMS binaries consists of 2316 systems. We compare our updated catalogue with recently published lists of WDMS binaries and conclude that it currently represents the largest, most homogeneous and cleanest sample of spectroscopic WDMS binaries from SDSS. B [email protected] Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China 2 Departamento de Fı́sica y Astronomı́a, Universidad de Valparaı́so, Avenida Gran Bretaña 1111, Valparaı́so, Chile 3 Millenium Nucleus ‘Protoplanetary Disks in ALMA Early Science,’ Universidad de Valparaı́so, Avenida Gran Bretaña 1111, Valparaı́so, Chile 4 Department of Physics, University of Warwick, Coventry CV4 7AL, UK 5 Institut für Theoretische Physik und Astrophysik, University of Kiel, D-24098 Kiel, Germany 1 318 Posters Stars & Stellar Systems SSS -9: #125 A Candidate Globular Cluster Behind the Milk Way? A. Roman-LopesB1 ; R. Barba; D. Minniti; R. Carrasco; P. Lucas In this contribution we will present the results of a study of a candidate Globular Cluster found in the framework of the VVV survey. The new cluster seems to be very old and is possibly crossing the Galactic plane just behind the Carina Arm, at an heliocentric distance of 7-8 kpc. B 1 2 3 4 [email protected] Universidad de La Serena (Chile) Pontificia Universidad Catolica (Chile) Gemini South Observatory (Chile) University of Hertfordshire - (United Kingdom) 319 320 Star Formation SF -1: #126 3D Simulations of the Beehive Proplyd Feitosa, J. A.B1 ; Vasconcelos, M. J.2 ; Cerqueira, A. H.3 Some star formation regions, like Orion nebula, have stars of different masses, from massive stars, responsible for strong ionizing winds and HII regions, to low-mass stars, which spends a long time in protostellar phase, frequently associated with protostellar disks and jets. Massive O or B stars emit a great deal of UV radiation, able to dissociate the hydrogen molecule (FUV radiation, energies between 6-13 eV), to ionize the atomic hydrogen (EUV radiation, energies greater than 13.6 eV) and heat the gas. Around these stars, a large and hot (104 K) region is formed, known as HII region. T-Tauri stars inside HII regions produce a type of young stellar object, a proplyd, described with accuracy in O’Dell et al. (1993). Due to the photoevaporation of protostellar disks by the UV radiation from massive stars in the vicinity, proplyds exibit a cometary shape from which we can distinguish a central low-mass star with an accretion disk and, eventually, a protostellar jet, an ionization front, a photodissociation region and, sometimes, a bow shock. Characteristics like the presence or absence of a bow-shock and the photodissociation region’s size depend on the distance between the low-mass star and the source of ionizing radiation. The Beehive, a giant proplyd in Orion Nebula, has atractted attention due to its exotic system of rings coaxial to the HH540 jet’s axis. Bally et al. (2005) suggested that the rings are perturbations due to the crossing of the ionization front by the jet. In this work, we test this hypothesis making 3D hydrodynamic numerical simulations over an adaptive grid, using the Yguazú-A code (Raga et al., 2000), properly adapted for the Beehive conditions. Our results show that the jet causes a perturbation in the ionization front of the proplyd, but is necessary to adjust carefully some parameters of the jet like its velocity and ejection frequency in order to have the results matching the observations. B 1 2 3 [email protected] Universidade Estadual de Santa Cruz Universidade Estadual de Santa Cruz Universidade Estadual de Santa Cruz 321 Star Formation Posters SF -1: #127 Study of triggered star formation in a bright-rimmed cloud Ortega, M. E.1 ; Paron, S.1 ; Giacani, E.B1 ; Petriella, A.1 Bright-rimmed clouds (BRCs) are small and dense molecular clouds located in the periphery of the evolved HII regions. The illumination of these dark clumps by nearby OB stars might be responsible for triggered collapse and subsequent star formation through the mechanism known as radiation-driven implosion (RDI). In this work, we present a multiwavelength study of a BRC located in the periphery of an uncataloged Galactic HII region. From the evaluation of the pressure balance between the ionized gas located at the illuminated border of the clump and the molecular gas, we analyze the influence the ionization front of the HII region has had on the stability of the BRC. Finally, the young stellar objects embedded in the BRC are characterized and the possibility that its formation has been initiated by the expansion of the HII region is discussed. B 1 [email protected] Instituto de Astronomia y Fisica del Espacio (CONICET-UBA) 322 Posters Star Formation SF -1: #128 On the association of young star clusters and their parental clouds: a statistical fractal analysis Hetem, A.B1 ; Gregorio-Hetem, J.2 We present a study of 21 young star clusters aiming to characterize their association to dense clouds. The structure of the clouds was evaluated by means of the Q statistical fractal analysis, designed to compare their geometric structure with the spatial distribution of the cluster members. The sample was selected from the study by Santos-Silva and Gregorio-Hetem (2012) that evaluated the radial density profile of the stellar superficial distribution of the young clusters. The fractal dimension and other statistical parameters of most of the sample indicate that there is a good cloud-cluster correlation, when compared to other works based on an artificial distribution of points (Lomax et al. 2010). As presented in a previous work (Fernandes et al. 2012), the cluster NGC 6530 is the only object of our sample that presents anomalous statistical behavior. The fractal analysis shows that this cluster has a centrally concentrated distribution of stars that differs from the substructures found in the density distribution of the cloud projected in the AV map, suggesting that the original cloud geometry was changed by the cluster formation. B 1 2 [email protected] CECS/UFABC IAG/USP 323 Star Formation Posters SF -1: #129 Increase of Ionization Fraction of Dusty Proto-Stellar Accretion Disks by Damping of Alfvén Waves Jatenco-Pereira, V.B1 The ambient of the cloud that gives rise to the process of star formation is consisted of: turbulence, magnetic field and dust. In general, in the process of star formation there is the formation of an accretion disk whose material must lose their angular momentum in order to be accreted into the central object. The magneto-rotational instability (MRI) is probably the mechanism responsible for a magneto-hydrodynamic (MHD) turbulence that leads to disk accretion. However, this mechanism only exists if the gas in the disk is sufficiently ionized to be coupled to the magnetic field. Besides the viscous heating mechanism often included in the models by means of the ↵-prescription, in this work we study the damping of Alfvéén waves as an additional heating source. The waves suffer a damping near the dust-cyclotron frequency, since charged grains in a magnetized disk are highly coupled to the waves due to cyclotron resonances. We study the transfer of energy from the damping of the waves to the disk and we show that this mechanism can increase the ionization fraction, making possible the presence of the MRI in a large part of the disk. B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo 324 Posters Star Formation SF -1: #130 Modeling the circumstellar environment of AB Aur using the Halpha line Lima, G. H. R. A.B1 ; Perrault, K.2 ; Benisty, M.2 ; Dougados, C.2 AB Aurigae is the brightest Ae Herbig star in the northern hemisphere and it shows evidence of accretion and ejection processes in the star, moreover the H↵ line shows a P-Cygni profile which is a common indication of wind. Its H↵ line is very variable, and most of this variation occurs in its blue-shifted side. One of the processes that can be used to explain this variation is a disk wind similar to those of the classical T Tauri stars. AB Aurigae has been observed using spectral interferometry in the optical region, by the VEGA spectrometer in the CHARA-array, which can resolve details of milliarcseconds in size that in the case of AB Aur represent sizes smaller than 1 AU. With these resolution, it’s possible to observe the region where the wind is being ejected. Using a radiative transfer code that already had been used to model the H↵ line profiles in classical T Tauri stars, and adapting it to model the H↵ line in AB Aur, it will be possible to calculate an intensity map showing the region where this line is being formed, and then compare it with data from the interferometric observations. This work will give us a better understanding of the ejection and accretion mechanism that are responsible for the formation of the H↵ line around AB Aur and in some of the Herbig Ae/Be stars, and wether a disk wind mechanism can explain or not this line in these objects. B 1 2 [email protected] Universidade Federal de Minas Gerais Institut de Planetologie et d’Astrophysique de Grenoble 325 Star Formation Posters SF -1: #131 Steady-state Accretion Disk Models With Variable Alpha Magalhaes, E. R. S. O.B1 ; Cerqueira, A. H.1 ; Vasconcelos, M. J.1 Accretion disks around young stellar objects are commonly described by models that use a standard average viscosity to allow, via differential rotation, a mechanism of dissipation and consequent accretion of mass and angular momentum transport. In this work we use this same prescription to reproduce the final characteristics of an accretion disk, but we relax the condition of constant viscosity using a variable ↵ parameter, as suggested in recent studies of a selected sample of YSO’s. We first discuss the behaviour of the solutions of ↵ variable, steady-state, thin accretion disks, in comparison with standard solutions of ↵ non-variable. For the sample of YSO’s studied, we emphasize that ↵ tends to high values close to the star (inner radius), allowing best conditions for launching jets as expected from both theoretical and observational results. We also evaluate the consequences of this choice on the determination of the initial mass of planetesimals (Mp ). Although this calculations could not be directly applied to planetary studies (since we have only the steady-state solutions), we can discuss the relevance of it to promote changes in seed values of the mass of the planetesimals, since it scales with the superficial density profile. These profiles, as we show, are very sensitivy to the ↵ choice, and then, changes Mp accordingly. B 1 [email protected] Universidade Estadual de Santa Cruz 326 Posters Star Formation SF -1: #132 A survey of extended H2 emission toward a sample of massive YSOs Navarete, F.B1 ; Daminelli, A.1 ; Barbosa, C. L.2 ; Blum, R. D.3 Very few massive stars in early formation stages were clearly identified in the Milky Way and moreover, the processes of formation of such objects lacks of observational evidences. Two theories predict the formation of massive stars: i) by merging of low mass stars or ii) by an accretion disk. One of the most proeminent evidences for the accretion scenario is the presence of bipolar outflows associated to the central sources. Those structures were found on both intermediate and low- mass young stars, but there are no evidences for associations with MYSOs. Based on that, a survey was designed to investigate the earliest stages of massive star formation through the molecular hydrogen transition at 2.12 µm. A sample of ⇠ 300 massive YSO candidates was selected from the Red MSX Source survey (Mottram et al., 2011) and the sources were observed with the IR cameras Spartan (at SOAR, Chile) and WIRCam (at CFHT, Hawaii). Extended H2 emission was found toward 55% of the sample and 30% of the positive detections (50 sources) have a bipolar morphology, suggesting collimated outflows. These results support the accretion scenario, since the merging of low mass stars would not produce jet-like structures. B 1 2 3 [email protected] Universidade de São Paulo, Brazil UNIVAP, Brazil NOAO 327 Star Formation Posters SF -1: #133 A Spectro-photometric study if the young stellar cluster sigma Orionis. Pérez A.B1 ; Hernández J.1 ; Calvet N.2 ; Olguin L.3 ; Contreras M.4 ; Briceño C.1 ; Allen L.5 ; Espailat C.6 We performed a spectro-photometric study of the young stellar cluster Sigma Orionis with the purpose of obtain a better characterization for its stellar population. The sigma Orionis cluster is a natural laboratory used to study the formation and early evolution of stars and protoplanetary disks from its most massive member to planetary mass objects. This is because it is reasonably near (D<500pc), the reddening toward the cluster is low (Av⇠0.2) and it is relatively populous. Its age of 3 Myr allows us to perform studies of protoplanetary disks around stars with different masses when disk dissipation processes have modified substantially the structure of disks. Analyzing great amount of data collected from different observatories and instruments we have the capacity to recognize and to characterize members of the cluster in a homogeneous way. With this in mind we have obtained UBVRI photometry from the OSMOS instrument installed in the 2.4 telescope at the MDM observatory. Low resolution spectra come from several spectrographs with similar spectroscopic coverage and resolution (HECTOSPEC-MMTO, FAST-FLWO, OSU-CCDS-MDMO, B&C-San Pedro Martir, B&C-Cananea). This data was processed with specialized programs such as IRAF and the SpTClass code (Spectral CLASSificator) to obtain spectral types and the basic analysis of spectral features normally present in young stars (e.g. Halpha in emission and LiI 6707 in absorption). With these results we have recognized members of the sigma Orionis cluster and obtained stellar parameter such as effective temperature, visual extinction and luminosity. In addition, radial velocity were derived from HECTOCHELLE data (obtained at MMTO) using the IRAF package rvsao with cross-correlates each spectrum with a set of templates. The radial velocity distribution for members of the cluster can be described by a Gaussian centered at 30.8 km/s with a sigma of 1.7 km/s. This result is in agreement with previous work. B 1 2 3 4 5 6 [email protected] Centro de Investigaciones de Astronomı́a (CIDA), Mérida, Venezuela Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, US U. de Sonora, Mexico UNAM-Ensenada, Mexico NOAO, USA Harvard-Smithsonian Center for Astrophysics. 328 Posters Star Formation SF -1: #134 Time-series JHK Photometry of Stars in the center of Cygnus OB2 Roquette, J. M. T.B1 ; Vaz, L. P. V1 ; Guimarães, M. M.2 Cygnus OB2 is an OB association located in the direction of the Local Spiral Arm, harbouring some of the most massive and luminous stars in the Galaxy. Studying its high mass population, we learned that it is a rich star forming region, located behind a dust cloud which is responsible for the high extinction measured in that area of the sky (10 – 20 MV ). Its estimated age of 3Myr makes it an appropriate target for studying young stars. We performed a photometric variability survey in this region using near-infrared filters (JHK), with the Wide Field Camera (WFCAM) of the United Kingdom Infrared Telescope (UKIRT), during 112 nights, unevenly spaced in a period of 217 days. A total area of 520.96 ⇥ 520.96 was covered with Cygnus OB2 in its center. We present provisional results concerning rotational periods for stars stars within its central region (a sub-area of 130 .65 ⇥ 130 .65 ). B [email protected] Universidade Federal de Minas Gerais (UFMG) 2 Universidade Federal de São João Del Rei (UFSJ) 1 329 Star Formation Posters SF -2: #135 Infrared study of new star clusters associated to dusty globules Soto King, P.B1 ; Barba, R. H.1 ; Roman Lopes, A.1 ; Firpo, V.1 ; Soto, M.2 ; Minniti, D.3 ; Lucas, P.4 We present results from a study of a sample of small star clusters associated to dusty globules and brightrimmed clouds that have been observed with VISTA telescope in the framework of the ESO/Chile public infrared survey Vista Variables in the Vı́a Láctea (VVV). Also, we included in the analysis data collected by Spitzer Space Telescope and Wide-field Infrared Survey Explorer. In this short communication, we present the infrared properties of the clusters derived from the color-color and color-magnitude diagrams. We identify and classify young stellar objects (YSOs) through the infrared spectral energy distribution combining the available mid-infrared photometry and the PSF analysis performed on VVV images. Also, we derive the ratio between Class I to Class II YSO source candidates in each globule. The sample of selected dusty globules and bright rimmed globules are extracted from the new list of VVV clusters discovered at Universidad de La Serena. These dusty globules are simple laboratories to study the star formation relatively free of the influence of large star-forming regions and clusters, and they are in contrast compared with those bright rimmed globules, which are influenced by the action of nearby O and B massive stars. B 1 2 3 4 [email protected] Universidad de La Serena Space Telescope Science Institute Pontificia Universidad Catolica de Chile University of Hertfordshire 330 Posters Star Formation SF -2: #136 The inner disks of classical T Tauri stars in NGC 2264 B1 Sousa, A. P. ; McGinnis, P. T.1 ; Alencar, S. H. P.1 ; Bouvier, J.2 ; Texeira, P.3 ; Stauffer, J.4 ; CSI2264 Team NGC 2264 is a young (⇠ 3 Myr) stellar cluster that was observed twice by the CoRoT satellite, for 23 days in 2008 and 40 days in 2011. Simultaneouslys with the 2011 CoRoT observations, a multiwavelength campaign was organized that included 30 days of Spitzer observations at 3.6 and 4.5 microns, 3.5 days of Chandra data, VLT FLAMES spectroscopy and U band photometry from Megacam (CFHT). We obtained simultaneous high precision light curves in the optical and near IR for more than 500 cluster members, about 150 of which are classical T Tauri stars. As shown in the first CoRoT campaign, a fraction of the accreting systems exhibit optical light curves with deep minima that vary substantially in width and depth in a rotational timescale. These light curves are interpreted as being due to an inner disk warp that eclipses the star as the system rotates, as observed in AA Tau, a well studied CTTS seen at high inclination. This warp is thought to be created by the star-disk interaction mediated by a stellar magnetic field inclined with respect to the stellar rotation axis. The observed variability indicates that the star-disk interaction is dynamic and the occulting material is inhomogeneous and located close to the co-rotation radius of the star-disk system. We present the photometric and spectroscopic analysis of the AA Tau-like CTTSs observed in NGC 2264. Initial light curve model results indicate that an inner disk warp located near the co-rotation radius can indeed explain the observed variability and that, if the variability is attributed to extinction alone, the properties of the dust in the inner disk are substantially different from the ISM. B 1 2 3 4 [email protected] Universidade Federal de Minas Gerais - UFMG Institut de Planétologie et d’Astrophysique de Grenoble - IPAG Institut für Astrophysik Universität Wien Spitzer Science Center - Caltech 331 Star Formation Posters SF -2: #137 Finding proto-spectroscopic binaries: Precise multi-epoch radial velocities of 7 protostars in Ophiuchus Viana Almeida, P.B1,2,3,4 ; Melo, C.2 ; Santos, N. C.1,3 ; Figueira, P.1 ; Sterzik, M.2 ; Gameiro, J. F.1,3 ; Alencar, S.4 Stars in the solar neighborhood are mostly found in multiple systems. While the existence of stellar companions at visual distances can be easily explained as a normal outcome of the star formation process itself, it is still unclear how spectroscopic companions are actually formed. If they are a by-product of the initial fragmentation of molecular clouds, or resultant from dynamical evolution within pristine multiple systems is still an open question in star formation. To uncover a young spectroscopic binary would be therefore an invaluable clue for understanding the mechanisms and the time scales involved in their formation. Aiming at finding such young spectroscopic companions, we present a near-IR high resolution (R > 50000) multiepoch radial velocity survey of 7 young stellar objects in the star forming region rho Ophiuchus. The radial velocities of each source were derived using a two-dimensional cross-correlation function designed to deliver the radial velocity of the target relative to the zero-point established by the earth’s atmosphere. We found that the spectra of the protostars in our sample agree reasonably well with predicted stellar photospheric profiles indicating that the radial velocities uncovered are of stellar nature. Three of the targets analyzed give us string evidence that the first proto-spectroscopic binaries might have been found. We present preliminary orbital solutions for two of the targets based on six epochs of observations. If these binaries are further confirmed, it will bring an important piece into the (binary) star-formation puzzle, namely, that multiplicity at sub-AU scale starts (or not) at birth. Our preliminary binary fraction of 71% (when merging our results with those of previous studies) is also in line with the notion that multiplicity is very high at young ages and therefore it might be a product of star-formation. B 1 2 3 4 [email protected] Centro de Astrofı́sica, Universidade do Porto ESO/Chile Departamento Fı́sica e Astronomia, Faculdade de Ciências da Universidade do Porto ICEX, Universidade Federal de Minas Gerais 332 Posters Star Formation SF -2: #138 Chromospheric and Coronal Activity in Stars Before the Main Sequence Alexander, N. C.B1 ; Giovanni, P. E.1 In the study of stellar activity spectroscopy plays an important role behind this variability are discussed in important lines of the spectra taken by powerful tools with which today account. In this work we make a spectroscopic analysis which makes fluxes calculation to find indicators such as chromospheric and coronal RHK indicator of CAII in 3920 Å, and two lines in the infrared triplet (IRT) at 6500 Å CAII activity chromospheric; for use coronal activity normalized soft X-ray bolometric fluxes; These indicators correlate with rotation Nr (Rossby number) and age for a sample of stars from different open clusters of different ages as: BMW (11-12 Myr), UCL (14Myr), LCC (16Myr), THA (30M yr) and different spectral types F, G and K the basic idea of this work is to verify that these indicators of activity decay with time and are closely related to stellar rotation (Marsden et al 2009). For chromospheric analysis using spectral subtraction technique (Montes et al. 1995) and also a compilation of sample data for the ROSAT X-ray fluxes in total the number of stars that will be analyzed is 42 and 4 reference stars. All spectra are taken from the database ESO (European Southern Observatory with the FEROS instrument (The Fiber-fed Extended Range Optical Spectrograph) whose resolution of 48000 and a hedge between 3200-9000 Å allows us to perform more detailed analysis of the lines of interest. B 1 [email protected] Universidad Nacional de Colombia 333 Star Formation Posters SF -2: #139 Emission-line stars in the star-formation region NGC 1850 Garrido, H. E.B1,2 ; Martayan, C.1 ; Mennickent, R. E.2 ; Aguayo, G.2 ; Baade, D.3 We studied the properties of the stellar populations in a field 11 x 8’ around the center of the OB association NGC 1850, based on the analysis of slitless spectroscopic data obtained with the ESO Wide Field Imager, 63 emission-line stars and one Double period variable star located in and around the LMC clusters NGC 1850 and NGC 1855 have been identified. Most of the emission-line stars are located in the vicinity of the young double cluster NGC 1850. Among them, In addition to pre-main sequence stars and giant stars, new candidate B0-B5 Be stars were also found. The photometry and lightcurves are also used to obtain additional physical parameters of those stars such as their evolutionary status/age. Combining all these observations suggests that the NGC 1850 star-formation history has followed different episodes due to the dynamical interaction between clusters, photo-ionization, and compression of the associated H II region, leading to ”recent” star formation bursts. The OB association NGC 1850 is found in the border of the Supergiant shell LMC 6 and their local background zone. We conjecture that the expansion of the SGS LMC 6 could play a role in the current star formation in the zone. Our analysis of the stars in the field indicate a possible mass and spatial segregation with the evolution/age of the clusters and stellar populations. B [email protected] European Organisation for Astronomical Research in the Southern Hemisphere, Alonso de Cordoba 3107, Vitacura, Casilla 19001, Santiago 19, Chile 2 Universidad de Concepción, Departamento de Astronomı́a, Casilla 160-C, Concepción, Chile 3 European Organisation for Astronomical Research in the Southern Hemisphere, Headquartes, Garching bei Munchen, Germany 1 334 Posters Star Formation SF -2: #140 Magnetic Fields dispersion and YSO properties on nearby Bok globules Magalhães, V. S.B1 ; Rodrigues, C. V.2 ; Pereyra A.2 ; Racca G. A.2 ; Vilas-Boas, J. W. S 2 We conducted an observational study of the relation between magnetic field properties and star formation in Bok globules. We used polarimetry to map the interstellar magnetic field direction in twenty (20) sky regions containing Bok globules. The maps created were used to estimate the dispersion of the magnetic field direction in each region fitting the polarization angle histogram to a gaussian curve. In addition to the Gaussian dispersion, we propose a new quantity to estimate the magnetic field organization that does not rely on any function fitting. We selected all the red sources in the WISE Point Source Catalog in 15’ x 15’ regions centered on the Bok Globules. We then constructed spectral energy distributions (SEDs) using publicly available data (2MASS, AKARI, GLIMPSE, WISE). To verify whether the sources are pre main-sequence objects we compared the SEDs to young stellar objects (YSOs) models available online (Robitaille et al. 2007). This also yielded estimates of mass, age, inclination of the found YSOs. With this information at hand we classified the regions as star forming or not. Statistical tests show no clear difference in the magnetic field dispersions of the sub-samples of globules with and without star formation. We also discuss some trends as a function of the YSOs properties. B 1 2 [email protected] Currently Unaffiliated Divisão de Astrofı́sica, Instituto Nacional de Pesquisas Espaciais 335 Star Formation Posters SF -2: #141 Star formation at the edge of the Universe Matos, S.B1 ; Best, P.1 ; Sobral, D.2 The most fundamental observational properties that need to be determined to obtain a comprehensive understanding of the physical processes of galaxy formation and evolution are the cosmic star formation history of the Universe and the volume-averaged star formation rate as a function of epoch. Previous studies have made considerable progress in recent years, but even so their measurements are affected by significant scatter and uncertainties due to the use of different star-formation indicators, worsened by small area sampling and the effects of cosmic variance. We aim at overcoming these issues by using wide-field, sensitive un-biased surveys of star-forming galaxies at a range of redshifts across the peak epoch of cosmic star-formation. We present the first robust sample of star-forming galaxies at high redshifts (Lyman-emitter at z > 7) is obtained from a large area (12 deg2 ) extragalactic survey within the epoch of reionisation and places strong constraints on the bright end of the Lyman-luminosity function. B 1 2 [email protected] Royal Observatory of Edinburgh, University of Edinburgh Leiden Observatory, University of Leiden 336 Posters Star Formation SF -2: #142 Rotation and activity of Post T Tauri Stars Pinzón, G.B1 We present the main results of a study of rotation and chromospheric activity of 33 young post T Tauri low mass stars of the southern hemisphere with spectral types G-K belonging to the stellar associations: TWA Hya ( 10Myr), BPMG ( Myr), Upper Centaurus Lupus (UCL, 20Myr), Lower Centarus Crux (LCC, 23Myr) and Tucana - Horologium (THA, 30Myr). Using both, UBVRI photometry and FEROS optical spectra we found that the rotation - activity relation shows prominent differences with those observed in main sequence stars indicating that young low mass stars generate their magnetic fields in a different way. Theoretical predictions using a time-dependent stellar spin evolution model were also done and confirm that such kind of spin up is a consequence of the end of the disks at the begining of the post T Tauri stage. B 1 [email protected] Observatorio Astronómico, Facultad de Ciencias, Universidad Nacional de Colombia 337 338 ISM ISM -1: #143 New Avenues for Measuring Magnetized Turbulence in the Multiphase Interstellar Medium Burkhart, B.B1 ; Lazarian, A.1 The current paradigm of the ISM and Solar Wind is that it is turbulent with turbulence affecting many important processes. For the ISM this includes star formation, cosmic ray acceleration, and the evolution of structure in the diffuse ISM. This makes it important to study interstellar and interplanetary turbulence using the strengths of numerical studies combined with observational studies. I shall discuss progress that has been made in the development of new techniques for comparing observational data with numerical magnetohydrodynamic (MHD) simulations. In particular I will discuss the robustness of measuring the sonic Mach number from molecular line observations, which is an important tool for investigating the dynamics of Giant Molecular Clouds. I will also discuss how one can obtain estimations of the magnetic field in interstellar clouds using statistical methods rather than the traditional time consuming methods such as Zeeman spliting. These new techniques fit into the broader scope of providing avenues for studying MHD turbulence across different ISM phases. B 1 [email protected] University of Wisconsin Madison 339 ISM Posters ISM -1: #144 3D Modelling of the Bipolar Planetary Nebula NGC 2346 Carneiro, C. M.B1 ; Gonçalves, D. R.1 Planetary nebulae (PNe) represent the final stages of evolution of low- and intermediate-mass stars, when the matter ejected from the star forms bright ionized shells. Most of the PNe are not spherically symmetric (about 70% are of ellipticals and bipolars and 20% have round morphologies) possibly because of the binarity of the central star. Photoionization codes intent to reproduce the interactions of the central star’s radiation with the nebular gas, in order to obtain information of both, gas and central star. So, it is possible to determine the electron temperature and density, the ionization stage of the elements, as well their ionic and total chemical abundances. Concerning the star, its effective temperature and luminosity can also be deduced. The chemical abundances of PNe provide an important tool to study the chemical evolution of galaxies. These abundances are mostly derived using the ionization correction factors empirical method, which are strongly uncertain, since they were derived using 1D photoionization codes, which assume spherical symmetry to all PNe. There is only one 3D model of a bipolar planetary nebula (NGC 6302) in the literature. We are developing the modelling of the bipolar PN NGC 2346, which has a single-lined spectroscopic binary central star. From the best model we obtained, so far, this is a low electron density nebula (⇠ 300 cm 3 ), with typical PNe electron temperature (10,000 K to 14,000 K) and a hot central star (10 K), for which lumi5 nosity (therefore, distance) is not yet well constrained. The agreement of our best fitting model with the intense optical emission-lines is of 96%, though the dimensions used in this model might be slightly underestimated. Improved models including dust and a more accurate central star ionizing radiation (T. Rauch’s stellar atmosphere results) will be presented, as well as the fitting to others (than optical) spectral regions whose observational constraints are available. B 1 [email protected] Observatório do Valongo, Universidade Federal do Rio de Janeiro 340 Posters ISM ISM -1: #145 G126.1–0.8–14: A molecular shell related to Sh2-187 Cichowolski, S.B1 ; Pineault, S.2 ; Gamen, R.3,4 ; Ortega, M. E.1 ; Arnal, E. M.3,5 ; Suad, L. A.5 In this work we present a multi-wavelength study of a region where a well defined molecular shell (G 126.1– 0.8–14) is observed. G 126.1–0.8–14 is located in the Orion arm, at a distance of about 1 kpc. Based on CGPS HI and CO data we analyze the atomic and molecular gas related to the structure and estimate its main physical properties. From the radio continuum and infrared data we analyze whether the emission associated with G 126.1–0.8–14 has a thermal origin. On the other hand, to disentangle the possible origin for the shell, and given the lack of catalogued O-type stars in the area, we observed with GEMINI the spectrum of four OB stars (Reed 2003, AJ, 125, 2531) located in projection inside the shell, to get their accurate spectral types and distances. The HII region Sh2-187 is located onto the densest part of this molecular shell. It is known that this ionized region is small (⇠ 9’) and young (⇠ 2 ⇥ 105 yr), and shows signs of recent star formation activity in its surroundings. A search for young stellar object candidates (cYSO) was made using different infrared point source catalogs (IRAS, MSX, WISE, and 2MASS). Besides the sources present near Sh2-187, many others are found spread out onto the shell. Based on all the available data, we discuss the possible origin of G 126.1–0.8–14 as well as its role in the formation of a new generation of stars. B 1 2 3 4 5 [email protected] Instituto de Astronomı́a y Fı́sica del Espacio (IAFE) Université Laval Facultad de Ciencias Astronómicas y Geofı́sicas Instituto de Astrofı́sica de La Plata Instituto Argentino de Radioastronomı́a (IAR) 341 ISM Posters ISM -1: #146 Deep infrared extinction maps of the Fourth Galactic Quadrant based on VVV and GLIMPSE surveys Firpo, V.B1 ; Soto, M.2 ; Barba, R. H.1 ; Roman Lopes, A.1 ; Minniti, D.3 ; Lucas, P.4 The ESO/Chile public infrared survey VISTA Variables in the Vı́a Láctea (VVV) is changing our view of the inner Galactic disk and Bulge. The VVV survey have observed 220 deg2 of the Galactic plane in 152 tiles, in five infrared bands. Based on these tiles of the Galactic disk, we have created a merged catalogue in three bands (J, H and Ks) using the photometric catalogues produced by the CASU pipeline. This merged catalogue with 136 millions sources was used to produce deeper source-count maps, and then again crossmatched with GLIMPSE (Spitzer Space Telescope) catalogue, to get a combined VVV-GLIMPSE catalogue, with 12.4 ⇥ 106 stars. In this presentation, we report the development of a VVV+GLIMPSE extinction map for the Fourth Quadrant of the Galactic disk based on the Rayleigh-Jeans Color Excess method (Majewsky et al.). For a wide range of spectral types, the combination of NIR and MIR photometry allows to sample the Rayleigh-Jeans part of the spectral energy distribution, where the intrinsic color of stars falls in a narrow range. Thus, a simple color equation can be used to derive the extincion per star in the Ks -band, AK . These new maps are in agreement with recent works, and represent a significant improvement over the current situation because of, thanks to the VVV protometry, we have obtained deep extinction maps with a spatial resolution of 1 arcmin. B 1 2 3 4 [email protected] Universidad de La Serena, Chile Space Telescope Science Institute, USA Pontifica Universidad Catolica, Chile University of Hertfordshire, UK 342 Posters ISM ISM -1: #147 A bolha infravermelha N10 Gama, D.B1 ; Lepine, J.1 ; Wu, Y.2 ; Yuan, J.2 A formação de estrelas massivas ainda não está totalmente compreendida. Bolhas infravermelhas podem prover indı́cios sobre as condições fı́sicas da interação entre regiões HII e ventos de estrelas massivas. O objeto N10 é uma bolha infravermelha, detectada através do GLIMPSE, um levantamento realizado entre 3.6 e 8.0 µm. A inspeção visual revelou anéis que podem representar bolhas tridimensionais. Autores sugerem que essas bolhas são primeiramente formadas por estrelas quentes em regiões de formação estelar. Bolhas formadas dinamicamente precisam de uma estrela, ou aglomerado, com emissão UV suficiente para excitar caracretı́sticas de PAHs nas bandas IRAC 5.8 e 8.0 µm. Também foi analisada a emissão em 24 µm, que é resultado da emissão da poeira quente. Já a emissão em 8 µm é dominada por caracterı́sticas de PAHs excitados por radiação proveniente das PDRs. No caso de N10, propõe-se que o excesso na banda 4.5 µm do IRAC indicaria um outflow - assinatura de estágios primários de formação de estrelas massivas. Sugere-se que a bolha seja soprada por uma região HII central. Esse objeto foi alvo de observações realizadas no PMO, que possui uma antena de 13.7 metros, situada na cidade de Nanjing, China. As transições moleculares observadas foram 12 CO (1-0), 13 CO (1-0) e C18 O (1-0), nas frequências de 115, 110 e 109 GHz, respectivamente. A investigação da bolha N10 pode revelar detalhes acerca da atividade de formação estelar devida a processos sequenciais nessa região, assim como fornecer informações a respeito do status do material molecular associado com a bolha. Os próximos passos serão utilizar rotinas adequadas para obter parâmetros observados na região, para a componente principal, segunda e terceira componentes, tanto para a emissão em 12 CO quanto em 13 CO. Por meio dos parâmetros observados, podemos estimar a distância do objeto e comparar o valor encontrado com valores da literatura calculados por outros métodos. A bolha N10 apresenta clumps, dos quais podemos obter parâmetros fı́sicos através dos parâmetros observados. A discussão seguirá acerca da distribuição do gás na região e seu ambiente molecular. Também pretendemos discutir sobre o estágio evolutivo dos clumps, comparando a localização destes com a posição de fontes rádio, maser de metanol e estrelas tipo O ionizantes. Para avaliar a situação de formação estelar em N10, também realizamos um levantamento dos YSOs. B 1 2 [email protected] Departamento de Astronomia do IAG/USP, São Paulo, Brasil Department of Astronomy, Peking University, Beijing, China 343 ISM Posters ISM -1: #148 The magnetic field and dust properties in the direction of the dark cloud CG12 Hickel, G. R.B1 The dark cloud CG12 is situated about 200 pc above the Galactic Plane and 600 pc away from us. It has a very denser double core with 100 M (Avmax ⇠ 20 mag.). The cloud is under a radiative shock that triggers low mass star formation (⇠50 TTauri stars) with a high efficiency (⇠15 to 35%). In this work, I present a linear polarization (BVRI filters) in the CG12 direction. I analyzed the relationship between the polarization degree and extinction, and the dependency on the polarization degree with the wavelength along the cloud. The geometry and magnetic field strength were evaluated using the dispersion of the vectors of linear polarization. B 1 [email protected] UNIFEI 344 Posters ISM ISM -1: #149 High dispersion spectra and kinematic line profiles of NGC3918 and NGC6302 Lago, P. J. A.B1 ; Costa, R. D. D.1 Planetary Nebulae have rich optical spectra, formed by recombination and collisional excitation lines. The use of these lines allows the derivation of several physical parameters such as density, electron temperature, ionization degree and the kinematic profile. These nebulae have typical expansion velocities between 20 and 40 km/s. Using high dispersion, long slit spectroscopy obtained with the Coudé spectrograph at Pico dos Dias Observatory (MCT/LNA) in Brazil, we derived the kinematic profile from forbidden lines for different angular positions along the slit for two nebulae, NGC3918 and NGC6302. The second one shows a velocity profile that grows linearly with the distance to center. Using the velocity diagrams from this work and data from the literature, it was possible to calculate the distance of NGC6302, estimated in 805pc with an error of 143pc, in a good agreement with other results from the literature. For NGC3918, the same diagrams were used to estimate its kinematic age, assuming expansion with uniform velocity; the result was 3111 years for the external shell. Hereafter we intend to use the kinematic profiles to model these planetary nebulae with the SHAPE code, and apply this technique for a large number of southern planetary nebulae. (FAPESP, CNPq) B 1 [email protected] Universidade de São Paulo, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas 345 ISM Posters ISM -1: #150 3MdB: Mexican million models database Christophe MorissetB1 ; Gloria Delgado-Inglada1 We present the actual status of the 3MdB (Mexican Million Models dataBase). This database of photoionization models obtained with Cloudy are managed by MySQL from python using the pyCloudy package. The genetic method used to converge models on a set of observations is also presented, with prelimininary results on physical properties and abundances determination. B 1 [email protected] Instituto de Astronomia, UNAM, Mexico 346 Posters ISM ISM -1: #151 Structure of Bubbles in the South-East region of the Large Magellanic Cloud Oddone, M. A.B1 ; Ambrocio-Cruz, P.2 ; LeCoarer, E.3 ; Goldes, G. V.4 In this work we report the kinematical results of the structure located in the South-East region of the Large Magellanic Cloud, the Super Giant Shell LMC9. The observations have been carried out in the frame of an H↵ survey of the Magellanic Clouds and the Milky Way, carried out at ESO with a 36cm diameter telescope, equipped with a focal reducer, a scanning Fabry-Perot interferometer and a photon counting camera. The Supergiant Shell LMC9 is composed of four giant shell DEM164 and DEM165, DEM208, DEM221, and several HII region being the most notorious DEM202, DEM206 and DEM207. Morfologically, two of the complexes present structure of bubble-type, one of them DEM208 of oval shape of (200 x 180) pc with another structure in its interior near circular of 100 pc, meanwhile the HII regions DEM202, DEM206, DEM207 semble to form a unique structure conected by curve filaments of eliptical shape with a mayor axis of 250 pc. Other two complexes DEM164 and DEM165 seen ensemble seems to form an extended filament (400 pc) with an “S” shape. The complex DEM221, is the most irregular with (400 x 300) pc size, resembling by its filamentary and irregular appearance to the 30 Dorado nebula. By means of energy balance we determine the characteristics parameters of these structures (superfical brightness, electronic density, emission measure, mass, luminosity, ambient density, age), that would allow us to distinguish which is the origin (stellar wind, supernova explosion or other mechanism) of the differents bubbles that compose the Super Giant Shell LMC9. In this way we will try to discern if the studied objects have kinematically some identity as an ensemble, or if they are relatively aisolated objects over the diffuse general background to which they belonged. The same were investigated with the intention of stablishing its general kinematic and morphological characteristics and in addition analyzing its possible association to a large structure aiming above all to contribute to the elaboration of a detailled global kinematics image of the LMC. B 1 2 3 4 [email protected] Observatorio Astronómico de la Universidad Nacional de Córdoba, Laprida 854, X500BGR, Córdoba, Argentina Instituto de Ciencias Básicas e Ingenierı́a, Universidad Autónoma del Estado de Hidalgo, México Laboratorio de Astrofı́sica de la Universidad Joseph Fourier, Grenoble, Francia Facultad de Matemática, Astronomı́a y Fı́sica, Córdoba, Argentina. 347 ISM Posters ISM -2: #152 A new distance scale of planetary nebulae Ortiz, R.B1 A new distance scale of planetary nebulae is proposed, based on two main quantities: the flux density (or magnitude) at 8µm and the nebular apparent size. These quantities are used to calculate the specific intensity of the radiation I8µm , which decreases as the nebula evolves. PNe situated in the Large Magellanic Cloud (LMC) with 8µm photometry obtained by Spitzer and diameter calculated from HST observations are used as calibrators. After calibration, distances of PNe in the LMC were recalculated, and showed a 1-sigma spread of 10 kpc (20%). Eventually, the method was applied to a sample of 88 Galactic PNe observed during the Spitzer survey. These results showed an agreement within 0.2 dex with the distances determined by Stanghellini et al. (2008), which is another method calibrated with PNe in the LMC. The main advantage of the present distance scale is the fact that it is nearly “extinction free”, which makes it especially suited for PNe severely affected by interstellar extinction, such as the Galactic disc and bulge. B 1 [email protected] Escola de Artes, Ciências e Humanidades da USP 348 Posters ISM ISM -2: #153 Spectroscopic studies of two supernova remnants in the Large Magellanic Cloud Pauletti, D.B1 ; Copetti, M. V. F.1 Some characteristics of supernova remnants can be quite different in different objects, depending on their formation mechanisms, evolution stages and the properties of the local interstellar medium. Even within a single remnant, some physical properties can vary considerably. However, a great part of the spectroscopic works published about supernova remnants are based on integrated data (distant objects) or on data obtained from special positions (near objects). Spatially resolved observation covering the whole remnant may be essential to get a better knowledge of these objects. This work presents a study of two supernova remnants belonging to the Large Magellanic Cloud, N49 and N11L, based on the spectroscopic mapping of their physical properties. Long slit spectroscopy was used to collect data from a grid of different positions covering the whole nebula by positioning the slit on different and equally spaced declinations. The data were obtained with the 4.1 m SOAR telescope (Southern Astrophysical Research Telescope), in Chile. The spectral coverage was about 3500-8000 Å. For each object, about 50 emission lines were measured on the spectra of each object, allowing to build maps of many interesting line intensity ratios. The maps of electron density and temperature were obtained using the [S II] 6717/ 6731 and [O III] ( 5007+ 4959)/ 4363 line ratio sensors, respectively. N49 presents a strong density gradient with the density varying from 600 cm 3 at the North-West to more than 3000 cm 3 at the South-East. The electron temperature distribution shows a rough spherical symmetry with the higher values found at the centre. In N211L the electron density varies from less than 100 cm 3 to about 400 cm 3 , with the higher values found on the bright filaments. These maps were used to build a picture of the structure of these two supernova remnants. B 1 [email protected] Universidade Federal de Santa Maria 349 ISM Posters ISM -2: #154 Densities, temperatures, pressures, and abundances derived from O II recombination lines in H II regions and their implications Peimbert, M.B1 ; Peimbert, A.1 Based on high quality observations of multiplet V1 of O II and the NLTE atomic computations of O II we study the density and temperature of a sample of H II regions. We find that the signature for oxygen rich clumps of high density and low temperature is absent in all objects of our sample. These results imply that the proper abundances are those derived from recombination lines. We discuss the possible mechanisms responsible for the abundance discrepancy problem in H II regions. B 1 [email protected] Instituto de Astronomia, Universidad Nacional Autonoma de Mexico 350 Posters ISM ISM -2: #155 Multiwavelength study of the young stellar cluster [DBS2003]156 Marcio C. PinheiroB1 ; Roberto P. Ortiz2 ; Zulema Abraham3 ; Marcus V. F. Copetti4 The Norma section of the Milky Way is especially interesting because it crosses three spiral arms: SagittariusCarina, Scutum-Crux and the Norma arm itself. We present a study of the [DBS2003] 156 stellar cluster in Norma, associated with several radio sources characteristic of the presence of massive stars, such as continuum, H109↵ and methanol. The cluster was observed in the J, H and Ks bands at 1.300 resolution and limiting magnitudes comparable to the 2MASS survey. Potential massive stars were chosen among the infrared sources detected in the survey according to colour criteria, and subsequent spectroscopy of these candidates was performed with the OSIRIS spectrograph attached to the SOAR 4.1-m telescope. As a result, four stars with spectral types earlier than B1 were found, which are capable of maintaining the ionization of this nebula. The distance of this cluster, calculated by the spectrophotometric parallax technique, is 3.30 ± 0.55 kpc, in full agreement with the distance of the neighbouring [DBS2003] 157 cluster, previously determined as 3.29 ± 0.59 kpc. A comparison between Spitzer mid-infrared counterparts of the infrared sources detected in this survey with mid-infrared colours generated by theoretical models allows a crude estimation of the density of the accreting envelope around the young stellar objects in the cluster, between log ⇢(g cm 3 )= 14.0 ⇠ 13.35. [DBS2003] 156 and 157 are mutually associated and are members of the Scutum-Crux spiral arm. B 1 2 3 4 [email protected] Universidade Federal da Fronteira Sul Escola de Artes, Ciências e Humanidades, Universidade de São Paulo Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo Laboratório de Análise Numérica e Astrofı́sica, Universidade Federal de Santa Maria 351 ISM Posters ISM -2: #156 Spatial variations of physical and chemical properties of the planetary nebulae NGC 6302 and NGC 2440 Rauber, A. B.B1 ; Copetti, M. V. F.2 ; Krabbe, A. C.3 In this work, we present an analysis of the physical and chemical conditions of the planetary nebulae NGC 6302 and NGC 2440 through spatially resolved spectroscopy. Multiple parallel long-slit spectra were obtained with the Goodman spectrograph attached to the 4.1 m SOAR telescope, allowing the construction of maps and spatial profiles. Densities were estimated from the [S II] and [Ar IV] sensors. For NGC 6302, a peaked distribution was found, with the densest area at the circumstellar region, reaching Ne ⇡ 40000 cm decreasing to Ne  1000 cm 3 at the bipolar lobes. Knots with Ne ⇡ 2000 3000 cm 3 3 and and an inner outflow region were observed. The density maps of NGC 2440 show complex characteristics. In the central structures densities reach more than 4500 cm 3 . Structures with 1000 < Ne < 1500 cm 3 are associated with the bipolar lobes at P.A. ⇡ 60 and P.A. ⇡ 85 . Electron temperatures were estimated from the [N II] and [O III] sensors and homogeneous distributions were found for these objects. The average values of the maps were 12304 K and 17380 K, respectively, for Te (N II) and Te (O III) in NGC 6302. In NGC 2440, these same values were 11273 K and 13722 K, respectively. Small temperature flutuations on the plane of the sky were obtained, with t2s  0.012 for NGC 6302 and t2s  0.017 for NGC 2440. Abundances of N+ , O+ , S+ , O2+ , Ne2+ , Ar3+ relative to H+ were determined from collisionally excited lines, and relative abundances of He+ and He2+ from recombination lines. These ionic abundance maps show significant spatial variations. The highest dispersions relative to the mean ionic abundances were observed for the N+ /H+ , O+ /H+ and S+ /H+ maps, going from 50% to 70%. Regions with marginal evidence of overabundance of N were found. No sign of shock excitation is found for any of the structures of these objects. B 1 2 3 [email protected] Universidade Federal de Santa Maria Universidade Federal de Santa Maria Universidade do Vale do Paraı́ba 352 Posters ISM ISM -2: #157 The Magnetic Field Structure in the Musca Dark Cloud Ribeiro, N. L.B1 ; Magalhães, A. M.1 ; Pereyra, A.2 Our goal is the study of the magnetic field (MF) structure of a pre-collapse structure of the interstellar medium - the Musca Dark Cloud (MDC), a nearby (200-250 pc), large (0.25 x 3 ) filamentary cloud. A description of the MF, together with knowledge on turbulence and gravitational forces, is key to understanding the evolution of interstellar clouds. We have obtained linear polarization measurements in the H band (1.65 µm) with the Brazilian’s 60 cm and 160 cm telescopes located at the OPD observatory. By combining these with our earlier optical observations (Pereyra & Magalhaes 2004), we were able to probe regions denser than what was possible in the optical. Our studies in the optical band showed that the cloud is surrounded by a MF which is well aligned with the projected small axis of the cloud. Our H-band data show in general the same tendency in the inner parts of the MDC. The comparison between the V and H bands allow us to conclude that the same type of grains are polarizing the light throughout the cloud at least up to Av ⇠ 8-9, and that these are the same as those in the general ISM. Utilizing the dispersion of the polarization vectors, we estimated the MF intensity (0.02-0.16 mG) across the cloud. We compared the magnetic and gravitational energies and concluded that Musca is a subcritical cloud. From the structure function of the polarization at the H band, we obtain 0.21-0.29 pc for the range of correlation lengths of the MF in the cloud. B 1 2 [email protected] IAG - University of São Paulo IAC - Spain 353 ISM Posters ISM -2: #158 The Magnetic Field Structure of the Interstellar Medium From the observations Open Clusters Rubinho, M. S.B1 ; Magalhães, A. M.1 This project aims to study the magnetic field of the Galactic diffuse interstellar medium (ISM) using imaging polarimetry data towards Open Clusters. These data are from the Interstellar Polarization Survey, that has been carried out in the LNA. The interstellar polarization toward members of these clusters will show the alignment of the grains in the ISM and hence trace the magnetic field. The study of our clusters at various distances from the Sun will thus probe the magnetic field at various angular scales. The polarization of stars was obtained by imaging polarimetry technique in the V filter, with Tel. 60cm IAG at LNA. For data analysis we used the pccdpack package, developed by our group for the IRAF environment. We show the current state of data reduction, and present results for various directions along the Galactic Plane for clusters with distances ranging between 484pc and 2200pc. B 1 [email protected] IAG-USP 354 Posters ISM ISM -2: #159 Carbon abundances in the disk of NGC300 from faint CII recombination lines Toribio-San Cipriano, L.B1 ; Esteban, C.1 ; Garcı́a-Rojas, J.1 We present the results of deep echelle spectrophotometry for a sample of HII regions in the Scd galaxy NGC300 obtained with the Ultraviolet and Visual Echelle Spectrograph (UVES) at the VLT. The main aim of this study is to detect and measure faint OII and CII recombination lines (RLs) along the disk of NGC300. In fact, we have successfully derived the C++/H+ ratio from the CII 4267A RL along the disk of NGC300. This is a very important result because, although Carbon (C) is the second most abundant heavy-element in the Universe, there are only few C abundance determinations for extragalactic HII regions, and they are mainly derived from UV collisionally excited lines (CELs), which intensity is very much affected by interstellar reddening. A well known, and striking, result is that the abundances obtained from the CII 4267A RL are larger than that obtained from the UV CIII] 1907+09 CELs. C abundance determinations from RLs in extragalactic HII regions, combined with chemical evolution models, may help to clarify which kind of lines -CELs or RLsgive the true abundances. If RLs give the ”real” abundances, it would imply that the actual content of heavy elements in the Universe is two times higher than usually assumed. B 1 [email protected] Instituto de Astrofisica de Canarias, Spain 355 ISM Posters ISM -2: #160 The Discrepant Kinematics of ORLs and CELs in NGC 7009 as a Function of Ionization Structure Richer, M. G.1 ; Georgiev, L.2 ; Arrieta, A.3 ; Torres-Peimbert, S.B2 We present spatially- and velocity-resolved echelle spectroscopy for NGC 7009 obtained with the UVES spectrograph at the European Southern Observatory’s Very Large Telescope. Our objective is to analyze the kinematics of emission lines excited by recombination and collisions with electrons to determine whether similarities or differences could be useful in elucidating the well-known abundance discrepancy derived from them. We construct position-velocity maps for recombination, fluorescence, charge transfer, and collisionallyexcited lines. We find a plasma component emitting in the C II, N II, O II, and Ne II recombination lines whose kinematics are discrepant: They are incompatible with the ionization structure derived from all other evidence and the kinematics derived from all of these lines are unexpectedly very similar. We find direct evidence for a recombination contribution to [N II] 5755. Once taken into account, the electron temperatures from [N II], [O III], and [Ne III] agree at a given position and velocity. The electron densities derived from [O II] and [Ar IV] are consistent with direct imaging and the distribution of hydrogen emission. The kinematics of the C II, N II, O II, and Ne II lines does not coincide with the kinematics of the [O III] and [Ne III] forbidden emission, indicating that there is an additional plasma component to the recombination emission that arises from a different volume from that giving rise to the forbidden emission from the parent ions within NGC 7009. Thus, the chemical abundances derived from either type of line are correct only for the plasma component from which they arise. Apart from [N II] 5755, we find no anomaly with the forbidden lines usually used to determine chemical abundances in ionized nebulae, so the abundances derived from them should be reliable for the medium from which they arise. B 1 2 3 [email protected] Instituto de Astronomı́a - Ensenada, Universidad Nacional Autónoma de México Instituto de Astronomı́a, Universidad Nacional Autónoma de México Universidad Iberoamericana, México 356 Galaxies GAL -1: #161 Stellar feedback from black-hole high-mass X-ray binaries in galaxy formation models Artale, M. C.B1,2 ; Tissera, P. B.1,2 ; Pellizza L. J.1,2 In recent years, many works have suggested the role of black-hole high-mass X-ray binaries (BH-HMXB) as potential sources of heating and reonization of the intergalactic medium, due to the large mean free path of X-ray photons. Furthermore, because of the suggested increase of their production rate and X-ray luminosity with decreasing metallicity, BH-HMXBs could be relevant to explain the thermal and ionization history of the Universe at its early stages. However, observations indicate that a meaningful amount of the energy released by these sources could be deposited in the local interstellar medium, suggesting that BH-HMXB could modify star forming regions on the host galaxy. In this work, we study the kinetic BH-HMXB feedback using hydrodynamical cosmological simulations of galaxy formation which also include SNe feedback. We present preliminary results on how the energy input from BH-HMXBs could change the star formation history of the galaxies over time. B 1 2 [email protected] Instituto de Astronomı́a y Fı́sica del Espacio, C.C. 67 Suc. 28, C1428ZAA Ciudad de Buenos Aires, Argentina Consejo Nacional de Investigaciones Cientı́ficas y Técnicas, Rivadavia 1917, C1033AAJ Ciudad de Buenos Aires, Argentina 357 Galaxies Posters GAL -1: #162 Properties of galaxies in fossil and non-fossil groups from the maxBCG sample Luiz AzanhaB1 ; Robert N. Proctor1 ; Claudia Mendes de Oliveira1 Fossil groups are defined as X-ray bright galaxy groups or clusters with a brightest cluster galaxy that is at least 2 magnitudes brighter than any other galaxy within half the virial radius of the system. The current consensus is that these systems form when dynamical friction causes any massive galaxies in the central regions of the system to spiral inwards and merge with the central galaxy. These systems are therefore expected to be relatively isolated and old. The goal of this project is to build a new sample of fossil group galaxies for statistical studies, from the maxBCG catalogue, as well as a control sample of normal cluster/groups and compare distributions of virial radii, radial velocities and luminosity functions of galaxies in fossil and nonfossil systems. A sample of 2000 groups of the maxBCG sample was analyzed and we found 30 candidate fossil groups. Our results on the comparison of the properties of fossil and non-fossil groups will be presented. B 1 [email protected] IAG-USP 358 Posters Galaxies GAL -1: #163 Dinâmica da Formação de Galáxias com Anel Polar Dino Beghetto JuniorB1 ; Irapuan Rodrigues de Oliveira Filho2 ; Maximilliano Faúndez-Abans3 Apresentamos aqui a fase inicial de um projeto que pretende investigar em detalhe a dinâmica da formação das Galáxias com Anel Polar (PRG, do inglês: ”Polar Ring Galaxy”). Uma PRG é formada por uma galáxia hospedeira do tipo precoce, lenticular ou elı́ptica, rodeada por um anel de gás e estrelas orbitando um plano quase perpendicular com relação ao plano principal da galáxia hospedeira. Discutiremos as principais propriedades dinâmicas desses objetos através de um levantamento bibliográfico com ênfase nos mecanismos propostos para explicar a sua formação. Existem dois principais cenários propostos para a formação de PRGs (BORNAUD; COMBES, 2003): (i) fusão de duas galáxias espirais com discos ortogonais em colisão frontal, e (ii) acréscimo de gás, de uma galáxia doadora para a galáxia hospedeira, durante um encontro próximo. Além desses, também existe o cenário de formação de anel polar por acréscimo de gás dos filamentos cósmicos (MACCIÒ et al, 2005). Em qualquer desses cenários teóricos, os anéis polares se formam por interações entre galáxias ou de uma galáxia com o seu entorno cósmico. Uma evidência disso é que os anéis polares observados parecem sempre mais jovens do que as respectivas galáxias hospedeiras. O objetivo primário deste trabalho é construir uma base de dados de simulações numéricas, buscando evidenciar que parâmetros estão mais diretamente envolvidos na formação das PRGs. Além disso, uma vez construı́da a base de dados, ela será uma ferramenta importante no estudo da dinâmica de PRGs observadas. Depois do processo de formação de uma PRG, quando o anel já se estabilizou, perde-se muito da ”memória” do processo de formação, tornando difı́cil o estudo da sua história dinâmica. Os resultados observacionais obtidos para uma PRG em estudo poderão ser confrontados com as simulações da base de dados e, a partir da análise do ”best match”, sua dinâmica atual e pregressa poderão ser investigadas. B 1 2 3 [email protected] IPD-UNIVAP IPD-UNIVAP LNA/MCTI 359 Galaxies Posters GAL -1: #164 Metal-Poor Active Galactic Nuclei Bicalho, I. C.B1 ; Telles, E.1 ; Thuan, T.2 ; Izotov, Y3 Active galaxies are considered to be metal-rich, with metallicity ranging from solar to slightly supersolar. This is due to the fact that the active galaxy nuclei are usually found in massive galaxies. We present the results based on analysis of data from Gemini Near Infrared Integral Field Spectrograph (NIFS+ALTAIR) of the metal-poor HII galaxy SDSS J1047+0739. We aim to test the hypothesis of the presence of an AGN in low metallicity dwarf galaxies that show strong permitted emission lines with extended wings, which is atypical for HII regions. We also use unconventional methods such as PCA tomography due to the benefits that it provides to data analysis. We are studying the kinematics of the nuclear region and the regions of star formation surrounding it, mostly through the Paschen-alpha and [He] lines. After a throughout discussion on the question of effective resolution of our observations provided by the point spread function (PSF) with the adaptive optics system, we find that the broad line emission comes only from the unresolved central region, consistent with the presence of an AGN in this metal-poor galaxy. B 1 2 3 [email protected] Observatório Nacional, Rio de Janeiro-RJ Astronomy Department, University of Virginia, Charlottesville - Virginia - USA Main Astronomical Observatory, Ukrainian National Academy of Sciences, Kyiv - Ukraine 360 Posters Galaxies GAL -1: #165 Analysis of the Velocity Data of Cluster A562 Calderón Espinoza, D.B1 ; Gomez, P.2 We present a study of the velocity of the cluster of galaxies Abell 562 to understand the physical mechanism that produces the bending in the radio jets of the central elliptical galaxy of the cluster. We test if the ram pressure between the central radio source and the intracluster medium (ICM) is a good explanation for the phenomenom. To do this we used Gemini North Multi-Object Spectroscopy data from the members of the cluster, finding that the central galaxy does not have enough relative velocity for bending its jets by ram pressure. But from the analysis of the velocity distribution we found a substructure that suggests a merger. B 1 2 [email protected] Departamento de Astronomı́a y Astrofı́sica, Pontificia Universidad Católica de Chile Gemini South Observatory 361 Galaxies Posters GAL -1: #166 Internal kinematics of HII galaxies Carvalho, M.B1 ; Plana, H.1 H II galaxies are dwarf galaxies caracterized by high stellar formation rate with spectrum dominated by strong emission lines, superimposed on a weak stellar continuum. The study of internal kinematics of these objects may be realized using the observed emission lines. Based on these lines we obtained monochromatic intensity, velocity dispersion and radial velocity maps. We have studied the internal kinematics of two H II galaxies: UM 461 and CTS 1020, observed with the Gemini South telescope using the GMOS instrument equiped with an IFU. We aim to investigate the origin of the line-broadening observed on emission lines from the use of kinematics diagnostic diagrams: I vs , I vs V , e V vs . The analysis of these diagrams was based on the Cometary Stirring Model that allows us to identify, for example, the presence of expanding shells and stellar winds. We found that radial velocity and velocity dispersion maps, for each galaxy, show a different kinematical pattern, although both are H II galaxies. CTS 1020 shows a velocity gradient consistent with a rotating disc with a velocity amplitude of ⇠50 km s 1 . On the other hand UM 461 does not exhibit a typical pattern of a rotating system, despite of the observed velocity gradient in both emission nuclei, but shows signs of an expanding shell. We also perform, for both galaxies, a PCA analysis of the data cubes, showing much weaker lines such as: He I 4471Å, [OI]6300Åand [SIII]6312Å. B 1 [email protected] Laboratorio de Astrofisica Teorica e Observacional - UESC - Ilheus - Brazil 362 Posters Galaxies GAL -1: #167 Dynamical Analyses of z= 0.3, 0.5 Galaxy Clusters from the SOAR Gravitational Arcs Survey Cibirka, N.B1 ; Cypriano, E.1 ; Caminha, G.2 ; Makler, M.2 We have performed dynamical analyses of galaxy clusters using optical spectroscopic data. These clusters belong to the SOAR Gravitational Arcs Survey (SOGRAS) (Furlanetto et al. 2013) and are among the richest structures in SDSS stripe 82 with redshifts around z= 0.3 or z= 0.5. For three of those clusters, all with strong lensing features, we carried out individual analysis using Gemini/GMOS data (⇠ 25 velocities per cluster). We obtained masses in the range of 3 8 1014 M and signs of substructure in one of them. For the whole SOGRAS sample (47 clusters) we used SDSS spectroscopic data. Given the low number of velocities per clusters, we stacked the data per redshift and/or richness. Our results indicate that the richest half of the clusters, independently of the redshift, tend to be ⇠ 2.5 times more massive than the poorest half. Also we have found that the z= 0.3 and the z= 0.5 clusters have overall masses statistically consistent with each other: 6.3(+3.9 B 1 2 2.1) and 8.6(+5.2 1.6)1014 M respectively. [email protected] Instituto de Astronomia, geofı́sica e Ciências Atmosféricas, Universidade de São Paulo Centro Brasileiro de Pesquisas Fı́sicas 363 Galaxies Posters GAL -1: #168 The connection between the origins of globular clusters and the evolution of their host galaxy Arianna CortesiB1 ; Ana Chies-Santos1 ; Steven Bamford1 ; Michael Merrifield1 ; Aaron Romanowsky2 ; Jacob Arnold2 ; Vincenzo Pota3 ; Duncan Forbes3 ; Lodovico Coccato4 ; J. P. Brodie2 ; Chris Usher3 ; Jay Strader5 ; Caroline Foster6 Star kinematics is directly connected to the evolution history of their host galaxy. However, to recover the correct kinematics, it is necessary to assign each tracer of the starlight to the galaxy component it belongs to: the disk (thin or thick) or the spheroid. Performing a multi-band decomposition of infrared images of our test case NGC 3115, using MegaMorph, and planetary nebulae (PNe) as tracers of the overall stellar populations, we recovered the velocity and velocity dispersion of the thick disk and of the spheroid. We then studied the globular cluster (GC) population in NGC 3115. Given a GC position and velocity we can estimate its probability of belonging to the disk, to the spheroid and in general to the system. We find that most GCs are consistent of being drawn from the light weighted velocity distribution of NGC 3115 stars. Nearly half of the GCs belong to the disk and half to the spheroid, but we don’t find any trend between their colour (B-R) or calcium triplet abundances with their kinematics. In this talk I will explore different formation scenarios that can accommodate our findings. B 1 2 3 4 5 6 [email protected] School of Physics and Astronomy, University of Nottingham, University Park, Nottingham NG7 2RD University of California Observatories, Santa Cruz, CA 95064, USA Centre for Astrophysics & Supercomputing, Swinburne University, Hawthorn VIC 3122, Australia European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany Michigan State University Australian Astronomical Observatory 364 Posters Galaxies GAL -1: #169 The evolution of galaxies between 0.05 < z < 0.8 Costa-Duarte, M. V.B1 ; Stasinska, G.2 ; Sodré Jr., L.1 ; Cid Fernandes R.3 Nowadays several surveys provide databases of thousands of galaxy spectra which allow us to investigate the evolution of galaxies. From the shape of the continuum and from the information encoded in the absorption and emission lines it is possible to recover the star formation history of the galaxies and investigate their nuclear activity. We have studied the evolution of galaxies in the redshift range 0.05< z <0.85 by considering spectra from the SDSS/DR7 and zCOSMOS surveys. We distinguished the galaxies by their stellar masses and for each mass and metallicity bin we obtained a representative spectrum by stacking all the relevant spectra. We see regular trends in the galaxy properties both as a function of stellar mass and of redshift. Using spectral synthesis we confirm the downsizing scenario, i.e., more massive galaxies present older stellar populations. Massive galaxies are already formed at z=0.85 while less massive objects are still forming stars. We also study the evolution of galaxies of different masses in emission-line diagnostic diagrams, and discuss how the proportion of galaxies of different types, i.e. pure star-forming, galaxies containing an active nucleus, and retired galaxies (galaxies that have stopped forming stars), evolve as a function of redshift for different mass bins. B 1 2 3 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas - Universidade de São Paulo Observatoire de Paris - Meudon - Paris - France Universidade Federal de Santa Catarina 365 Galaxies Posters GAL -2: #170 Galaxy Concentration Index in Low X-ray Luminosity Galaxy Clusters Cuevas, H.B1 ; Nilo Castellón, J. L.1 ; Alonso, M. V.2 Using a sample of 10 low x-ray luminosity galaxy clusters (Nilo Castellón et al. 2013B), we studied the properties of 146 galaxies classified as members in a redshift range of 0.185 < z < 0.701. Following Concelice et al. 2000, we define the galaxy concentration index (C), as the ratio of two circular radii which contain 80 and 20 percent of the total Petrosian flux. Mainly, we observed an increment of C for early-type and lenticular galaxies at redshifts lower than 0.3, that can be related to the presence of giant galaxies in these low redshift clusters (C > 4). Contrary to these results, for late-type galaxies we found smaller C values for the lower redshift clusters. These results could be associated to the morphological evolution of galaxies, as proposed by different authors (Poggianti et al. 2009, Dressler et al. 2009) for rich clusters. B 1 2 [email protected] Departamento de Fı́sica, Universidad de La Serena, Chile Instituto de Astronomı́a Teórica y Experimental (IATE-CONICET), Argentina 366 Posters Galaxies GAL -2: #171 Probing the Spacial Distribution of the Near-infrared Stellar Population in Starburst Galaxies N. Z. DamettoB1 ; R. Riffel1 ; M. G. Pastoriza1 ; A. Rodrı́guez-Ardila2 ; E. A. Carvalho2,3 ; J. A. Hernandez-Jimenez1 In this work we employ Infrared Telescope Facility SpeX near-infrared (0.8-2.4µm) spectroscopy to investigate the spatial variation of the stellar populations in four well known Starburst galaxies: NGC 34, NGC 1614, NGC 3310 and NGC 7714. We use the STARLIGHT code, updated with the synthetic simple stellar populations models computed by Maraston 2005, to fit combinations of stellar population models of various ages and metallicities. Our main results are that the near-infrared light in the central region of the galaxies is dominated by intermediate-age stars (1 ⇥ 108  t  2 ⇥ 109 Gyr), summing ⇠50% of the light, followed by a secundary contribution of a young stellar population. The only case ruling this out is NGC 34, which shows a predomiance of a young age (t  50 ⇥ 106 Myr) stellar population in the nuclear surroundings (60 %). We found evidence of a circumnuclear star formation ring-like structure with young/intermediate- age star in NGC 1614, in agreement with previous studies. Also, we conclude that the metallicity traces the intermediate-age stellar population in almost all the sources. The reddening is nearly constant along the whole galaxy in the four cases. B 1 2 3 [email protected] Departamento de Astronomia, Universidade Federal do Rio Grande do Sul Laboratório Nacional de Astrofı́sica/MCTI Campus São João Del Rei, Instituto Federal do Sudeste de Minas 367 Galaxies Posters GAL -2: #172 The relation between the spectral synthesis of galaxies in the visible region and their UV emission Dantas, M. L.B1 ; Sodré Jr., L.1 Under the STARLIGHT Project, almost a million spectra, which were extracted from the Sloan Digital Sky Survey (SDSS), were analyzed with the empirical spectral synthesis approach described by Cid Fernandes et al. (2005). The spectral synthesis involves the fitting of the optical spectrum of a certain galaxy based on the spectral database of Bruzual & Charlot (2003). It also considers the reddening caused by dust and the spectral line widening caused by the Doppler Effect due to the motion of the stars within the galaxy. Since the model that best fits the optical region can also be extended to the ultraviolet, we have compared our predictions to the UV photometry of the same galaxies mesured by the GALEX satellite, studying the systematics and nature of the differences. The main motivation of this study is to obtain realistic spectral models from the UV to the optical region for the study of high redshift galaxies. B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas da USP 368 Posters Galaxies GAL -2: #173 Resolving galaxies in time and space: Applying STARLIGHT to CALIFA data cubes de Amorim, A. L.B1 ; Cid Fernandes, R.1,2 ; Perez, E.2 ; Garcia Benito, R.2 ; González Delgado, R. M.2 ; Sanchez, S. F.2, 3 ; Husemann, B.4 ; Falcon Barroso, J.5,6 ; Sanchez-Blazquez, P.7 ; Walcher C. J.4 ; Mast D.2,3 Fossil record methods based on spectral synthesis techniques have matured over the past decade, and their application to integrated galaxy spectra fostered substantial advances on the understanding of galaxies and their evolution. Yet, because of the lack of spatial resolution, these studies are limited to a global view, providing no information about the internal physics of galaxies.Motivated by the CALIFA survey, which is gathering Integral Field Spectroscopy over the full optical extent of 600 galaxies, we have developed an end-to-end pipeline which: (i) partitions the observed data cube into Voronoi zones in order to, when necessary and taking due account of correlated errors, increase the S/N, (ii) extracts spectra, including propagated errors and bad-pixel flags, (iii) feeds the spectra into the STARLIGHT spectral synthesis code, (iv) packs the results for all galaxy zones into a single file, (v) performs a series of post-processing operations, including zone-to-pixel image reconstruction and unpacking the spectral and stellar population properties into multi-dimensional time, metallicity, and spatial coordinates.This work provides a description of this whole pipeline and its data products. These include 3D cubes of the stellar formation history, 2D maps of galaxy properties such as the v-field, stellar extinction, mean ages and metallicities, mass surface densities, star formation rates on different time scales and normalized in different ways, 1D averages in the temporal and spatial dimensions, projections of the stellar light and mass growth (x,y,t) cubes onto radius-age diagrams, etc. The results illustrate the richness of the combination of IFS data with spectral synthesis, providing a glimpse of what is to come from CALIFA and future IFS surveys. B 1 2 3 4 5 6 7 [email protected] Universidade Federal de Santa Catarina Instituto de Astrofı́sica de Andalucı́a Centro Astronómico Hispano Alemán, Calar Alto Leibniz-Institut für Astrophysik Potsdam Instituto de Astrofı́sica de Canarias Universidad de La Laguna, Tenerife Universidad Autónoma de Madrid 369 Galaxies Posters GAL -2: #174 Detection and modelling of star cluster early phases in grand-design, spiral galaxies Grosbol, P.1 ; Dottori, H.B2 Deep, near-infrared maps in ZJHK-maps for ten nearby, grand-design, spiral galaxies using HAWK-I at the ESO Very Large Telescope, allowed to obtain a complete, magnitude-limited list of candidates of star-forming complexes searching within the K-band maps. The detection of thousands of candidates per galaxy enables a good statistic treatment of the data. Our analysis indicates that cluster younger than 7 Myr have significant internal extinction AV =3-7 mg, while for the older ones AV ' 1m .0. The cluster luminosity function is well fitted by a power law with exponential around 2 and does not show evidence of high luminosity cut-off. The brightest cluster complexes reach luminosities MK =-15m .5 with estimated masses of 106 M . The CLF in the arms is also shifted towards brighter MK by at least 0m .4. At the two-armed spiral pattern the star formation rate is higher by a factor of 2-5 than in the inter-arm regions. The (J-K) vs MK diagram of several galaxies shows, for the brightest clusters, a clear separation between young clusters that are highly attenuated by dust and older ones with low extinction. Monte Carlo simulations of cluster populations were performed using the power-law distribution function g(M, ⌧ ) / M ↵ ⌧ . Integrated colors were computed from Starburst99 models. The derived near-infrared color-magnitude diagrams were compared to those observed for 6 granddesign, spiral galaxies using statistical tests for goodness-of-fit. The color-magnitude distributions indicate a significant mortality of young, massive clusters with = -1.1±0.3. High initial extinction AV = 8-11 and strong nebular emission are required to reproduce the bi-modal color distributions of the clusters. An extended star formation phase of more than 5 Myr is suggested during which the extinction starts to decrease over a period of 5-10 Myr. B 1 2 [email protected] European Southern Observatory, K. Schwarschild Str. 2, Garching b. München Instituto de Fı́sica, UFRGS, Brazil 370 Posters Galaxies GAL -2: #175 Two-dimensional Stellar Kinematics and Dynamical Models for NGC 4258 and NGC 1052 Drehmer, D. A.B1 ; Storchi-Bergmann, T.1 ; Ferrari, F.2 ; Riffel, R. A.3 In this work we present a two-dimensional mapping of the stellar kinematics of the inner 300 ⇥300 region of the galaxies NGC 4258 and NGC 1052, derived from spectroscopic observations with the Near-Infrared Integral Field Spectrometer (NIFS) at the GEMINI North Telescope. For NGC 4258, the velocity distribution is dominated by a strong velocity dispersion gradient, requiring the presence of a Supermassive Black-Hole (SMBH) there. Assuming that the distribution function (DF) depends on three integrals of motion, we constructed a Jeans Anisotropic Model to fit the observed velocity distribution. Our dynamical model assumes that the galaxy has axial symmetry and uses the Multi-Gaussian Expansion (MGE) method to parametrize the observed surface brightness distribution. The model has three free parameters: the mass of the central SMBH (M• ), the mass-luminosity ratio (M/L) of the galaxy and the anisotropy in the velocity distribution. Modeling the kinematics of the galaxy without considering the contribution of the SMBH, we obtain a velocity profile dominated by rotation. By adding the contribution of a central SMBH, and systematically increasing the value of its mass, the modeled velocities increase considerably in the central region, passing from a velocity field dominated by rotation to one dominated by velocity dispersion in the innermost region, consistent with the observations. From the best-fitting model, we obtain the values for the free parameters which best reproduce the observed kinematics. After testing the reliability of our model on NGC 4258 (which has already a well determined value for M• ), we apply the same procedure to model the stellar kinematics of NGC 1052, and determine the mass of the SMBH at the nucleus. B 1 2 3 [email protected] Universidade Federal do Rio Grande do Sul Universidade Federal de Rio Grande Universidade Federal de Santa Maria 371 Galaxies Posters GAL -2: #176 Open Cluster Radial Velocity determination from observations at Observatório Pico Dos Dias Faria, M. A. F.B1 ; Monteiro, H.1 ; Dias, W. S.2 ; Lépine, J. R. D.3 In studies of the dynamics of the Galactic disk, such as the determination of the speed of the spiral pattern and the permanence of stars in the spiral arms, it is crucial to know orbits obtained from proper motions, radial velocities and the potential of the Galaxy. Aiming to improve the statistics of our catalog of open clusters, maintained by our research group, we determined the radial velocity of stars belonging to a group of open clusters using spectra with a resolution of 4000, obtained at the Pico dos Dias Observatory (LNA) with the 1.60 m telescope and the Coudé spectrograph. We observed the open cluster’s member stars and calculated their radial speeds using standard techniques. The stars were selected from our own database based on relevant information concerning the clusters, obtained by statistical analysis of their proper motions and/or their position in the HR’s diagram. In this work, we present the detailed analysis of the data reduction and radial velocity determination using synthetic spectra from different libraries. Finally we present the open cluster’s radial (and spacial) velocities. B 1 2 [email protected] Universidade Federal de Itajubá Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas 372 Posters Galaxies GAL -2: #177 Effects of dark matter and energy on the chemical enrichment of Dwarf Spheroidal Galaxies Ferle, O. L.B1 ; Lanfranchi, G. A.1 We analyse several physical processes that may play important roles in the chemical enrichment and evolution of dwarf spheroidal galaxies by means of a detailed chemical evolution models and from results of hydrodynamical simulation of dwarf galaxies. We adopted several different scenarios for the evolution of the dwarf spheroidal galaxies by varying the prescriptions in the chemical evolution code for the mass and distribution of dark matter, the star formation history and rate, and the energetic interaction among dark matter, luminous matter, and gas. The adopted prescriptions are based on the results of the numerical simulations of the hydrodynamics of the gas content of the system. For each adopted scenario, the predictions of the chemical evolution models are analysed and compared to the data. The occurrence and intensity of galactic winds and their effect in the chemical properties are investigated by comparing the predictions with observed data. B 1 [email protected] NAT - Universidade Cruzeiro do Sul, Brasil 373 Galaxies Posters GAL -2: #178 The effects of the interaction on the kinematics and abundance of AM 2229-735 P. Freitas-LemesB1 ; I. Rodrigues1 ; O. L. Dors Jr.1 ; M. Faúndez-Abans2 ; E. Pérez-Montero3 We present an observational study of the effects of the interaction on the kinematics and chemical abundance of the component galaxies of AM 2229-735. This system is formed by a disk galaxy, NED01, and a compact perturbed Sb(s)-like galaxy, NED02, the later showing a tail and counter-tail arc-shaped feature. The sky projected tail is very luminous and seems to connect the galaxies. Our study was based on BVRI broad band imagery as well as longslit spectroscopy in the wavelength range 4100-8600Å, performed at the 1.6m telescope at the Observatório do Pico dos Dias (OPD), Brazil. We have estimated heliocentric radial velocities of 17 518±25 km/s (NED01) and 17 326±27 km/s (NED02). Standard diagnostic diagrams were used to classify the main ionizing source of selected emission-line regions. It turns out that all regions are mainly ionized by massive stars. Using two empirical methods, we found that the H II regions in AM 2229-735 have high metallicity: 12+log(O/H)=8.3-8.6 dex. B 1 2 3 [email protected] Universidade do Vale do Paraı́ba. Av. Shishima Hifumi, 2911, CEP: 12.244-000, São José dos Campos, SP, Brazil MCT/Laboratório Nacional de Astrofı́sica, Caixa Postal 21, CEP:37.504-364, Itajubá, MG, Brazil Instituto de Astrofisı́ca de Andalucı́a, CSIC, Apartado de correos 3004, 18080 Granada, Spain. 374 Posters Galaxies GAL -3: #179 Low surface brightness galaxies and void walls B1 Gaspar Galaz ; Laura Ceccarelli2 ; Rodrigo Herrera-Camus3 ; Nelson Padilla1 ; Diego Garcia-Lambas2 We present new results showing that low surface brightness galaxies (LSB) populate in significant larger fraction the walls which define the large scale structure voids in the cosmic web. Results were obtained using data from the Sloan digital sky survey, and combined with simulations for analysis. Moreover, our results show that at some poinf LSBs in void walls eventually evolve to high surface brightness galaxies. B 1 2 3 [email protected] Instituto de Astrofı́sica, P. Universidad católica de Chile Observatorio Nacional de Córdoba Universityvof Maryland 375 Galaxies Posters GAL -3: #180 Rotation effects on the Lyman-alpha line morphology in distant galaxies Garavito-Camargo, N.B1 ; Forero-Romero, J. E.1 ; Dijkstra, M.2 Rotation is present in the gas kinematics of galaxies up to the highest redshifts. In this talk we present for the first time radiative transfer calculations that show the impact of rotation on the morphology of the Lyman ↵ line. To this end we construct simplified models where a galaxy is modeled as an homogeneous sphere composed as an homogeneous mixture of dust and hydrogen at a constant temperature. These spheres have a solid-body rotation with linear velocities at the surface in the range 0 300 km s 1 . We consider radiation sources both in the center of the rotating cloud and also homogeneously distributed around the sphere. We find that higher rotational velocities increase the width of each peak in the outgoing line profile while it also increases the amount of Lyman alpha photons escaping in the line center. This trends makes that for high rotational velocities and large Hydrogen optical depths the double peak of the line tends to be erased an be replaced by a single peak the lines center. This is more pronounced for radiation sources homogeneously distributed. Concerning the escape fraction we find that rotation does not have any effect, provided that all the sources are centrally emitted. However in the case of homogeneously emitted sources we measure an increase of about a factor of 2 in the escape fraction for higher rotational velocity values. Our work shows clearly that gas rotation has a non negligible impact on the shape of the Lyman ↵ line. B 1 2 [email protected] Departamento de Fı́sica, Universidad de los Andes, Bogotá, Colombia Institute for theoretical astrophysics, University of Oslo 376 Posters Galaxies GAL -3: #181 Visualizing VVV catalogue and image data Gurovich, SebastianB1,2 ; Samual Skillmann3 We are exploring python community-based methods to visualize multi-epoch data from the Vista Variables in the Via Lactea Survey. Our efforts include use of the python YT and astropy modules to detect and characterize moving objects in the ecliptic as well as the light curve of periodic variables. B 1 2 3 [email protected] Observatório Astronómico de Córdoba, Universidad Nacional de Córdoba, Laprida 854, x5000 BGR, Córdoba, Argentina Instituto de Astronomı́a Teórica y Experimental, CONICET, Laprida 922, 5000, Córdoba, Argentina Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO, USA 377 Galaxies Posters GAL -3: #182 Photometry and Dynamics of the Minor Merger AM 1219-430 with Gemini/GMOS-S Hernandez-Jimenez, J. A.B1 ; Pastoriza, M. G.1 ; Rodrigues I.3 ; Krabbe, A. C.3 ; Winge, C.5 ; Bonatto, C.1 We present an observational study of the interaction effect on the dynamics and morphology of the minor merger AM 1219-430. This work is based on r0 and g 0 images and long-slit spectra obtained with the Gemini Multi-Object Spectrograph at the Gemini South Telescope. We detected a tidal tail in the main galaxy (AM 1219A) and a bridge of material connecting the galaxies. On the other hand, the secondary galaxy (AM 1219B) shows prominent symmetric tidal tails. We separated the two-fold symmetric and the nonsymmetric parts of the galaxies by performing successive image rotations and subtractions. The symmetric images, obtained by subtracting the asymmetric one from the observed image, show the “original” disk and the non-perturbed spiral pattern. The overall geometrical parameters of the galaxies, such as inclination and position angle of the line-of-nodes, were obtained from the photometric analysis of the symmetrized g0 and r0 images. The surface brightness profile of AM 1219A was decomposed into bulge and disk components. The profile shows a light excess of ⇠ 53% due to the contribution of star-forming regions, which is typical of starburst galaxies. On the other hand, the surface brightness profile of AM 1219B shows a lens structure in addition to the bulge and disk. The scale lengths and central magnitudes of the disk structure of both galaxies agree with the average values derived for galaxies with no sign of ongoing interaction or disturbed morphology. The Sérsic index (n < 2), the effective and scale radii of the bulge of both galaxies are typical of pseudo-bulges. The rotation curve of AM 1219A derived from the emission line of ionized gas is quite asymmetric, suggesting a gas perturbed by interaction. The overall best-fitting solution for the mass distribution +0.3 of AM 1219A was found with M/L for bulge and disk of ⌥b = 2.8+0.4 0.4 and ⌥d = 2.4 0.2 , respectively, and a +1.2 12 Navarro, Frenk & White profile of M200 = 2.0+0.5 0.4 ⇥ 10 M and c = 16.0 1.1 . B 1 2 3 [email protected] Instituto de Fı́sica, Universidade Federal do Rio Grande do Sul, Porto Alegre, RS, Brazil Universidade do Vale do ParaÍba, São José dos Campos, SP, Brazil Gemini Observatory, La Serena, Chile 378 Posters Galaxies GAL -3: #183 Physical properties of galaxies in the Sloan Digital Sky Survey detected in infrared Herpich, F. R.B1 ; Mateus, A.1 ; Cid Fernandes, R.1 ; Lacerda, E. A.1 ; de Amorim, A. L.1 ; Rossi, L. L.2 ; Cendron, M. M2 ; Klein, V. B.2 ; Crestani, T.2 ; Parize, M. M.2 ; Braz, F. J.3 The extragalactic astrophysics is experiencing a golden age with the availability of an almost inconceivable amount of observational data and projects in different spectral regions. Our research group at UFSC, in collaboration with other researchers from Brazil and France, was successful in following these new challenges, especially with the spectroscopic analysis of the SDSS data. The result of this effort was to build a database of physical properties of galaxies to nearly 1 million objects, which is completely public. Recently we also started analyzing data from the GALEX ultraviolet, spectral broadening our coverage. In this work, we continue this expansion, focusing our attention in the infrared region of the electromagnetic spectrum with the inclusion of font catalogs obtained a recently mission, the WISE project. We increase our database with the data obtained from the WISE and made the match in the catalog of creating a subsample of SDSS galaxies about 300 000 objects. These objects are analyzed using a new computational tools in order to identify the properties in the infrared. This is done in conjunction with the Department of Computer Science of Santa Catarina Federal Institute. In the first analysis, we obtain a clear separation between star forming galaxies (SF) and “retired” galaxies (RT). In this work, we present the latest results of the analysis of this data. B 1 2 3 [email protected] Universidade Federal de Santa Catarina - UFSC Instituto Federal Catarinsense, campus Videira Instituto Federal Catarinense, campus Araquari 379 Galaxies Posters GAL -3: #184 SFR in dwarf spiral galaxies Hidalgo-Gàmez, A. M.B1 ; Vega-Acevedo, I.1 ; Magaña-Serrano, M. A.1 In this investigation the SFR of a sample of 15 dwarf spiral galaxies (dS) is studied. They were obtained from H↵ images from the 1.5m telescope at OAN-SPM (Mexico). The SFR values obtained for the dS galaxies, of the order of 0.01 M yr 1 , are lower than for earlier spirals (e.g. Sd), being closer to those of irregular galaxies. A study of the SFR vs. the gas mass density, as well as vs. the number of H II regions, the size of the largest region, and the chemical abundance have been perfomed for the dS galaxies and it was compared with the results for some other spiral galaxies. It is very interesting that, although one might think that dS are just small, late-type, spiral galaxies they do not follow the trends of the other spirals. Neither they follow the trend for irregular galaxies. Therefore, it might be considered as an intermediate type between the large Sd-Sm galaxies and the irregular ones. B 1 [email protected] Escuela Superior de Fisica y Matemáticas, IPN, México 380 Posters Galaxies GAL -3: #186 E+A galaxies in SDSS. Stellar population and morphology Rodrigo LeivaB1 A sample of E+A galaxies from SDSS DR7 is selected by having a strong H absorption line and few H↵ and [OII] emission lines. The morphology and star formation history are studied. Visual classification and photometric light profile criteria are used as complementary approaches to determine the morphology using for the first the results from volunteer based classification project Galaxy Zoo 1. Also automatic light profile parameter determination published in SDSS are used as alternative approach. With the premise that E+A are post-starburst (PSB) galaxies, star formation history is studied fitting synthetic spectra using Galaxev. Each galaxy is fitted with two populations, an old composite stellar population and a recent single stellar population. This simple fit is compared with the PSB hypothesis and compared with the more sophisticated fit from VESPA where a complete star formation history is determined. B 1 [email protected] Instituto de Astrofı́sica, Pontificia Universidad Católica de Chile 381 Galaxies Posters GAL -3: #187 High-redshift translucent clouds: detection of neutral species in QSO absorbers López P.B1 ; López S.1 ; Sánchez P.1 We analyze a sub-sample of high-redshift Mg II absorption systems drawn from a sample of 900 MgII systems detected in the ESO archive of VLT/UVES QSO spectra. In these particular systems we find absorption due to Si I, Ca I, Fe I and other neutral species. The presence of such neutral species is not common, given their low ionization potential, and suggests that the clouds are shielded from ionizing photons. Thus, these cold neutral clouds could be the high-redshift precursors of the molecular clouds, where stars are born. B 1 [email protected] Universidad de Chile 382 Posters Galaxies GAL -4: #188 SFH of galaxies using spectroscopy in the optical range of the CALIFA sample and ultraviolet photometry of the GALEX mission López-Fernández, R.B1 ; González Delgado, R. M.1 ; Cid Fernandes, R.2 ; Pérez, E.1 ; Garcı́a Benito, R.1 Why study the stellar populations? Different evolutionary processes leave a different fossil record in the stellar population properties of galaxies. A very powerful method to study the formation and evolution of galaxies is to reconstruct the star formation history through the properties of stars that form them. Currently is used the evolutionary synthesis technique to infer the properties of the stellar population through the integrated light of all the stars, assuming an initial mass function (IMF) and a star formation rate. To analyze the data we use the code STARLIGHT. The spectral range of the CALIFA sample is ideal for the study of stellar populations, as it contains the lines of the Balmer series and the Balmer jump. However, the method can present age-metallicity-extinction degenerations, producing uncertainties in determining the physical properties of the stellar population characteristics. So we combine CALIFA spectroscopic data with photometric data in the ultraviolet range obtained with the GALEX mission in order to break these degeneracies, including data that provide additional information about the young stellar populations, which contribute to a lesser extent in the optical range. B 1 2 [email protected] Instituto de Astrofı́sica de Andalucı́a (CSIC), Camino Bajo de Huétor s/n Aptdo. 3004, E18080-Granada, Spain Departamento de Fı́sica, Universidade Federal de Santa Catarina, P.O. Box 476, 88040-900, Florianópolis, SC, Brazil 383 Galaxies Posters GAL -4: #189 The distribution of stellar populations within galaxies Martins-Novais, P.B1 ; Sodré Jr., L.1 The study of stellar populations in galaxies is particularly interesting, since they are a fossil record of several physical processes associated with the formation and evolution of galaxies. In this work we present the first results of our approach to study the spatial distribution of stellar populations inside galaxies. We are using ugriz magnitudes and principal component analysis (PCA) to obtain pixel-by-pixel proxies of the stellar populations and their distributions inside each galaxy. The distribution of these populations are then investigated with a variety of statistical tools, including Gini Indices and the Euler-Poincaré characteristic. This approach is a step forward the conventional profile fitting and allows to obtain quantitative estimates on how the different stellar populations are distributed within a galaxy, bringing hints on how galaxies grow and evolve. B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas. IAG/USP 384 Posters Galaxies GAL -4: #190 The environmental properties of galaxies probed by marked statistics Mateus, A.B1 Galaxies are generally treated as point particles in clustering analysis. However, these objects have physical and stellar population properties that must be taken into account if one wants to study the environmental effects on galaxy evolution. In this work, we apply a statistical method to investigate the role of environment in driving galaxy properties based on the marked correlation function. This methodology was applied for galaxy samples drawn from the Sloan Digital Sky Survey (SDSS) Data Release 7 and from the Wide-field Infrared Survey Explorer (WISE). Our main aim is to reproduce environmental relations among galaxy properties for galaxy catalogues based purely on photometric data, evaluating the effects of errors in photometric redshift estimations on analysis involving galaxy environment. We show that marked statistics are powerful to reproduce environmental trends for variables like luminosities, star formation rates and mean stellar ages, as well as to quantify the relative importance of them with respect to the environment. B 1 [email protected] Universidade Federal de Santa Catarina, Brazil 385 Galaxies Posters GAL -4: #191 Submillimeter Galaxy Number Counts in a Semi-analytic Model: the ”Count Matching” Approach Muñoz Arancibia, A. M.B1 ; Navarrete, F.2 ; Padilla, N.1,3 ; Cora, S.4,5 ; Gawiser, E.6 ; Kurczynski, P.6 ; Ruiz, A.7 Fitting submillimeter galaxies (SMGs) into the current theory of galaxy formation has been a challenge since their discovery, even though they are the most luminous star-forming sources at the epoch where galaxy formation peaks. Recent ALMA observations of the Extended Chandra Deep Field South (for which LABOCA detections are available) show that the bright end of the LABOCA number counts is actually comprised by emission from multiple fainter sources, given the high sensitivity and resolution of ALMA maps compared to LABOCA. With the aim of exploring the properties of SMGs, and in analogy to the now-standard abundance matching approach, we perform a ”Count Matching” approach through lightcones drawn from a semi-analytic model. We choose various physical galaxy properties given by the model as proxies for their submillimeter fluxes, assuming a monotonic relationship so that the combined LABOCA plus bright-end ALMA observed number counts are reproduced. After turning the catalogs of galaxy positions and fluxes given by the different proxies into submillimeter maps that include a modeling of the observational process, we perform a source extraction as done for maps obtained through observations. With this we study the effects of the observational process in the recovered counts, as well as the galaxy properties derived from the detected sources for each proxy. The difference between the counts with and without the beam of LABOCA can be used to find the best proxy: sources with the highest submm fluxes will have different clustering depending on the assumed proxy, since the sources with the highest value of a given property will be clustered in a particular way; the best proxy then will be such that the clustering measured from the model galaxies is the same that the one given by the ALMA sources, while the recovered clustering from the simulated maps is the same that the one given by the LABOCA SMGs. This can also be confirmed exploring other statistics like redshift, stellar mass and host halo mass distributions. B 1 2 3 4 5 6 7 [email protected] Departamento de Astronomı́a y Astrofı́sica, Pontificia Universidad Católica de Chile Max-Planck-Institut für Radioastronomie Centro de Astro-Ingenierı́a, Pontificia Universidad Católica de Chile Consejo Nacional de Investigaciones Cientı́ficas y Técnicas de Argentina Facultad de Ciencias Astronómicas y Geofı́sicas, Universidad Nacional de La Plata, e Instituto de Astrofı́sica de La Plata Department of Physics and Astronomy, Rutgers Observatorio Astronómico de Córdoba, Universidad Nacional de Córdoba 386 Posters Galaxies GAL -4: #192 Properties of Galaxies and Groups at z < 1.4 Nascimento, R. S.B1 ; Lopes, P. A. A.1 ; Ribeiro, A. L. B.2 In this work, we analyse a sample of galaxy groups constructed from the fourth data release of the Deep Extragalactic Evolutionary Probe 2 (DEEP2) including the Extended Groth Strip (EGS). This sample was obtained by Gerke et al. (2012) using the Voronoi-Delaunay Method. We selected 412 galaxy groups with at least 8 members in a radius of 4Mpc. For each group we estimated its properties such as velocity dispersion ( ), physical radius (R200 ) and mass (M200 ). We also classify the groups as Gaussian and non-Gaussian (dynamic evolved or not) based on their galaxy velocity distributions. This classification is based on the following statistical tests: Anderson-Darling, Kolmogorov-Smirnov, Shapiro-Wilk, Jarque-Bera, Cramer-von Mises, D’Agostino and Dip test. When the Dip test confirms the hypothesis of the unimodality and all other tests prove the normality of the system, the group is classified as Gaussian. The behavior of gaussianity was checked varying the distance to the center of the group in 2-4 times its physical radius. Our preliminary results show that the number of systems classified as non-Gaussian groups grows with the increase of the physical radius. B 1 2 [email protected] Observatório do Valongo, Universidade Federal do Rio de Janeiro Laboratório de Astrofı́sica Teórica e Observacional, Universidade Estadual de Santa Cruz 387 Galaxies Posters GAL -4: #193 Secular Evolution in Green Valley Galaxies Nogueira-Cavalcante, J. P.B1 ; Menéndez Delmestre, K.1 ; Gonçalves, T. S.1 The distribution of galaxies in the color-magnitude diagram shows two distinct peaks: the red sequence and the blue cloud. The red sequence is predominantly populated by early-type galaxies, whose stellar population is mostly old. Within the blue cloud most galaxies are late-types, where the dominant stellar population is young. Between these two peaks there is a sparsely populated region in the color-magnitude diagram known as the green valley, which arguably represents an intermediate, brief stage in the evolution of galaxies. Several factors can cause this rapid transition, including active galactic nuclei (AGNs) and mergers. There are observational evidences that these factors act differently in different epochs of the history of the universe. In particular, Martin et al. (2007) and Gonçalves et al. (2012) pointed out that green valley galaxies evolve faster at higher redshifts (z ⇠ 0.8), compared to those at low redshift (z ⇠ 0.2). Bars play an important role in the secular evolution of galaxies, acting on a much longer timescale than mergers and AGNs. We aim to trace the impact of secular evolution in the green valley by identifying bars in green valley galaxies at z ⇠ 0.2 and z ⇠ 0.8. We here present this analysis for a small sample of z ⇠ 0.8 galaxies in the Extended Groth Strip (EGS) region imaged with the Hubble Space Telescope. In the future we intend to extend this analysis to a wider sample of high-z green valley galaxies as well as to the low-z green valley galaxy sample. B 1 [email protected] Observatório do Valongo, Universidade Federal do Rio de Janeiro 388 Posters Galaxies GAL -4: #194 Low-redshift compact UV luminous starbursts: a door to understand high-redshift Lyman-Break Galaxies Oliveira, C. S.B1 ; Menéndez-Delmestre, K.2 ; Gonçalves, T. S.3 Lyman-break galaxies (LBGs) are a population of distant objects (z ⇠ 3) selected at rest-frame UV that represent the typical starburst galaxy at a time when the universe was going through its peak in star formation activity. The star formation rates of LBGs suggest that these galaxies may be the progenitors of a large part of the massive galaxies in the local universe, making them important objects of study. However, detailed studies of the morphology and kinematics of these distant galaxies are limited by the sensitivity of current instruments. We study a sample of low-redshift UV-selected supercompact starbursts that share many properties (morphology, surface brightness, luminosity) with high-redshift LBGs and are hence denominated as Lyman-break Analogs (LBAs). These UV luminous galaxies (UVLGs) were recently uncovered by the Galaxy Evolution Explorer (GALEX) satellite. At significantly lower redshifts (z ⇠ 0.2) than LBGs, they provide us with a unique opportunity to draw analogies with their high-redshift counterparts and study in great detail the astrophysical conditions that lead to the star formation activity we observe in the distant universe. We have undertaken the near-IR photometric analysis of a sample of LBAs based on observations taken with the Fourstar instrument on the 6.5m Baade Telescope (Las Campanas Observatory, Chile). We now extend this work to the wider population of compact UVLGs, with surface brightness one or two orders of magnitude than normal galaxies, but less extreme than supercompact UVLGs. Based on J, H, Ks, and optical photometry for ⇠ 40 compact and supercompact UVLGs we are in the process of analyzing the spectral energy distribution (SED) of each individual galaxy to derive stellar masses and ages in order to explore the similarities and differences between these two populations relative to normal galaxies in the local universe and to LBGs in the distant universe. B 1 [email protected] Valongo Observatory, Federal University of Rio de Janeiro 389 Galaxies Posters GAL -4: #195 An approach to measuring the density of the environment of galaxies: results and comparisons with other measurements René A. Ortega-MinakataB1 ; Juan P. Torres-Papaqui1 ; H. Andernach1 With the aim of obtaining a homogeneous and reliable measurement of the density of the environment of a large sample of galaxies, we have written a code that counts the number of neighbouring galaxies around a target galaxy. As targets, we have selected a large sample of galaxies from the spectroscopic catalogue of the SDSS-DR7 with with redshifts between 0.03 and 0.30. The photometric catalogue of the SDSS-DR7 was used to extract and count the neighbouring galaxies from, including all objects for which a photometric redshift was available to serve as a distance estimate. The code counts all galaxies within an absolute distance of 1.5 Mpc around the target (translated to an apparent radius and a redshift range of the neighboring galaxies, based on the redshift of the target). We only count galaxies more luminous than an absolute magnitude of 19 in the SDSS r band. Within the mentioned redshift and magnitude limits, and in the North Galactic region of the SDSS, there are about 600K target galaxies and about 24M in the neighbouring galaxies sample. We present our results and compare them to other measurements of the density of the environment of galaxies, such as given by the MaxBCG catalogue of brightest cluster galaxies. As a control of our method, we apply it to a sample of galaxies from the 2MIG catalogue of isolated galaxies, and also to a sample of galaxies from a compilation of members of Abell clusters. We aim to use our results to test the morphologylocal density relation and to study the relationship between the different types of emission-line activitiy of galaxies and the density of their environment. B 1 [email protected] Departamento de Astronomı́a, Universidad de Guanajuato, Mexico 390 Posters Galaxies GAL -4: #196 A kinematic study of different stellar populations in the irregular NGC 6822 M. PeñaB1 ; S. Flores-Durán1 ; L. Hernández-Martı́nez1 ; J. Garcı́a-Rojas2 The kinematics of planetary nebulae (PNe) in in our own and other galaxies and , is a clue to understand the behavior of the low-intermediate mass stars and their relation with other galactic components. Highresolution spectroscopy of a significant sample of PNe (intermediate-age population) and HII regions (young objects) in the irregular galaxy NGC 6822 is analyzed, aiming to determine if both populations share the kinematics of the HI disk found in this galaxy. Observations were made with the Magellan telescope (MIKE spectrograph) and the 2-m telescope of SPM-OAN (MES spectrograph). The data have a resolution better than 10 km/s. The analysis shows that HII regions and other members of the young stellar population follow closely the rotation of the HI disk. On the contrary, PNe are not moving along with the HI gas and their kinematics is closer to the behavior of the spheroid of C stars, which is a system with different spatial distribution and kinematics. Thus we confirm that the irregular galaxy NGC6822 has at least two very different kinematical systems. In the future we plan to use the kinematics of these systems to model the distribution of the dark matter halo in this galaxy. B 1 2 [email protected] Instituto de Astronomı́a, UNAM, México Instituto de Astrofı́sica de Canarias, Spain 391 Galaxies Posters GAL -5: #197 Mapping Triangulum-Andromeda with the SDSS B1,5 Perottoni, H. D. ; Rocha-Pinto, H. J.1,5 ; Girardi, L.4,5 ; Balbinot, E.3,5 ; Santiago, B. X.3,5 ; Da Costa, L.2,5 ; Maia, M. A. G.2,5 The last decade has brought the first data releases of some large astronomical surveys (e.g., 2MASS, RAVE, SDSS), which allowed the discovery of several stellar overdensities in the Galactic halo. One of this overdensities is Triangulum-Antromeda (TriAnd), which was found by Rocha-Pinto et al. (2004) and Majewski et al. (2004) using a sample 2MASS M giants candidates. The existence of such overdensities argues against the canonical homogeneous stellar halo coming from the classical ELS model for the formation of the Galaxy; they point to a halo partially formed by tidal debris from former satellites galaxies of the Milky Way. TriAnd is a very diffuse cloud-like substructure - it contains approximately 1 M giant per deg2 o o o spread over a large o area between 100 < l < 150 and -10 > b > -50 . Due to its patchy density, the structure could not be well mapped with 2MASS M Giants by Rocha-Pinto et al. (2004); it is not clear whether it has a core or not. Despite the number of years since this discoveries, TriAnd is still not well known. In order to gain a better understanding about the origin of this structure, we are mapping it using photometric data from the SDSS DR9 and comparing the observations with simulations from the TRIdimensional modeL of thE GALaxy (TRILEGAL; Girardi et al. 2005). B 1 2 3 4 5 [email protected] OV/UFRJ ON/MCT UFRGS Osservatorio Astronomico di Padova LINEA 392 Posters Galaxies GAL -5: #198 Galaxy Model in Infrared Polido, P.B1 ; Jablonski, F.1 We present in this work a new approach to the derivation of galactic parameters via the star counts method. It uses a modern version of the model of Ortiz & Lépine (1993) and the 2MASS data in J, H and KS to estimate, based on a regular grid of lines-of-sight over the whole sky, the most important structural parameters of the Galaxy. It is the first time that the star counts method is used in the whole sky, including the complex region of the galactic plane. We have used a conservative approach to derive parameter values and their uncertainties, and also investigate the effects of using several limiting magnitudes over the best set of parameters which describes the Galaxy. Since the landscape for the figure of merit of a model can be pretty complex when we have a number of free parameters in excess of a dozen, the Markov Chain Monte Carlo method looks like ideal for an overview of the parameter space, to constrain regions of interest for further exploration and to provide realistic uncertainties. The pinpointing of the best parameter values is carried out with the Nested Sampling method, very robust in terms of progression to the optimum solution of a multiparameter model. B 1 [email protected] Instituto Nacional de Pesquisas Espaciais 393 Galaxies Posters GAL -5: #199 Physical parameters of galaxies with star formation through mid-infrared SED models Andrés F. Ramos P.B1 ; J. R. Martı́nes-Galarza2 ; Mario-A. Higuera-G.3 ; Seditsira Quintero4 We present a multiwavelength study of a sample of 22 starburst galaxies and derive physical parameters using Bayesian SED fitting. We take into account the emissions of the Polycyclic Aromatic Hydrocarbons (PAHs), as well as the total bolometric luminosities of the observed galaxies. We use state of the art SED models, as a necessary tool in order to investigate physical properties. Our study of this local sample of galaxies helps in the understanding of massive star formation through cosmic history. Using a Bayesian fitting routine, we fit the Spitzer-IRS spectra of local (z<0.5) galaxies in the range of 5 to 35 µm, complemented with infrared photometry obtained by the Spitzer Space Telescope and the Herschel Space Observatory. We derive marginalized probability distribution functions (PDFs) for model parameters. We calculate metallicity, interstellar medium pressure, star formation rates (averaged over 1, 10 and 100 Myr), compactness C (related to the dust heating flux), PDR fraction fP DR , extinction AV and attenuation of diffuse dust. We compare the derived parameters and search for galaxy to galaxy correlations between them. Finally, we also study the correlations between our derived parameters and nebular line emission from atomic species. With this study we aim at relating the global star-forming properties of these galaxies to the internal physics at the level of individual HII regions. Our 22 galaxies are an excelent comparison sample for star-forming galaxies at higher redshifts. B 1 2 3 4 [email protected] Department of Physics, National University of Colombia, Ciudad Universitaria, Bogotá D.C., Colombia Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-51, Cambrigde, MA 02138, USA National Astronomical Observatory, National University of Colombia, Ciudad Universitaria, Bogotá D.C.,Colombia Department of Mathematics, National University of Colombia, Ciudad Universitaria, Bogotá D.C., Colombia 394 Posters Galaxies GAL -5: #200 Disk Mass-to-light Ratio Distribution from Stellar Population Synthesis: Application to Rotation Curve Decomposition of NGC 5278 Repetto, P.B1 ; Martı́nez-Garcı́a, Eric E.2,3 ; Rosado, M.2 ; Gabbasov, R.2 In this work we extend the study on the mass distribution of the spiral galaxy NGC 5278, performing 1D and 2D (GALFIT) bulge-disk decomposition to determine which components constitute the baryonic mass in this galaxy. Our analysis does not detect any bulge; instead we find a bright source probably related to the central active galactic nucleus and an exponential disk. We fix the stellar disk contribution to the rotation curve (RC) with broadband photometric observations and population synthesis models, to obtain the 2D mass distribution of the stellar disk. In the particular case of NGC 5278, we find that the typical assumption of considering the mass-to-luminosity ratio (M/L) of the disk as constant along the galactocentric radius is not valid. We also extract a baryonic RC from the mass profile to determine the inability of this baryonic RC and also the baryonic RC with more than and less than 30% disk mass (in order to consider the disk mass errors) to fit the entire RC. We perform the RC decomposition of NGC 5278 by considering the baryonic RC and four types of dark matter (DM) halo: Hernquist, Burkert, Navarro, Frenk, & White, and Einasto. Our results determine that the Hernquist DM halo better models our observed RC in the case of disk mass Md = 5.6⇥1010 M and also with less than 30% disk mass. In the case of more than 30% disk mass, the cored Einasto (n < 4) DM halo is the best-fitting model. B 1 2 3 [email protected] Laboratorio Nacional De Astrofisica, R. Estados Unidos 154, Barrios das Naçoes 37.504-364, Itajuba-MG Instituto de Astronomı́a, Universidad Nacional Autónoma de México (UNAM), Apdo. Postal 70-264, 04510 México, D.F., Mexico Instituto Nacional de Astrofı́sica, Óptica y Electrónica (INAOE), Aptdo. Postal 51 y 216, 72000 Puebla, Pue., Mexico 395 Galaxies Posters GAL -5: #201 AM2217-490: Uma galáxia com anel polar em formação Priscila Freitas-Lemes1 ; Irapuan RodriguesB1 ; Maximilliano Faúndez-Abans2 ; Oli Dors1 O presente trabalho é parte de uma série de estudos de caso de Galáxias com Anel Polar (PRG, do inglês: ”Polar Ring Galaxy”). Uma PRG é formada por uma galáxia hospedeira do tipo precoce, lenticular ou elı́ptica, rodeada por um anel de gás e estrelas orbitando um plano aproximadamente perpendicular ao plano principal da galáxia hospedeira). AM2217-490 é um caso interessante de PRG em formação, com um anel ainda assimétrico que rodeia a galáxia hospedeira. Ao que tudo indica, essa estrutura azulada (que é caracterı́stica dos anéis das PRGs), ainda não está em equilı́brio com a galáxia hospedeira. O presente estudo, ainda em fase preliminar, se baseia em espectros de 6250 - 7250 Å obtidos no telescópio de 1.5m do CTIO - Chile. A partir deles, medimos a velocidade heliocêntrica do sistema: 9152 ± 18 km/s. Diagramas de diagnóstico apontam que a região nuclear da galáxia se comporta como uma região HII. Os valores médio encontrados são: log(NII/H↵ ) = -0.16 e log(SII/H↵ ) = -0.69. O seu parâmetro de ionização (log U = -2,99), é similar ao valor encontrado em galáxias isoladas. Entre as PRGs estudadas até o momento, várias delas apresentam atividade nuclear. Se a atividade nuclear nas PRGs é desencadeada pela queda de gás durante a formação do anel polar, é compreensı́vel que no caso de AM2217-490 ela ainda não tenha ocorrido, pois seu anel ainda está em formação. As imagens de baixa resolução do SDSS não mostram pontes ou caudas que liguem a galáxia a outros objetos, entretanto, em um raio de 5 arcmin existem 3 outras galáxias com velocidades similares, caracterizando um grupo. Uma hipótese plausı́vel é que dessas galáxias pode ter interagido com AM2217-490, doando material para a formação do anel. B 1 2 [email protected] Universidade do Vale do Paraı́ba - UNIVAP Laboratório Nacional de Astrofı́sica - LNA/MCTI 396 Posters Galaxies GAL -5: #202 Determination of Halo Occupation Distribution Rodriguez, F.B1 ; Sgró, M. A.1 ; Merchán, M.1 The current paradigm assumes that galaxies form within dark matter halos. However, the diversity of astrophysical mechanisms involving in galaxy formation do not allow to determine how many galaxies lie in a halo of a given mass. In this context, the Halo Occupation Distribution (HOD) gives the probability that a halo of mass M contains N galaxies and allows associate, in a statistics way, the amount of galaxies residing in a halo. In this work, we propose a method of background subtraction for calculate the HOD. This allows to combine spectroscopic information from catalogs of galaxy groups with photometric information from a catalog of galaxies. To evaluate the procedure, we used mock catalogs of galaxies and groups constructed with a imposed HOD. We compare this fiducial HOD with the obtained results by applying our method. Finally, we implement background subtraction in the Sloan Digital Sky Survey DR7. B 1 [email protected] Instituto de Astronomı́a Teórica y Experimental (UNC-CONICET), Observatorio Astronómico de Córdoba. 397 Galaxies Posters GAL -5: #203 Effects of interaction in chemical evolution and stellar population of galaxy pairs Rosa, D. A.B1 ; Dors Jr., O. L.1 ; Krabbe, A. C.1 ; Pastoriza, M. G.2 ; Winge, C.3 ; Hägele, G. F.4,5 ; Cardaci, M. V.4,5 In this work we present a study about the influence of interactions on the metallicity, traced by the oxygen abundance of the gas phase, and on the stellar population in a sample of galaxy pairs. We used data of long slit spectroscopy in the spectral region 3000-7000 Åobtained with the GMOS/Gemini South telescope for a sample of six pairs of galaxies. These data were combined with stellar population synthesis models using the program STARLIGHT and a grid of photoionization models built with the Cloudy code. We found that some objects are dominated by younger populations with up to 500 billion years and other have a profile along the disk with stellar population composed of heterogeneous elements. We derived flatted oxygen abundance gradients in the interacting galaxies, with values in consonance with the solar value (i.e. 12+log(O/H)=8.7). We conclude that interactions change significantly the chemical evolution and the history of star formation of galaxy pairs. B 1 2 3 4 5 [email protected] Universidade do Vale do Paraı́ba, Av. Shishima Hifumi, 2911, Cep 12244-000, Brazil Instituto de Fı́sica, Universidade Federal do Rio Grande do Sul, Av. Bento Gonçalves, 9500, Cep 91359-050, Porto Alegre, RS, Brazil Gemini Observatory, c/o AURA Inc., Casilla 603, La Serena, Chile Instituto de Astrofı́sica de La Plata (CONICET La Plata–UNLP), Argentina Facultad de Ciencias Astronomicas y Geofısicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, 1900 La Plata, Argentina 398 Posters Galaxies GAL -5: #204 The dense gas in M82 B1 Salas, P. ; Galaz, G.1 ; Bolatto, A.2 ; Salter, D.2 ; Herrera, R.2 Understanding how galaxies evolve is one of the major goals of modern astronomy. In order to obtain an integral understanding of how galaxies evolve there is a need to understand how different physical processes shape the ISM. One of these processes is that of star formation, which can be studied through observations of dense gas. The key question regarding galactic evolution is to know how different high density molecular tracers allow us to study the star-forming conditions of their hosts. Studying how different star formation indicators change over different physical scales is the question we want to address. In order to study the properties of the star-forming disk present in the prototypical starburst galaxy M82 we have obtained 3 mm maps of 6 high density tracers using CARMA. Our maps have resolutions of 6”x6” (⇠ 100 pc at the distance of M82), allowing us to study its structure in detail. The properties of the central star-forming disk reveal a picture consistent with the model of an evolutionary sequence for starburst galaxies as traced by their molecular gas abundances. Our higher resolution, compared to previous surveys, allows us to study how these abundances change on smaller scales. B [email protected] Instituto de Astrofı́sica, Facultad de Fı́sica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile 2 Department of Astronomy and Laboratory for Millimeter-Wave Astronomy, University of Maryland, College Park, MD 20742, USA 1 399 Galaxies Posters GAL -5: #205 PAH lines at high redshift as galaxy evolution marker Santos, J. H. B.B1 ; Friaça, A. C. S.1 Based in chemodinamycal models for galaxy evolution, we studied the formation of PAH lines at high redshifts. The model considers carbon and silicon grains, and also PAH molecules. It distinguishes diffuse ISM the molecular clouds associated to star forming regions. The PAH lines provide a good signature of the evolutionary stage of galaxies, star formation rate, in addition to allowing the assessment the relative importance for of AGN and stellar emission on the output of the galaxy. In particular, the line ratio 11.3/7.7 µm is a good marker of the age of high redshift galaxies. We expected that our calculations provide some benchmarks both for future observations both with ground and satellite instruments. The ages derived in this way for high redshift objects could be used to test dark energy models. In addition to the cosmological applications, the observations of the PAH features could be used to check the charge state of PAHs. Apparently, anions and neutrals are favored over cations. B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo (IAG-USP) 400 Posters Galaxies GAL -6: #206 The mass–metallicity–star formation rate relation under the STARLIGHT microscope Schlickmann, M. S.B1 ; Vale Asari, N.1 ; Fernandes, R. C.1 ; Stasinska, G.2 The correlation between stellar mass and gas-phase oxygen abundance (M –Z relation) has been known for decades. The slope and scatter of this trend is strongly dependent on galaxy evolution: Chemical enrichment in a galaxy is driven by its star formation history, which in turn depends on its secular evolution and interaction with other galaxies and intergalactic gas. In last couple of years, the M –Z relation has been studied as a function of a third parameter: the recent star formation rate (SFR) as calibrated by the H↵ luminosity, which traces stars formed in the last 10 Myr. This mass–metallicity–SFR relation has been reported to be very tight. This result puts strong constraints on galaxy evolution models in low and high redshifts, informing which models of infall and outflow of gas are acceptable. We explore the mass–metallicity–SFR relation in light of the Sdss–starlight database put together by our group. We find that we recover similar results as the ones reported by authors who use the MPA/JHU catalogue. We also present some preliminary results exploring the mass–metallicity–SFR relation in a more detailed fashion: Starlight recovers a galaxy’s full star formation history, and not only its recent SFR. B 1 2 [email protected] Departamento de Fı́sica - CFM - Universidade Federal de Santa Catarina, Florianópolis, SC, Brazil LUTH, Observatoire de Paris, CNRS, Université Paris Dieterot, Place Jules Janssen, 9210 Meudon, France 401 Galaxies Posters GAL -6: #207 MagAl: A new tool to analise galaxies photometric data Schoenell, W.B1 ; Benitez, N.1 ; Cid Fernandes, R.2 On galaxy spectra, one can find mainly two features: emission lines, which tell us about the ionised gas content, and the continuum plus absorption lines, which tell us about the stellar content. They thus allow us to derive gas-phase abundances, the main radiation sources, chemical enrichment and star formation histories. Braad-band photometry, on the other hand, is much more limited and hinders our ability to recover a galaxy’s physical properties to such a degree of detail. However, with the recent development of redshift surveys using the technology of ultra-narrow filters (⇡ 100 Å), such as ALHAMBRA, J-PAS and DES, it will be invaluable to be able to retrieve information on physical properties of galaxies from photometric data. Motivated by this data avalanche (which goes up to the petabyte scale), we decided to build our own SED-fitting code: Magnitudes Analyser (MagAl), which has three modules. 1) A template library generation module: generates empirical and theoretical template libraries. 2) Bayesian fitting module: calculates probability distribution functions (PDFs) for given observed and library template data. This is similar to the method to measure photometric redshifts by Benitez (2000). 3) A result-analyser module: streamlines data analysis from the large output PDFs files. A fourth module to manage 3D data is being developed and a few preliminary tests are also shown. To investigate the reliability of results obtained by MagAl, we have created a mock galaxy sample for the ALHAMBRA survey filter system (http://alhambrasurvey.com) and tried to recover their physical properties. We show that for our sample of simulated galaxies we can measure stellar ages, metallicities and extinctions with a precision of less than 0.3 dex. Also, we apply the code to the ALHAMBRA survey catalog and show that we can measure stellar masses with an accuracy of 0.2 dex when comparing to previous results like COSMOS masses measured by Bundy et al. (2006). B 1 2 [email protected] Instituto de Astrofı́sica de Andalucı́a - CSIC Departamento de Fı́sica, Universidade Federal de Santa Catarina 402 Posters Galaxies GAL -6: #208 The NEBULATOM cookbook Stasinska, G.B1 ; Morisset, C.2 We present a series of problems on nebular physics with detailed comments and solutions in python. Their aim is to lead the student to a better understanding of the respective roles of the different processes at play in ionized nebulae, and to use with proper insight some tools that have been developed for the analysis of nebulae. These exercises have been proposed at the NEBULATOM workshop in Choroni (Venezuela, 3-16 March 2013), a capacity development workshop for Latin American astronomers on emission-line objects in the Universe. B 1 2 [email protected] LUTH, Observatoire de Paris, CNRS, Université Paris Diderot, Place Jules Janssen, 92190 Meudon, France Instituto de Astronomı́a, Universidad Nacional Autónoma de México, Apdo. Postal 70264, Méx. D.F., 04510 Mexico, Mexico 403 Galaxies Posters GAL -6: #209 Physical conditions and kinematics of an HII galaxy with extraordinary dense nucleus: Mrk 996 Eduardo TellesB1 ; Trinh X. Thuan2 ; Yuri I. Izotov3 ; Eleazar Rodrigo Carrasco4 We present an integral field spectroscopic study with the Gemini Multi-Object Spectrograph (GMOS) of the unusual blue compact dwarf (BCD) galaxy Mrk 996. We show through velocity and dispersion maps, emission-line intensity and ratio maps, and by a new technique of electron density limit imaging, that the ionization properties of different regions in Mrk 996 are correlated with their kinematic properties. From the maps, we can spatially distinguish a very dense high-ionization zone with broad lines in the nuclear region, and a less dense low-ionization zone with narrow lines in the circumnuclear region. Four kinematically distinct systems of lines are identified in the integrated spectrum of Mrk 996, suggesting stellar wind outflows from a population of WR stars in the nuclear region, superposed on an underlying rotation pattern. From the intensities of the blue and red bumps, we derive a population of ⇠473 WNL stars and ⇠98 WCE stars in the nucleus of Mrk 996, resulting in a high N (WR)/N (O+WR) of 0.17. We derive, for the outer narrow line region, an oxygen abundance12+log(O/H)=7.94±0.03 (⇠ 0.2 Z )by using the direct Te method derived from the detected narrow [O III] 4363 line. The nucleus of Mrk 996 is however nitrogen-enhanced by a factor of ⇠20, in agreement with previous CLOUDY modeling. This nitrogen enhancement is probably due to nitrogen-enriched WR ejecta, but also to enhanced nitrogen line emission in a high-density environment. Although we have made use here of two new methods (PCA tomography and a method for mapping low- and high-density clouds) to analyze our data, new methodology is needed to further exploit the wealth of information provided by integral field spectroscopy. B 1 2 3 4 [email protected] Observatorio Nacional, Rua Jose Cristino, 77, Rio de Janeiro, RJ, 20921-400, Brazil Astronomy Department, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904, USA Main Astronomical Observatory, Ukrainian National Academy of Sciences, Zabolotnoho 27, Kyiv, 03680, Ukraine Gemini Observatory/AURA, Southern Operations Center, Casilla 603, La Serena, Chile 404 Posters Galaxies GAL -6: #210 Metallicity gradients in tidal tails and merging systems B1 Torres-Flores, S. ; Scarano Jr, S.2 ; Mendes de Oliveira, C.3 ; de Mello, D. F.4 ; Amram, P.5 ; Plana, H.6 ; Alfaro, M.1 ; Olave, D.1 Interacting systems are ideal laboratories to study galaxy evolution. During the collision process, gas coming from different regions of interacting galaxies can mix, producing a flattening in the radial distribution of metals in these systems. In this talk, we present an analysis of the metal distribution in the tidal tails of three interacting systems: NGC 92, NGC 2782 and NGC 1487. We also have studied the main body of the merger system HCG 31. Using Gemini/GMOS spectroscopic data, we found no metallicity gradients for the tails of the systems NGC 92 and NGC 2782, which suggests that gas mixing triggered by the interaction produces a flattening in the original metallicity gradient of these systems. A similar scenario was detected in the central region of the merger HCG 31. Our results suggest that a fraction of the enriched gas that was originally located in the center of the interacting galaxies was expelled into the tidal tails when the interacting process that formed the tail happened. B 1 2 3 4 5 6 [email protected] Universidad de La Serena, Chile Universidade Federal de Sergipe, Brazil Instituto de Astronomia, Geofı́sica e Ciencias Atmosféricas da Universidade de Sao Paulo, Brazil Catholic University of America, Washington, USA Laboratoire d’Astrophysique de Marseille, France Universidade Estadual de Santa Cruz, Brazil 405 Galaxies Posters GAL -6: #211 FIR/Radio correlation for different systems of galaxies Vena Valdarenas, R. R.B1 ; Valotto, C.1,2 We present preliminary results from the statistical analysis of the correlation between the radio and far infrared fluxes in different samples of groups and clusters of galaxies, and isolated galaxies. We use 1.4 GHz fluxes from the NRAO VLA Sky Survey (NVSS) and Faint Images of the Radio Sky at Twenty centimiters (FIRST), and infrared fluxes at 12, 24, 60 and 100 microns from Infrared Astronomical Satelite (IRAS) and 12 and 22 microns from the Wide-field Infrared Survey Explorer (WISE). We show variations on the behavior of this correlation for the different samples. This correlation has been studied by several authors for different samples isolated galaxies and groups of galaxies. B 1 2 [email protected] Instituto de Astronomı́a Teórica y Experimental Observatorio Astronómico de Córdoba, Universidad Nacional de Córdoba 406 Posters Galaxies GAL -6: #212 The lost population of post-starburst galaxies Werle, A.B1 ; Mateus, A.1 Post-starburst (PSB) galaxies comprise a class of objects that show strong traces of young stellar populations in their spectra, but no sign of ongoing star formation. Their star formation histories (SFH) indicate that these galaxies stopped forming stars in the past 1.5 Gyr. Samples of PSB galaxies are usually generated by selecting spectra with strong Balmer absorption lines, but no detectable emission lines that characterize star formation (e.g. [OII] 3727 and H↵). The usual criterion to limit star formation is to set the equivalent width of the H↵ emission line to be smaller than 5 Å (Goto el al. 2004). Post-starburst galaxies identified in the Sloan Digital Sky Survey (SDSS) by requiring minimal H↵ equivalent width generally exhibit weak but nonzero emission lines with typical ratios of Active Galaxy Nuclei (AGN) hosts. This suggests that most PSB galaxies may harbor “low-ionization nuclear emission-line regions” (LINERs) and, more rarely, Seyferts (Yan et al. 2008). In this research, we use the STARLIGHT spectral synthesis code (Cid Fernandes et al. 2005) to compute the fraction of light coming from young stellar populations, here denoted by fy , in a volume-limited sample from the SDSS DR7 catalog. We then classify as PSB those galaxies with fy larger than 80% and log([NII] 6584/H↵) higher than 0.4. This second criterion select galaxies without current star formation (Cid Fernandes et al. 2011). When plotting this sample in the BPT diagram, we identify a high occurrence of LINER and Seyfert hosts, as found by Yan et al. (2008). However, we show that a large amount of poststarburst galaxies with low emission lines are in fact passive galaxies, frequently misclassified as weak AGN hosts. B 1 [email protected] Grupo de Astrofı́sica, Universidade Federal de Santa Catarina, Brazil 407 Galaxies Posters GAL -6: #213 Galaxy Detection Behind the Milky Way using the VVV Survey Baravalle, L.B1 ; Alonso, M. V.2,3 ; Nilo Castellon, J. L.2,4 Our participation in the VVV survey (Vista Variables in the Vı́a Láctea ) gives us a great opportunity to study the distribution of galaxies, obscured by the presence of our Galaxy. The survey includes observations in five near-infrared passbands of the bulge and part of the disk of the Galaxy. This work consists of the d115 TILE analysis looking for extended objects. We study the star-galaxy separation and we obtain photometric properties of extended objects. As a first step, we also perform a visual inspection of these images, finding 205 candidates for galaxies. Our main goal is to automatically detect these extended objects and to separate them in a photometric way. We analyse different regions in the Color- Magnitude and Color-Color Diagrams. B 1 2 3 4 [email protected] Facultad de Matemática, Astronomı́a y Fı́sica, Universidad Nacional de Córdoba (UNC) Instituto de Astronomı́a Teórica y Experimental (IATE-CONICET), Córdoba Observatorio Astronómico de Córdoba, UNC Departamento de Fı́sica, Facultad de Ciencias, Universidad de La Serena, Cisternas 1200, La Serena, Chile 408 Posters Galaxies GAL -6: #214 Confirmation of a cluster of galaxies hidden behind the Galactic bulge using the VVV Survey Minniti, D.1 ; Hempel, M.1 ; Ivanov, V. D.2 ; Coldwell, G.B3,4 ; Alonso S.3,4 ; Duplancic, F.3,4 We report the confirmation of a rich cluster of galaxies located behind the Milky Way bulge using the VVV Survey database. This year the X-Ray satellites SUZAKU and CHANDRA discovered an X-ray cluster of galaxies located in the crowded regions of the bulge. The near-infrared photometry of the VVV survey allowed us to provide infrared confirmation of this cluster. We build a deep near-infrared image of the field based on 30 different epochs. We also present color-magnitude and color-color diagrams using SExtractor, and device specific criteria based on colors and morphology to select the galaxies among the numerous stellar sources in the foreground. We find two dozen candidate galaxies, from which the cluster red sequence can be identified. Using all the information available, we also estimate the total extinction along this line of sight towards the bulge. B 1 2 3 4 [email protected] Instituto de Astrofisica, Pontificia Universidad Catolica de Chile, Santiago, Chile European Southern Observatory, Santiago, Chile ICATE - CONICET FCEFyN - Universidad Nacional de San Juan 409 Galaxies Posters GAL -7: #215 Subhalo abundance matching in different Semi Analytic Models Contreras, S.B1,2 ; Baugh, C. M.2 ; Norberg, P.2 ; Padilla, N.1 Semi-analytic models (SAMs) have become one of the most useful tools to study galaxy formation and evolution, and that is why we decided to study two of the most advanced SAMs available today, the Guo model from MPA (Guo et al. 2011) and the Lagos models from Durham University (Lagos et. al. 2012) using subhalo abundance matching (SHAMs) for several physical properties of the galaxies and for different redshifts. We find a good agreement between the models for the properties of galaxies typically well reproduced by SAMs (like stellar mass or r-band magnitude) by construction, but we find a less good agreement between the models for other properties such as cold gas, SFR, U-band magnitude and black hole mass, demonstrating that even though some predictions from semi-analytic models are consistent, some still have not reached a unique prediction from different groups. B 1 2 [email protected] Instituto de Astrofı́sica, Pontificia Universidad Católica de Chile Institute for Computational Cosmology, Department of Physics, Durham University 410 Posters Galaxies GAL -7: #216 Potential-Density Pairs for Thin Disks and Spheroidal Haloes I: Expansion in Chevishev Type I Polinomials Cortés-Serrano, F.B1 ; González, G. A.; Reina, J. I. We present an infinite family of power-density pairs for galaxy models composed by thin disks and spheroidal haloes. In order to obtain the models, we first introduce the oblate spheroidal coordinates, which adapt in a natural way to the geometry of the model. On crossing the disk, one of the oblate coordinates present a change of sign without changing their absolute value, leading so to a finite discontinuity of the normal derivative of the potential across the disk. Accordingly, we can obtain the surface mass density of the disk by applying the Gauss law across the disk and the density of matter of the spheroidal halo by computing means of the Poisson equation. The models are then obtained by expressing the gravitational potential as a superposition of products of the Legendre functions of second class with the Chevishev Type I polynomials. Given a solution for the potential with these characteristics, we obtain the corresponding expressions for the density of the spheroidal halo of matter, the surface density of the disk and the circular velocity or rotation curve. B 1 [email protected] Escuela de Fı́sica, Universidad Industrial de Santander 411 Galaxies Posters GAL -7: #217 Triplets of galaxies: A connection with compact groups? Duplancic, F.B1,2 ; O’Mill, A. L.3 ; Lambas, D. G.4,2 ; Sodré, L.3 ; Alonso, S.1,2 We analyse a sample of 71 triplets of luminous galaxies derived from the work of O’Mill et al. (2012). The triplets are restricted to have members with spectroscopic redshifts in the range 0.01 < z < 0.14 and Mr < 20.5. We compare the properties of triplets and their members with those of control samples of compact groups, the ten brightest members of rich clusters, and galaxies in pairs. Our analysis suggest that triplet galaxy members behave similarly to compact group members and galaxies in rich clusters. We also find that systems comprising 3 blue, star-forming, young stellar population galaxies (blue triplets) are most probably real systems and not a chance configuration of interloping galaxies. The same holds for triplets composed by 3 red, non star-forming galaxies, showing the correlation of galaxy properties in these systems. From the analysis of the triplet as a whole, we conclude that, at a given total stellar mass content, triplets show a total star formation activity and global colours similar to compact groups. However, blue triplets show a high total star formation activity with a lower stellar mass content. From an analysis of the compactness parameter of the systems we find that light is even more concentrated in triplets than in compact groups. We propose that triplets composed by 3 luminous galaxies, should not be considered as an analogous of galaxy pairs with an extra member, but rather they are a natural extension of compact groups. B 1 2 3 4 [email protected] Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE) Consejo de Investigaciones Cientı́ficas y Técnicas (CONICET) Departamento de Astronomia, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas da USP Instituto de Astronomı́a Teórica y Experimental (IATE), Observatorio Astronómico, Universidad Nacional de Córdoba 412 Posters Galaxies GAL -7: #218 The galaxy-halo connection and scale relations for disks galaxies Mancillas-Vaquera B. L.B1 In this work is used the galaxy-halo connection empirically constrained to build an updated static model which is a generalization of Mo Mao & White model (1998), and wich obtains scale relations, dynamicstructure functions and the rotation curves decompositions of local disc galaxies population. We proceed generating a synthetic catalog (mock catalog) with semi-empirical relations formed by millions of galaxies with stellar masses, halo masses, color, satellites population which are in staticall agreement with observations. The aim of this work is to constrain the spin parameter of the galaxy, and to compare the structural and dynamics properties of the synthetic catalog with observations from a sample of galaxies compiled and adequately homogenized from literature. Thereby, applying the static model to each of galaxies in the catalog, we measure scale relations, baryonic mass-dark mass into optical radius function of mass and surface density. Furthermore, we calculate stellar mass and velocity functions for each galaxy in the synthetic catalog. B 1 [email protected] Instituto de Astrofı́sica, Universidad Nacional Autónoma de México 413 Galaxies Posters GAL -7: #219 Potential-Density Pairs for Thin Disks and Spheroidal Haloes II: Expansion in Chevishev Type II Polynomials Martı́nez, S. M.B1 ; González, G. A.; Reina, J. I. We present an infinite family of power-density pairs for galaxy models composed by thin disks and spheroidal haloes. In order to obtain the models, we first introduce the oblate spheroidal coordinates, which adapt in a natural way to the geometry of the model. On crossing the disk, one of the oblate coordinates present a change of sign without changing their absolute value, leading so to a finite discontinuity of the normal derivative of the potential across the disk. Accordingly, we can obtain the surface mass density of the disk by applying the Gauss law across the disk and the density of matter of the spheroidal halo by means of the Poisson equation. The models are then obtained by expressing the gravitational potential as a superposition of products of the Legendre functions of second class with the Chevishev Type II polynomials. Given a solution for the potential with these characteristics, we obtain the corresponding expressions for the density of the spheroidal halo of matter, the surface density of the disk and the circular velocity or rotation curve. B 1 [email protected] Escuela de Fı́sica, Universidad Industrial de Santander 414 Posters Galaxies GAL -7: #220 Potential-Density Pairs for Thin Disks and Spheroidal Haloes III: Expansion in Gegenbauer Polynomials Nieto, O.B1 ; González, G. A.; Reina, J. I. We present an infinite family of power-density pairs for galaxy models composed by thin disks and spheroidal haloes. In order to obtain the models, we first introduce the oblate spheroidal coordinates, which adapt in a natural way to the geometry of the model. On crossing the disk, one of the oblate coordinates present a change of sign without changing their absolute value, leading so to a finite discontinuity of the normal derivative of the potential across the disk. Accordingly, we can obtain the surface mass density of the disk by applying the Gauss law across the disk and the density of matter of the spheroidal halo by means of the Poisson equation. The models are then obtained by expressing the gravitational potential as a superposition of products of the Legendre functions of second class with the Gegenbauer polynomials. Given a solution for the potential with these characteristics, we obtain the corresponding expressions for the density of the spheroidal halo of matter, the surface density of the disk and the circular velocity or rotation curve. B 1 [email protected] Escuela de Fı́sica, Universidad Industrial de Santander 415 Galaxies Posters GAL -7: #221 Weak lensing measurements from radio data Paez Tagliaferro, T.B1 ; Valotto, C.2,3 In this work we present a statistical study on the possibility of detecting gravitational lenses by the presence of galaxies or systems of galaxies from the analysis radio data. We present some preliminary results, compared with previous works, where we have used the radio catalogs NVSS y FIRST. In order to give same restrictions on the detection, will present a study carried out using simulated catalogs to analyze the probability of identify lenses in the sample. B 1 2 3 [email protected] Facultad de Matemática, Astronomı́a y Fı́sica (FaMAF) Observatorio Astronómico de Córdoba Instituto de Astronomı́a Teórica y Experimental (Iate) 416 Posters Galaxies GAL -7: #223 Sagittarius dwarf galaxy population from the VVV behind the galactic bulge Santucho, M. V.B1 ; Gurovich, S.1 ; Domı́nguez, M.1,2 In this work we identify the stellar population of Sagittarius dwarf satellite galaxy using combined data from both the VVV and 2MASS surveys. While the VVV data is more sensitve to the lower RGB and Red Clump components, the 2MASS data is more sensitive to the upper RGB, where the VVV is non-linear and saturates. Both data sets are matched, put on the VVV photometric system (Vega), isochrones modelled. Since Sgr dSph is behind the galactic bulge, the selected area for this work is strongly affected by reddening and stellar crowding. We address the issue of reddening with dust-extinction maps. Since the Schlegel maps are not as reliable at low galactic latitudes, to be safe we use new dust-maps derived from bulge red clump stars from VVV data which offer a significantly higher spatial resolution. Sgr dSph stars are then separated from the foreground galactic disk and bulge populations with a CMD filter. This filter includes the Sgr dSph’s horizontal and the RGB branches that we use in a subsequent search of stars, in adjacent tiles, associated with Sgr dSph. We present a surface density map of Sgr dSph based on the spatial distribution of all filtered stars in accordance with our selected criteria. Finally we examine if there is evidence for a lack of of Sgr dSph stars towards the mid-plane of the Milky-Way, possibly due to tidal interaction, as suggested by earlier studies. B 1 2 [email protected] Instituto de Astronomı́a Téorico y Experimental (IATE) Observatorio Astronómico de Córdoba 417 418 AGN AGN -1: #224 IFU spectroscopic analysis of the active nucleus NGC 6951 Andrade, I. S.B1 ; Steiner, J. E.1 ; Ricci, T. V.1 Active Galactic Nuclei are associated to black holes accreting mass. The study of this objects can show us not only the geometry and the physics process related to them as well their contribution to the galaxy evolution. The goal of this work is to study the nucleus of the galaxy NGC 6951 (SAB(rs)bc), at the distance of 22.8 Mpc. We will compare our the nuclear emission lines analysis, with that obtained by Storchi-Bergmann et al. 2007. Our analysis of the data cube was performed using a series of sophisticated techniques that presumably will result in more reliable measurements and conclusion. This analysis will also be compared with the data obtained with the NIFS spectrograph on Gemini North in the K band, using adaptive optics. One of our main conclusions is that this AGN is highly obscured by a dust lane/torus, perpendicular to the line-of-sight, quite similar to what is seen in the Seyfert galaxy NGC 1068. B 1 [email protected] Institute of Astronomy, Geophysics and Atmospheric Sciences, University of Sao Paulo 419 AGN Posters AGN -1: #225 Testing the Physical Properties of the Unified Model for AGN Audibert, A.B1 ; Riffel, R.1 ; Pastoriza, M. G.1 ; Sales, D. A.2 According to the Unified Model (UM), the energy from Active Galactic Nuclei (AGN) is provided by the accretion of matter into a supermassive black hole (SMBH). The UM also suggests that different AGNs classes are due to the presence of a dusty torus, which under different view angles can obscure the SMBH and the broad line region. Recent studies contest the UM on the physical and geometrical properties of the torus, i. e., the traditional “donut” or if the matter is distributed in a clumpy medium arranged in a toroidal structure. Our goal is to study and to analyze statistically the physical parameters of a sample of about 100 Seyfert galaxies using public data from Spitzer telescope in the mid infrared (5.2-38 µm). We compare the spectral energy distributions (SEDs) with ⇠ 106 theoretical SEDs which consider that the torus is formed by dusty clouds. We present the results for the following 8 parameters: the observers viewing angle, i, the number of clouds in the torus equatorial plane, N0 , the number of clouds along the viewing angle, Nobs , the clouds individual optical depth, ⌧V , the power law index for the spatial distribution of the clouds, q, the torus angular width, , the radial extension of the clumpy distribution, Y and the optical extinction produced by the torus along the line of sight, AV . B 1 2 [email protected] Departamento de Astronomia, Instituto de Fı́sica, UFRGS Rochester Institute of Technology 420 Posters AGN AGN -1: #226 Two-dimensional kinematics of the central region of NGC4501 from Gemini/GMOS integral field spectrocopy Brum, CarineB1 ; Riffel, R. A.1 ; Storchi-Bergmann, T.2 ; Müller, A. S.2 ; Robinson, A.3 We present two-dimensional stellar and gas kinematics in the central region of the Seyfert galaxy NGC 4501 from optical Integral Field Spectroscopy obtained with Gemini Multi-Object Spectrograph (GMOS) at GeminiNorth telescope. The final data cube contains ⇠16000 spectra covering the inner 7” ⇥ 15” at spatial resolution of ⇠ 48 pc and covering the spectral region from 5600 Å to 7000 Å. Two-dimensional maps for the flux, velocity and velocity dispersion ( ) were obtained from the fitting of the emission-line profiles of H↵, [N II] 6548,6584 and [S II] 6717,6731. All lines present extended emission to up to 5” from the nucleus with flux peak at it. The gas velocity field for all lines are similar, being dominated by rotation in the plane of the galaxy with a velocity amplitude of 100 km/s, although deviations from rotation are seen at some locations. On the far side of the galaxy we observed blueshifts and on the near side redshifts along spiral structuras, being interpreted as inflows towards the nucleus of NGC 4501. The forbidden lines show values ranging from 50 to 150 km/s while the H↵ shows overall smaller values, with the highest ones reaching ⇠ 100 km/s. The highest values for all emission lines are observed at 2-3 arcsec northeast from the nucleus, being co-spatial with a distortion seen in the velocity field. The electron density map obtained from the [SII] 6731/6716 line ratio shows values between 100 cm densities. B 1 2 3 [email protected] Universidade Federal de Santa Maria Universidade Federal do Rio Grande do Sul Rochester Institute of Technology 421 3 the nucleus to 900 cm 3 in a ring of high AGN Posters AGN -1: #227 The SDSS quasars as a testbench for the Gaia fundamental reference frame grid-points Coelho, B.B1 ; Andrei, A.1,2,3 ; Antón, S.4,5 The ESA mission Gaia will furnish a complete census of the Milky Way, delivering astrometry, dynamics, and astrophysics information for 1 billion stars. Operating in all-sky repeated survey mode, Gaia will also provide solar system objects and exo-planets observations and discoveries, plus fundamental physics experiments and measurements of extra-galactic objects. Among the later there will be about 500,000 quasars that will be used to build the reference frame upon which the several independent observations will be combined and interpreted. Not all the quasars are equally suited to fulfill this role of fundamental, fiducial grid-points. Each object will have the error budget defined by its brightness, morphology, and variability. We developed 3 morphological parameters based on the PSF sharpness, circularity and gaussianity, which enable us to distinguish the ”real pointlike” QSOs suitable to establish the Gaia core quasars frame. These parameters are being explored on the spectroscopically certified QSOs of the SDSS DR7, to compare the performance against other morphology classification schemes, as well as to derive properties of the host galaxy. We also present a new method, based on the Gaia quasar database, to derive absolute magnitudes, either in the Gaia and SDSS filters domains, as well as all over the extended optical window. Comparing the obtained morphological classification with the color, the apparent and absolute magnitudes, and the redshift distributions we want to discuss properties of the host galaxies. B 1 2 3 4 5 [email protected] Observatório do Valongo, Universidade Federal do Rio de Janeiro Observatório Nacional, MCT SYRTE, Observatoire de Paris CICGE, Faculdade de Ciências da Universidade do Porto SIM, Faculdade Ciências da Universidade de Lisboa 422 Posters AGN AGN -1: #228 Kinematics and excitation of the nuclear spiral in the active galaxy Arp 102B Couto, G. S.B1 ; Storchi-Bergmann, T.1 ; Axon, D. J.2 ; Robinson, A.2 ; Kharb, P.3 ; Riffel, R. A.1,4 We present a two-dimensional analysis of the gaseous excitation and kinematics of the inner 2.5 ⇥ 1.7 kpc2 of the LINER/Seyfert 1 galaxy Arp 102B, from optical spectra obtained with the GMOS integral field spectrograph on the Gemini North telescope at a spatial resolution of ⇡ 250 pc. Emission-line flux maps show the same two-armed nuclear spiral we have discovered in previous observations with the HST-ACS camera. One arm reaches 1 kpc to the east and the other 500 pc to the west, with a 8.4 GHz VLA bent radio jet correlating with the former. Gas excitation along the arms is low, with line ratios typical of LINERs, and which rule out gas ionization by stars. The gas density is highest (⇡ 500 - 900 cm 3 ) at the nucleus and in the northern border of the east arm, at a region where the radio jet seems to be deflected. Centroid velocity maps suggest that most gas is in rotation in an inclined disk with line of nodes along position angle ⇡ 88 , redshifts to the west and blueshifts to the east, with lower blueshifts correlated with the eastern arm and radio jet. This correlation suggests that the jet is interacting with gas in the disk. This interaction is supported by the gas excitation as a function of distance from the nucleus, which requires the contribution from shocks. Channel maps show blueshifts but also some redshifts at the eastern arm and jet location which can be interpreted as originated in the front and back walls of an outflow pushed by the radio jet, suggesting also that the outflow is launched close to the plane of the sky. Principal Component Analysis applied to our data supports this interpretation. We estimate a mass outflow rate along the east arm of 0.08 0.2 M yr 1 (depending on the assumed outflow geometry), which is between one and two orders of magnitude higher than the mass accretion rate to the active nucleus, implying that there is mass-loading of the nuclear outflow from circumnuclear gas. The power of this outflow is 0.01 0.2 %Lbol . We propose a scenario in which gas has been recently captured by Arp 102B in an interaction with Arp 102A, settling in an inclined disk rotating around the nucleus of Arp 102B and triggering its nuclear activity. A nuclear jet is pushing the circumnuclear gas, giving origin to the nuclear arms. A blueshifted emitting gas knot is observed at ⇡ 300 pc south-east from the nucleus and can be interpreted as another (more compact) outflow, with a possible counterpart to the north-west. B 1 2 3 4 [email protected] Universidade Federal do Rio Grande do Sul Rochester Institute of Technology Indian Institute of Astrophysics Universidade Federal de Santa Maria 423 AGN Posters AGN -1: #229 Two-dimensional Kinematics of the Central Region of NGC 2110 Marlon R. DinizB1 ; Rogemar A. Riffel; Thaisa Storchi-Bergmann We present a two-dimensional mapping of the central region of the active galaxy NGC 2110, using k-band infrared integral field spectroscopy with the Gemini NIFS (Near-infrared Integral Field Spectrograph) at a spatial resolution of ⇡ 24 pc. We present flux distributions and kinematics for the molecular and ionized gas emission lines, as well as the stellar kinematics. The maps for the kinematics and flux distributions of the emitting gas for NGC 2110 were obtained by fitting the H2 2.1218 µm and H I 2.1661 µm emissionline profiles by Gauss-Hermite series. The H2 presents extended emission in the whole field of observation, while the Br is extended only in the southeast – northwest direction. The H2 emission is consistent with emission of gas excited by thermal processes, such as gas heated by X-rays from the AGN or shocks. We estimated an excitation temperature of ⇡ 2100 2700 K for H2 emitting gas. The masses of molecular and ionized gas were estimated from fluxes of the H2 2.1218 and Br emission lines as MH2 ⇡ 1.4 ⇥ 103 M and MH II ⇡ 1.7 ⇥ 106 M , respectively. The gas velocity fields present a similar rotation pattern than those observed for the stars. In addition, the H2 velocity field presents other kinematic components. Two spiral structures are observed in blueshifts to the north of the nucleus and redshifts to the south of it. If these kinematic structures are originated from emission of gas located in the plane of the galaxy, they can be interpreted as gas flows towards the nucleus (inflows) of the galaxy. In this case, the mass inflow rate is estimated to be ⇡ 4 ⇥ 10 4 M yr 1 . Another kinematic component observed for H2 emitting gas was interpreted as an ejection of gas from the nucleus (outflows) within a bi-cone with a mass outflow rate of ⇡ 4.66 ⇥ 10 B 1 4 M yr 1 . [email protected] Universidade Federal de Santa Maria 424 Posters AGN AGN -1: #230 Unveling the LINER nature of NGC1052 B1 Diniz, S. I. F. ; Riffel, R.1 ; Pastoriza, M. G.1 ; Riffel, R. A.2 , Storchi-Bergmann, T.1 ; Diniz, M.2 Early type galaxies are known to have a diverse and rich interstellar medium, but the excitation mechanism of their interstellar gas are still being investigated. One of these interesting objects is NGC 1052, it is an E4 galaxy and classified as a typical LINER harboring a stellar rotating disk. However, the central region is spectroscopically unusual with broad optical emission lines. NGC 1052 has been subject of many studies, but the nature of its emission line gas remains unclear. According to recent studies NGC 1052 exhibit H↵ luminosities an order of magnitude above that estimated for an evolved population of extreme horizontal branch stars. Their H↵ equivalent widths and optical-to-near infrared (NIR) spectral energy distributions are consistent with them being young stellar clusters aged < 7 Myr, and according to previous works, NGC 1052 may have experienced a merger event about 1 Gyr ago. There are mainly three possibilities to explain LINER’s spectra: i) post asymptotic giant branch stars (post-AGB) that ionize their rapidly expanding shells, (ii) active galactic nuclei (AGNs) powered by the in fall of matter into an accretion disk, and (iii) shocks. The main difference between the stellar population (SP) of active and non-active galaxies is an excess of intermediate age stars in the former. Besides, NIR stellar population studies have revealed that the continuum of active galaxies is dominated by the contribution of intermediate age stellar populations. Hot dust emission unresolved is also commonly detected in NIR nuclear spectra of galaxies Seyfert and LINERs. Therefore, the NIR spectral region is very adequate to probe the 3 scenarios. Aimed to discriminate the dominant ionizing source of NGC 1052 we present preliminary results of high spatial resolution integral field spectroscopy, taken with gemini NIFS to map the dominant stellar population, as well as disentangling the featureless and hot dust components. B 1 2 [email protected] Universidade Federal do Rio Grande do Sul Universidade Federal de Santa Maria 425 AGN Posters AGN -1: #231 IFU spectroscopic analysis of M81 Giansante, L.B1 ; Steiner, J. E.1 ; Ricci, T. V.1 New spectrographs with IFUS (Integral Field Units) allow us to study extended objects very precisely by constructing and analyzing data cubes. Specially, the study of Active Galactic Nuclei (AGN) and the inner region of their host galaxy can take much advantage from these techniques. We present in this work our analysis of M81, a LINER galaxy classified as SA(s)ab at a distance of 3.7(5) M pc. We re-analyze data published by Schnorr-Müller et al. (2011), but now we are focusing on the nucleus of this object (7 ⇥ 5 arcsec2 ) and we intend to apply new techniques of noise removal, so that we can possibly obtain more accurate information. After the data reduction, we applied the Butterworth filter (spacial and spectral) in order to remove the high frequencies noise, that are incompatible with the PSFs. Then, we identified some low frequencies noise that are characteristic of the detector and are called instrumental fingerprint. It was done with the PCA (Principal Component Analysis) Tomography technique (Steiner et al. 2009), that is very efficient in identifying patterns and correlations. Using this same technique we could remove this kind of noise. After removing the noise, we applied the Richardson-Lucy deconvolution with 10 iterations and Gaussian PSF with FWHM = 0, 8700 , took from the broad component of H↵. Finally, we used the PCA again and we saw that the data quality was much better. The eigenvector/tomogram 1 shows the basic characteristics of the spectrum and the image of the object, since it has the largest part of the variance (93.5%). The eigenvector 2 shows strong emission of [OI] and H↵, that are typical of LINERs. The eigenvector 3 shows the same characteristic, but its continuum is bluer and it is deslocated about 0.400 . The other eigenvectors show kinematic characteristics (inflows and outflows) that are compatible with Schnorr-Müller’s interpretation (2011). By observing the second and third eigenvectors, we propose that the second AGN is the first reflected by free electrons in the least obscured ionization cone. This interpretation has been proposed by Ricci et al. (2011) for the NGC 7097 galaxy. In addition, eigenvectors 1 and 2 show the emission line [N II] 5577Å. This line allows us to determine a gradient of the gas temperature of the object. B 1 [email protected] Institute of Astronomy, Geophysics and Atmospheric Sciences - University of São Paulo (IAG - USP) 426 Posters AGN AGN -1: #232 A nuclear molecular ring in Mrk 1066 revealed by PCA tomography Hennig, Moiré G.B1 ; Riffel, Rogemar A.1 We used the PCA (Principal Component Analysis) tomography technique to analyze J and K band datacubes for the inner ⇡ 350 pc radius of the Seyfert 2 galaxy Mrk 1066, obtained with the Gemini/NIFS (Near-Infrared Integral-Field Spectrograph) at a spatial resolution of ⇡ 35 pc. In the first eigenvector, both in the J band as the K band is observed the emission of AGN and continuous because the stars of the bulge of the galaxy corresponding to more than 95% of the variance of the data for the two bands. The second eigenvector for the K band presents a anti-correlation between the blue part and the red part the spectrum. In tomogram corresponding to this eigenvector, it is observed that the nuclear emission is dominated by red part, and thus eigenvector interpret this as being caused by the dust toroid core. A rotating disk is observed in eigenspectrum 2 (in J band) and eigenspectrum 3 (in K band) and their respective tomograms. It is noted that the emission lines in eigenvector 3 in the J band and K band in eigenvector 4 is correlated with structures seen in radio. An anti-correlation between the emission lines [Fe II] and the emission Pa is observed in the eigenvector 4, which shows that the tomogram corresponding emission [Fe II] is extended along the radio jet, whereas the emission Pa is more compact and originated from regions near the core. The analysis of the fifth eigenspectrum and its tomogram shows that H2 emission shows a ring surrounding the nucleus, spiral arms which run north and south. Some cinematic effects appear as anti-correlations between the blue and red wings of the emission lines in eigenspectrum that contribute less than 0.05% of the variance of the data in the two bands. B 1 [email protected] Universidade Federal de Santa Maria 427 AGN Posters AGN -2: #233 Physical properties of FeII emission in active galactic nuclei Marinello, M. A. O.B1 ; Rodrı́guez-Ardila, A.2 Among the spectral lines emitted by the broad line region (BLR) in active galactic nuclei (AGN) the FeII emission is the most prominent one and therefore constitutes one of the most important contributors to the cooling of that region. The large number of lines (⇠25000) forms a pseudo-continuum that extends from the ultraviolet to the optical region, difficulting the identification of individual lines. In the near infra-red (NIR) the FeII emission is still intense but free of blending effects opening a window to a more consistent analysis of that emission. With the aim of studying the FeII in the range 0.8-1.2 µm in a sample of 17 AGNs we utilize a semi-empirical template obtained from IZw1, which is considered the prototype of FeII active galaxy emitter. Iron Templates are important tools in the study of that emission because they allow to quantify, subtract and study it. That particular template reproduces accurately the FeII in IZw1 and it is now applied, by the first time in other AGNs. In this work we made a detailed analysis of the width and intensity of the FeII lines in order to derive the most probable location of the emitting region and to study the formation mechanisms of that ion, respectively. We compare the width of the individual FeII lines with that of other lines emitted in BLR. Our results show that the FWHM of iron systematically approaches to that of OI and CaII and is considerably smaller than that of Hydrogen, confirming previous assumptions that the gas responsible for the FeII emission is the outer portion of the BLR. We correlate the strength of the NIR, optical and UV iron lines to derive the relative contribution of the different mechanisms that produces that emission. We found that in all cases the Ly↵ fluorescence plays an important role, being a process that needs to be considered to fully understand this complex emission. B 1 2 [email protected] Universidade Federal de Itajubá Laboratório Nacional de Astrofı́sica 428 Posters AGN AGN -2: #234 The Architecture of the Active Galactic Nuclei of NGC 1068 May, DanielB1 ; Steiner, J.1 ; Menezes R. B.1 ; Ricci T. V.1 NGC 1068 is the brightest and most studied AGN in the sky. It’s study motivated the development of the Unified Model for AGN as it is the prototype of an obscured Seyfert 1 galaxy. The opportunity of studying such an object with IFU spectrographs in the near infrared allow us to understand the details of how gas is being fed to the central black hole and how the gas is being ionized and ejected from the center. We reanalyzed data taken from the SINFONI (VLT) and NIFS (GEMINI North) public archives, in the HK bands with spatial resolution of ⇠0,1 arcsec (1,7 pc/spaxel). We concentrated our analysis on the molecular H2 lines, the low ionization line [Fe II] and the high ionization line [Si VI]. The analysis shows very distinct behavior for the different lines. In particular we found a clear structure resembling a “glowing-hourglass” shape for the low velocity [Fe II] emission, while the high velocity emission fills the “hourglass”. The shape of this image suggests that the dusty torus and the ionization axis, possibly associated to the central accretion disk, are not co-planar. The primary wind is probably originated from this asymmetry while the secondary wind is likely to be originated from an H2 emitting cloud, about 1” to the north of the AGN, impacted by the primary wind and ionized by the central source. B 1 [email protected] Instituto de Astronomia e Geofı́sica IAG - Sao Paulo University 429 AGN Posters AGN -2: #235 Evolutionary Sequence for Seyfert Galaxies: A Point of View from Dust Geometric Distribution Mendoza-Castrejón, S.B1 ; Dultzin, D.1 ; Krongold, Y.1 ; González, J. J.1 ; Elitzur, M.2 We analyze the mid-infrared (MIR) spectra of 39 Seyfert galaxies observed with Infrared Spectrograph aboard the Spitzer Space Telescope, our sample consists of 16 Seyfert galaxies type 1 (Sy1) and 23 Seyfert galaxies type 2 (Sy2). Their circumgalactic environment was studied by Dultzin-Hacyan et al. (1999) who concluded that Sy2s show higher frequency of nearby neighbors of similar mass than Sy1s. In order to elucidate the characteristic of the obscuring torus in this sample of galaxies we study the emission of the Silicate dust that dominates the MIR spectra of galaxies. This dust can produce both the continuum and prominent spectral features at 10 and 18 µm. The strengths of the two silicate features together are sensitive to the dust distribution. We measure the strength of the emission or absorption of the Silicate features to find if there is a correlation between the geometric distribution of the circumnuclear dust and the incidence of companions. For Sy1s galaxies we find that regardless of the presence of a companion, the majority have a clumpy dust geometric distribution. In the case of Sy2s galaxies, those with one or more companions have mostly smooth dust distribution, whereas for those without companions we find that the geometric distribution of dust can be either smooth or clumpy. We discuss the implications of this result within the evolutionary model for Seyfert galaxies (Krongold et al. 2003). B 1 2 [email protected] Instituto de Astronomia, Universidad Nacional Autonoma de México, Mexico City Mexico Departament of Physics and Astronomy, University of Kentucky, Lexington, KY 430 Posters AGN AGN -2: #236 Studying the kinematics of the jet of 3C279 using the method Cross-entropy Motter, J. C.B1 ; Abraham, Z.1 VLBI images of blazars are characterized by the presence of jets that have enhanced emission regions and seem to recede from the central core with apparently superluminal velocities. It is still under discussion if the movement of these jet components is ballistic or not, although it is well established that different components of the same jet may have different velocities. The determination of these velocities depends strongly on the identification of the same components at different epochs, and also on a reliable model for their positions. The components are, in general, taken as two dimensional gaussians, and to identify them, the procedures commonly used are subjective in the sense that they depend on initial conditions. Recently, Caproni, Monteiro & Abraham (2011) adopted the method Cross-entropy (CE) that allows the fitting of an unlimited number of components and determines their parameters without the need of initial conditions. In this work we used this method to analyze the images of the quasar 3C279 obtained at 15 GHz by the VLBA. We used the method CE to fit original components on the image plane and then convolved them with the characteristic restoring beam for each epoch in order to compare our models with the observations. With this procedure we were able to identify the components of the jet of 3C279 and follow them along different epochs to estimate their proper motions and ejection times. B 1 [email protected] IAG - Universidade de São Paulo 431 AGN Posters AGN -2: #237 Probing AGN accretion through microlensing Neri-Larios, D. M.B1 ; Webster, R. L.1 ; Floyd, D. J. E.1 ; O’Dowd, M.2 ; Bate, N. F.3 ; Labrie, K.4 Understanding quasar accretion is both at the frontier of new physics, and essential in understanding the driving force behind the great power of quasars and their energetic feedback onto their galactic environments. However, the accretion disks are at micro-to-nano arcsecond scales, unresolvable from Earth. Gravitational microlensing of quasars provides statistical information on the microarcsecond structure of the lensed quasar. By measuring the flux ratio in two of the lensed images and comparing to a lens models for the intervening galaxy, we can establish upper limits on the size of the emission region. The principle is now well-established, with variability (due to caustic-crossing events) and statistical modelling of the microlens population giving consistent results. Both techniques have shown tantalising evidence that the emission region does not fit the standard accretion disk model, being larger, and with flatter profiles (change of source size with wavelength), than expected. In this project, we will observe the ratio of the quasar continuum emission at a range wavelengths and at least with three samples in three different instruments: VLT/X-shooter, HST/WFC3 and WiFeS/IFU. With all these data we pretend obtain the ratio of microlensing magnifications. B 1 2 3 4 [email protected] School of Physics, The University of Melbourne Astronomy Department, Columbia University School of Physics, The University of Sydney Gemini Observatory 432 Posters AGN AGN -2: #238 Spectral Properties of Narrow Line Seyfert 1 galaxies Oio, G. A.B1,2 ; Vega Neme, L. R.2 ; Schmidt, E.1,2 ; Ferreiro, D.2 Narrow Line Seyfert 1 (NLS1) are a subclass of Active Galactic Nuclei (AGN) with Seyfert 1 characteristics but without prominent broad lines. We selected a sample of 130 NLS1s up to z = 0.1 from Sloan Digital Sky Survey Data Release 8 to study both stellar and non-stellar content in AGNs. By using spectral synthesis techniques, we quantify the non-stellar continuum of NLS1s. We also derive some of their most relevant parameters, such as black hole masses and accretion rates, as well as those of their host galaxies, such as kinematics and state of the ionized gas. Finally, we show some results concerning a possible link between the inner parts and large scale properties of NLS1s. B 1 2 [email protected] Instituto de Astronomı́a Teórica y Experimental (IATE) Facultad de Matemática, Astronomı́a y Fı́sica, Universidad Nacional de Córdoba 433 AGN Posters AGN -2: #239 Diagnostic diagrams with polycyclic aromatic hydrocarbons in diferent types of galaxies Seditsira QuinteroB1 ; Andrés F. Ramos P.2 ; Mario-A. Higuera-G.3 ; J. R. Martı́nes-Galarza4 ; Alexander Garzón1 In this contribution, we investigate the processes associated to star formation activity in local AGN, and infrared galaxies. In this way, spectroscopic and photometric data were used to discriminate these processes in a sample of starburst, luminous infrared galaxies-LIRGs, ultraluminous infrared galaxies-ULIRGs, and also in Seyfert, quasars and radio, galaxies. The diagnostic diagrams using the PAH features (6.2, 7,7, 8.6, 11,3 and 17 µm) allow us to discriminate the behavior of starbursts and LIRGs-ULIRGs objects from Seyfert and quasar galaxies. The study also let us determine physical parameters, in galaxies with signs of star formation, taking into account the intensity of the PAH emissions and continuum luminosities. Our study of this local sample of galaxies could be relevant in high redshift studies. B 1 2 3 4 [email protected] Department of Mathematics, National University of Colom- bia, Ciudad Universitaria, Bogota D.C.,Colombia Department of Physics, National University of Colombia, Ciudad Universitaria, Bogota D.C.,Colombia National Astronomical Observatory, National University of Colombia, Ciudad Universitaria, Bogota D.C.,Colombia Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-51, Cambrigde, MA 02138, USA 434 Posters AGN AGN -2: #240 Molecular hydrogen and [Fe II] in active galactic nuclei - III. Low-ionization nuclear emission-line region and star-forming Riffel, R.B1 ; Rodrı́guez-Ardila, A.2 ; Aleman, I.1 ; Brotherton, M. S.3 ; Pastoriza, M. G.1 ; Bonatto, C.1 ; Dors, O. L.4 We study the kinematics and excitation mechanisms of H2 and [FeII] lines in a sample of 67 emission-line galaxies with Infrared Telescope Facility SpeX near-infrared (NIR, 0.8-2.4µm) spectroscopy together with new photoionisation models. H2 emission lines are systematically narrower than narrow-line region (NLR) lines, suggesting that the two are, very likely, kinematically disconnected. The new models and emission-line ratios show that the thermal excitation plays an important role not only in active galactic nuclei but also in star forming galaxies. The importance of the thermal excitation in star forming galaxies may be associated with the presence of supernova remnants close to the region emitting H2 lines. This hypothesis is further supported by the similarity between the vibrational and rotational temperatures of H2 . We confirm that the diagram involving the line ratios H2 2.121µm/Br and [FeII]1.257µm /Pa is an efficient tool for separating emission-line objects according to their dominant type of activity. We suggest new limits to the line ratios in order to discriminate between the different types of nuclear activity. B 1 2 3 4 [email protected] Departamento de Astronomia, Universidade Federal do Rio Grande do Sul, Av. Bento Gonçalves 9500, Porto Alegre, RS, Brazil Laboratório Nacional de Astrofı́sica/MCTI - Rua dos Estados Unidos 154, Bairro das Nacões, CEP 37504-364, Itajubá, MG, Brazil Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA Universidade do Vale do Paraı́ba, Av. Shishima Hifumi 2911, CEP 12244-000, São José dos Campos, SP, Brazil 435 AGN Posters AGN -2: #241 Nuclear outflows in the Seyfert 2 galaxy NGC 5929 Rogemar A. RiffelB1 ; Thaisa Storchi-Bergmann2 ; Rogério Riffel2 We present two-dimensional (2D) near-infrared spectra of the inner 300 ⇥ 300 of the Seyfert 2 galaxy NGC 5929 at a spatial resolution of ⇠20 pc obtained with the Gemini Near infrared Integral Field Spectrograph. We report the discovery of a linear structure ⇠ 300 pc in extent and of ⇠ 50 pc in width oriented perpendicular to the radio jet, showing broadened emission-line profiles. While over most of the field the emission-line profiles have full-widths-at -half-maximum (FWHM) of ⇡210km s 1 , at the linear structure perpendicular do the radio jet the emission-line FWHMs are twice this value, and are due to two velocity components, one blueshifted and the other redshifted relative to the systemic velocity. We attribute these velocities to an outflow from the nucleus which is launched perpendicular to the radio jet. This means that: (1) both ionizing radiation and relativistic particles are escaping through holes in the torus perpendicular to the radio jet; and/or (2) the torus is also outflowing, as proposed by recent models of tori as winds from the outer parts of an accretion flow; or (3) the torus is absent in NGC 5929. B 1 2 [email protected] Universidade Federal de Santa Maria Universidade Federal do Rio Grande do Sul 436 Posters AGN AGN -3: #242 Estimating the size of the emitting region in the lens quasars HE0047-1756 and SDSS1155+6346 Rojas K.B1 ; Motta V.1 ; Mediavilla E.2 ; Falco E.3 ; Muñoz J. A.4 We search for microlensing effect in the gravitational lens systems HE0047-1756 and SDSS1155+6346 using spectra obtained with Magellan/IMACS (2007) and MMT/Blue-Channel (2008). Comparing the magnitude difference in the emission line cores with the magnitude difference in the continuum under de lines we found evidence of chromatic microlensing in HE0047-1756 and SDSS1155+6346. This will be used to estimate the size of the emitting region. B 1 2 3 4 [email protected] Universidad de Valparaı́so Instituto de astrofisica de Canarias Whipple Observatory, Smithonian Institution Universidad de Valencia. 437 AGN Posters AGN -3: #243 The Proximity Effect toward z > 3.5 QSOs: Assesing systematics with XSHOOTER data Paula SánchezB1 ; Sebastian Lopez1 ; Joseph Hennawi2 The ESO Large Programme ”Quasars and their absorption lines” is currently assembling a legacy dataset of 100 z > 3.5 QSO spectra observed with the UV/VIS/NIR spectrograph XSHOOTER mounted on the ESO Very Large Telescope. One of the LP objectives is to constrain the UV background and the QSO environments for the first time at z > 3.5 using the proximity effect, i.e., the drop in the incidence of Ly-alpha forest absorption lines at za bs ⇠ zQ SO due to QSO ionizing photons. In this talk I will present a preliminary study of well- known uncertainties like QSO redshifts and QSO SEDs, using a significant fraction of the data already at hand. B 1 2 [email protected] Universidad de Chile Max Planck Institute for Astronomy 438 Posters AGN AGN -3: #244 Correlating X-rays, UV and optical emission from the accretion disk in the nucleus of NGC1097 Schimoia, Jaderson S.B1 ; Storchi-Bergmann, Thaisa1 ; Eracleous, M.2 ; Grupe, D.2 ; Peterson, B. M.3 Broad Balmer emission lines from active galactic nuclei are thought to be originated in gas clouds of the socalled broad line region (BLR) surrounding the central supermassive black hole (SMBH). Its distance from the SMBH ranges from a few light-days to a few light-weeks, as determined from reverberation mapping. In the case of the LINER nucleus of NGC 1097 the broad emission lines are double-peaked, and attributed to emission by the outer parts of an accretion disk. Our group has been monitoring the variation of this double-peaked profile for more than twenty years. In a previous recent work, we found a short time scale variability of the profile of the order of 7 days, which we have concluded to be approximately the lighttravel time between the nucleus and a typical radius of the emitting part of the disk (about 1000 gravitational radii). This result, plus the typical LINER line ratios of the more external emitting gas suggest that the line emission in the accretion disk could be driven by a central radiatively inefficient accretion flow (RIAF), that emits mainly a hard continuum (in particular X-rays). In this work we present a test of this scenario, as follows. We have monitored the emission from the nucleus and accretion disk of NGC 1097, from August 2012 to February 2013, in three bands: (1) in the optical via long-slit spectroscopy with the SOAR telescope, to observe double-peak profile; (2) in X-rays and (3) in the UV, both with the Swift satellite in order to observe the emission at these wavelengths which probably originate in the central ionizing RIAF. We present the light curves for these three bands, as well as results of the cross-correlation between them, discussing the implications for the reverberation scenario. In addition, we present also the evolution of the parameters of the accretion disk model which best reproduces the observed double-peaked profile variations. B 1 2 3 [email protected] Universidade Federal do Rio Grande do Sul Pennsylvania State University Ohio State University 439 AGN Posters AGN -3: #245 Feeding and Feedback around the active nucleus of the Seyfert galaxy Mrk766 Schönell, A. J. J.B1 ; Riffel, R. A.2 ; Storchi-Bergmann, T.1 ; Winge, C.3 We have mapped the emission-line flux distributions and ratios as well as the gaseous kinematics of the inner 450 pc radius of the Seyfert 1 galaxy Mrk 766 using integral field near-IR J- and Kl -band spectra obtained with the Gemini-North instrument NIFS at a spatial resolution of 60 pc and velocity resolution of 40 km s 1 . Emission-line flux distributions in ionized and molecular gas extend up to ⇡ 300 pc from the nucleus. The coronal [S IX] 1.2523µm line emission is resolved, being extended up to 150 pc from the nucleus. At the highest flux levels, the [Fe II] 1.257µm line emission is most extended to the south-east, while the H2 2.122µm line emission is most extended at the approximately perpendicular direction, to the south-west. The H2 gas has an excitation temperature Texc = 2360 ± 45 K and its emission is dominated by thermal processes, mainly due X-ray heating by the active nucleus. The [Fe II] emission seems also to be produced by these thermal processes, but with contribution also from shocks, as evidenced by the correlation between enhanced [Fe II]/[P II] line ratios, increased [Fe II] velocity dispersion ( ) and radio extended emission to the south-east of the nucleus. The gas velocity field is dominated by rotation, and the fit of a rotating disk model to the Pa velocity field gives a position angle of 80 for the line of nodes, which is the approximate orientation of the most extended H2 emission. This fact, combined with the low H2 - close to the velocity resolution of the data, supports a location of the H2 emitting gas in the galaxy plane, and its association with the feeding of the supermassive black hole (SMBH). There is about 103 M of hot H2 , implying ⇡ 109 M of cold molecular gas in the inner 450 pc radius. The higher (150 km s 1 ) for [Fe II] to the south-east of the nucleus, and the presence of both blueshifts and redshifts in the channel maps at the corresponding locations, support the presence of an outflow, with an axis lying close to the plane of the sky. The ionized gas outflow rate is estimated to be 2.18 M yr 1 , and the power of the outflow 0.011 Lbol . The mass of the SMBH is estimated to be ⇡ 1 ⇥ 10 M . 7 B 1 2 3 [email protected] Universidade Federal do Rio Grande do Sul Universidade Federal de Santa Maria Gemini Observatory 440 Posters AGN AGN -3: #246 Characterization blazars environment PG1553 +113 and 3C66A from GMOS data in the bands i ’ and r’ Juanita Torres ZafraB1 ; Sergio Aldo Cellone; Ileana Andruchow Blazars are active galactic nuclei that, because of their particular orientation with respect to the observer, are characterised by beamed electromagnetic emission, which is dominated by the relativistic jet. It is thus challenging to detect either continuum or line radiation from the nucleus or from the host galaxy; in many cases this prevents the measurement of a spectroscopic redshift. However, the analysis of their environments may give valuable information, considering that galaxies in the blazar’s field could share physical and chemical properties with the host galaxy, besides having a similar redshift. We have thus undertaken a photometric study of the galaxies in the fields of the blazars PG1553+113 and 3C66A, based on r’ and i’ images taken with the GMOS instrument (multi-object spectrograph and camera) at Gemini North 8m telescope. Our goal is to look for concentrations of galaxies around both blazars in order to have a first knowledge of the general characteristics of their immediate environments. B 1 [email protected] Instituto de Astrofı́sica de La Plata (IALP), Universidad Nacional de La Plata, Argentina 441 AGN Posters AGN -3: #247 FHILs in Seyferts and Liners in the optical spectra Portilla, J. G.1 ; Rodriguez, A. M.2 ; Vera, R. J. CB3 We present the main results from a selection of optical spectra of Active Galactic Nuclei (AGNs) from the Sloan Digital Sky Survey (SDSS) with detectable emission of forbidden high ionization lines (FHILs), better known as coronal lines. The presence of these lines gives evidence of a nuclear environment with very unique characteristics such as ionization potentials equal or greater than 100eV. Results continue indicating that FHILs are not observed in LINER type galaxies, nonetheless, for the first time a catalog of more than 300 unreported Seyfert 1 and Seyfert 2 type galaxies with FHILs is presented. Using these objects and another 80 more reported by Gelbord, Ekens, Osterbrock and others, we study the following line flux ratios and their distribution for Sy1 and Sy2 galaxies: [Fe V II ] 6087/[Fe X] 3426/[Fe V II ] 6087. B 1 2 3 [email protected] Observatorio Astronomico Nacional, Universidad Nacional de Colombia Observatorio Astronomico Nacional, Universidad Nacional de Colombia Observatorio Astronomico Nacional, Universidad Nacional de Colombia 442 6374; [Fe X] 6374/[Fe XI ] 7892 and [Ne V ] Posters AGN AGN -3: #248 A physical model for AGN feedback: the role of BH spin and magnetic field Garrido, F.B1 ; Padilla, N.1 ; Cora, S.2 We study the effects of feedback from Active Galactic Nuclei (AGN) on cosmological samples of galaxies using a semi-analytic model of galaxy formation (SAG) within a dark matter N-Body simulation. The SAG model allows us to follow the evolution of the black hole mass and spin. In the base model the process of mass accretion and AGN feedback have been included in a phenomenological way, which means that they scale to match certain observational data. We now explore a more physical description of the feedback process, with a new model for the BH magnetosphere which invokes the Magnetic Coupling (MC) between the BH and its surrounding disc, and allows the existence of the Blandford-Znajek (BZ) effect, associated with jet production. The new model allows us not only to match the shape of the galaxy luminosity function by concentrating the effect of AGN feedback on luminous elliptical galaxies, and allowing intermediate mass galaxies to form slightly more stars than in the base model, it also allows us to make successful predictions for the quasar and radio luminosity functions, since the BZ effect is present in galaxies where their spin is adequate; these predictions are now physically related to the evolutionary history of the model galaxies. B 1 2 [email protected] Instituto de Astrofı́sica, Pontificia Universidad Católica de Chile Facultad de Ciencias Astronómicas y Geofı́sicas, Universidad Nacional de la Plata 443 AGN Posters AGN -3: #249 Optical stellar and emission gas kinematics of the Seyfert 2 Circinus galaxy Rodrigues, F. P.B1 ; Rodrı́guez-Ardila, A.2 Among the subjects that have generated more discussions and observational efforts in the last years, in the context of active galactic nuclei, are stellar formation and stellar and gas dynamics in the circumnuclear region (<100 pc) of galaxies. The correlations between the galactic nuclear properties, such as the central black-hole mass, and the major scale properties, such as the bulge mass and luminosity, represent a fundamental link concerning galaxy evolution. The Circinus galaxy, at a distance of 4.2±0.8 Mpc, is an ideal object to contribute to this discussion because of its proximity and also because it hosts a Seyfert 2 nucleus and a ring of intense stellar formation at a scale of 100 – 200 pc. Previous studies show that a fraction of that gas originates outside the galaxy disc, resembling outflowing gas aligned to the ionization cone. In spite of the high volume of data in the X-ray, infrared and radio frequencies available for this object, very little has been studied in the visible region. In this study, SOAR medium and high resolution spectroscopy in the region 3200-7000 Å is used to investigate, for the first time, the emission gas kinematics of the inner 200 pc of the galaxy, by means of the H↵, [NII], [OIII] and [OII] lines at an angular resolution of 10 pc. Due to the presence of stellar absortion lines in the spectra (Ca H and K, MgI, NaI, H ), the stellar population, its kinematics and luminosity and the mass bulge are, for the first time, determined. Measurements of the emission lines fluxes as well as dust extinction and excitation maps of the gas are also presented for the first time at such spatial and spectral resolution for the nucleus and circumnuclear regions of that source. B 1 2 [email protected] Universidade Federal de Itajubá Laboratório Nacional de Astrofı́sica 444 Posters AGN AGN -3: #250 Integral Field Spectroscopy SINFONI observation of AGN at z ⇠ 1.6 San Martı́n, A.B1 ; Gavignaud, I. The aim of the study is to obtain properties of distant low luminosity active galactic nuclei (AGN). In terms of galaxy evolution, nuclear activity seems to play an important role. AGN feedback processes may have impacts on the predictions for galaxy properties, as these processes are thought to affect the efficiency of star formation. Therefore it becomes interesting to study the AGN host galaxy. SINFONI is an adaptive optics assisted near infrared integral field spectrometer mounted to the ESO VLT. The integral field spectroscopy allows us to explore spatially extended sources, to resolve properties of high redshift galaxies. We present the observation of two low luminosity AGNs from which we want to disentangle the properties of it’s host galaxy. The selected galaxies to be studied were observed with SINFONI from VLT at H band. A first data set reduction was perform using the ESO-SINFONI pipeline, additionally was used some Python routines in order to improve some reduction steps. As a result we obtain the data-cube and the spectrum from which can be clearly observed the H↵ broad emission line. The deconvolution in the AGN and host galaxy components is the next step in this study. B 1 [email protected] Universidad Andres Bello 445 446 Cosmology COS -1: #251 Constraining Cosmological Parameters from Galaxy Clusters Michel Aguena da SilvaB1 ; Marcos Lima1 Over the past years, the abundance of galaxy clusters has been recognized as a powerful cosmological probe, especially to study models of cosmic acceleration. This study aims to investigate the possibility of constraining dark energy parameters through the abundance of galaxy clusters as a function of their mass and redshift. We analyze different mock catalogs of dark matter halos and use a Monte Carlo Markov Chain (MCMC) sampler to estimate cosmological parameters and their uncertainties. We expect to apply these techniques to real cluster catalogs in the near future, including those from the Dark Energy Survey (DES). B 1 [email protected] Institute of Phyisics, University of Sao Paulo 447 Cosmology Posters COS -1: #252 Improving the Modeling and Cosmological Constraints of the Galaxy Angular Correlation Function Camacho H. O.B1 ; Lima M.1 The advent of wide-area photometric galaxy surveys brings new practical challenges in cosmological analyses. These surveys will gain in area and depth, in exchange for a poorer determination of radial positions. In this context, the study of the angular clustering of galaxies appears as a valuable tool to extract cosmological information from the evolution of cosmic structures. We present a general formalism for the angular correlation function (ACF) theoretical model on FLRW space-times including bias, photo-z uncertainties and redshift space distortions. Based on [Sobreira et. al. (2010) PRD 84] and [Crocce et. al. (2011) MNRAS 414] we show the appropriate small angle limit of the general result. In this limit and restricting the analysis to a spatially flat model we also present a comparison between different approaches to perform its numerical computation in order to obtain cosmological constraints implementing Monte Carlo Markov Chain (MCMC) sampling methods. B 1 [email protected] Departamento de Fı́sica Matemática. Instituto de Fı́sica. Universidade de São Paulo. 448 Posters Cosmology COS -1: #253 Central Dominant Galaxies and the evolution of their host Galaxy Clusters Caretta, C. A.B1 ; Andernach, H.1 ; Trejo-Alonso, J. J.1 ; de Anda-Suárez, J.2 ; Muñiz-Torres, M. A.2 ; Hernández-Aguayo, C.2 ; Santoyo-Ruiz, H.2 ; Islas-Islas, J. M.1 We have studied a sample of 50 galaxy clusters, all with more than 150 spectroscopic confirmed member galaxies, from all Bautz-Morgan types, in order to determine the importance of the brightest cluster members (BCMs) and their relation to the structure and dynamical state of their host clusters. Strict tests for membership and the presence of substructure were applied. Near-infrared data were used for photometry and astrometry, which allowed us to rank the member galaxies in order of their stellar content. We found a clear correlation between the evolutionary state of the BCMs, represented by their absolute magnitude, morphology and luminosity gaps, and the dynamical state of their host clusters. More massive clusters present more than one dominant galaxy, while the less massive ones present only one, at most. This correlation goes in the sense that most of the evolution of Central Dominant Galaxies occurs in groups that are doomed to merge and form clusters. B 1 2 [email protected] Departamento de Astronomı́a, DCNyE-CGT, Universidad de Guanajuato Departamento de Fı́sica, DCI-CLE, Universidad de Guanajuato 449 Cosmology Posters COS -1: #254 New Catalogues of Superclusters of Abell/ACO Galaxy Clusters up to z ⇠ 0.15 Chow, M.B1 ; Andernach, H.1 ; Caretta, C. A.1 We present two new catalogues of superclusters of galaxies within a redshift of z = 0.15, constructed using the Abell/ACO cluster redshift compilation by one of us (H.A.). One is the all-sky Main SuperCluster Catalogue (MSCC), the other is the Southern ( < 17 ) SuperCluster Catalogue (SSCC) which includes the sup- plementary S-clusters. These are currently the deepest all-sky supercluster catalogues based on optical data. A tunable Friends-of-Friends (FoF) algorithm was used in order to take into account the selection functions of the samples. For the MSCC, a subsample of 3410 A-clusters (92% of them with measured redshift) was used, yielding 601 superclusters with multiplicities between 2 and 42. For the construction of the SSCC two used both the 1227 A-clusters and 1177 S-clusters, 90% of them with measured redshifts. From the latter we derived 425 superclusters with multiplicities between 2 and 39. A comparison of the two catalogues revealed that the inclusion of the S-clusters tends to fragment very rich superclusters (m>20) into more compact structures due to the smaller linking length implied by the higher space density of clusters in this region of sky. Other effects of the inclusion of S-clusters are: new superclusters with S-clusters around A-cluster cores (12.6%); the formation of bridges of S-clusters between A-clusters (1.2%); and the addition of new superclusters formed by S-clusters only (25.4%). An analysis of the space density of clusters shows that S-clusters appear to inhabit lower-density regions than do A-clusters. We also determined morphological parameters for the superclusters, based on ellipsoid fits and the calculation of Minkowski Funtionals, with the result that 39% of the rich (m>5) superclusters are prolate ellipsoids and 61% are oblate ones. The cumulative multiplicity functions of both catalogues follow very closely a power law, with exponent 2.0 for MSCC and 1.9 for SSCC. This power law appears to be consistent with a fractal distribution of the Large-Scale Structure, up to a scale of almost 150 h701 Mpc. This power law is clearly inconsistent with the cumulative multiplicity function we derived for a supercluster catalogue based on a simulated sample of randomly distributed clusters. It is also inconsistent, though less significantly, with an application of our F-o-F algorithm applied to the Bolshoi cosmological simulation of the evolution of the large-scale structure of the universe. B 1 [email protected] Departamento de Astronomia, Universidad de Guanajuato 450 Posters Cosmology COS -1: #255 A new method to estimate distances to Type II SNe Alejandro ClocchiattiB1 ; Ósmar Rodrı́guez1 ; Mario Hamuy2 We present some standardizations of Type II plateau supernova (SN IIP) brightness, based on the Expanding Photosphere Method (EPM). A difference with the EPM, is that we do not define a temperature, which requires parameters provided by Radiative Transfer theory of SN photospheres, but base our approach in the empirical calibration of brightness with color. We test the method with a sample of SNe IIP with a well constrained shock breakout epoch, well determined host galaxy distance and our own estimates of extinction by dust in the hosts. For the latter, we develop a method to measure reddening using SN cooling curves. We also propose an alternative way to obtain a RV for SNe IIP. In one approach, akin to a C-M Diagram, we use five SNe IIP meeting these three requirements to obtain dispersion of 0.4 magnitudes in the distance. The same standardization, but using as independent variable time since shock breakout instead of color, reduces the dispersion to 0.24 mag or 11% in distance. Moreover, we demonstrate that the latter method is a generalization of the “Standardized Candle Method.” As a reality check, we apply the method to 18 SNe IIP from in the Hubble flow and obtain a couple of Hubble diagrams. Our estimate of the Hubble Constant ranges from 68 to 71 km/s/Mpc, consistent with the measurement of the HST Key Project. B 1 2 [email protected] Pontificia Universidad Católica de Chile Universidad de Chile 451 Cosmology Posters COS -1: #256 J-PAS: Cosmology with galaxy clusters Clayton Garcia da SilvaB1 ; Laerte Sodré Jr.1 We present estimates on the expected number of clusters of galaxies to be detected by The JavalambrePhysics of the Accelerated Universe Astrophysical Survey (J-PAS), their redshift distribution and their power for cosmological parameter estimation. The J-PAS is a very wide field cosmological survey to be carried out from the Javalambre Observatory in Spain with a purpose-built, dedicated 2.5m telescope, using a set of 54 narrow band and 5 broad band filters. Starting in 2015, J-PAS will image 8500 sq. deg. of Northern Sky and obtain 0.003(1 + z) precision photometric redshifts for 90 million galaxies, about 50 times more than the largest current spectroscopic survey. The main goal of J-PAS is to investigate the origin of the accelerated expansion of the Universe using a variety of probes, clusters of galaxies among them. B 1 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, USP 452 Posters Cosmology COS -1: #257 Contrasting distances using Type Ia supernovae and gamma ray events in the local universe Rafael GirolaB1 In the year 1998, it is discovered –through Type Ia supernova observation– that the universe is expanding at an accelerating rate. One interpretation, which is not contrary to General Relativity, accepts the existence of a cosmological constant other than zero and of Quintessence, a repulsive force. These supernovae are used as standard candles to measure both distances and the accelerating expansion rate of the universe. Although this is based on well-known and proven facts, it was found that the method employed contains systematic errors. The purpose of this study is to present an alternative method to reduce the errors through the measurement of galactic distances, using gamma-ray events from gamma-ray binaries and microquasars. As the actual supernova population is rather small to be statistically reliable, it is supported with numerical simulations to provide a contrast between Type Ia supernovae and gamma-ray events. To this end, we apply the measurement of Type Ia supernovae to nearby galaxies where is possible to measure the accelerating expansion of the universe. Afterwards, assuming that the observations and instrumentations would enable this possibility, we perform the measurements of a group of microquasars, taking on account their approximate equitable distribution of energy which is contrary to the results of supernovae. Our study remains open to further exploration on whether there is a difference between the distances measured or they are compatible and they manage to minimize the systematic error of Type Ia supernova method. In this way, we estimate if the distances are consistent in each case as well as we calculate the measurement of the universe’s expansion. B 1 [email protected] Universidad Nacional de Tres de Febrero 453 Cosmology Posters COS -1: #258 Figure of Merit for Dark Energy Parameterizations González, J. E.B1 ; Barboza Jr., E. M.2 ; Alcaniz, J. S.3 Determining the mechanism behind the current cosmic acceleration constitutes a major question nowadays in theoretical physics. If the dark energy route is taken, this problem may potentially bring to light new insights not only in cosmology but also in high energy physics theories. In this work, we discuss a general uncorrelated form for time-dependent parameterizations of the dark energy equation of state (EoS) by performing a linear mapping of the EoS parameters (w0 , w1 ) into a new set (w0 , wc ). Considering two EoS parameterizations and using current data from type Ia supernovae (Union2.1 compilation), CMB (Planck collaboration) and BAO measurements from SDSS, WiggleZ and 6dFGS surveys, we show that the Figure-ofMerit of the w0 wc plane becomes significantly larger than that of w0 w1 . A general analytical expression to quantify the increase of the FoM by using the Fisher Matrix approach is also derived. B 1 2 3 [email protected] Observatório Nacional Departamento de Fı́sica, Universidade do Estado do Rio Grande do Norte Observatório Nacional 454 Posters Cosmology COS -1: #259 The use of rendering techniques in Galaxy Cluster Finding Hector Javier Ibarra MedelB1 ; Maritza Arlene Lara-López; Omar López Cruz We have developed a new approach to find clusters in optical redshift surveys that combines self-adapting rendering techniques and dynamical estimators. The procedure consists in looking for overdensities within a continuous galaxy number density fields,followed by the performance of a caustic analysis using the Galaxy and Mass Assembly (GAMA) redshift survey. The caustic analysis is performed to minimize the contribution of nearby substructures. This have resulted in a robust way to determine the cluster mass. Using our technique we have detected and measured 93 clusters of galaxies within GAMA. Our clusters have been selected by mass in the range 3x101 3 to 101 5 solar masses. We present an analysis on the on the mass-luminosity relationship at the cluster scale and its implications with their central and satellite galaxies. B 1 [email protected] INAOE 455 Cosmology Posters COS -2: #260 The Galaxy Cosmological Mass Function Lopes, A.B1 ; Iribarrem, A.1 ; Ribeiro, M. B.2 ; Stoeger, W. R.3 This aims to study the galaxy cosmological mass function (GCMF) in a semi-empirical relativistic approach which uses the luminosity function (LF) data derived from galaxy redshift surveys. Starting from a relativistic relation between the mass-to-light ratio, the selection function and luminosity density as presented by Ribeiro & Stoeger (2003), we obtained the average luminosity L at some redshift value using the ratio between the luminosity density and the selection function. We calculated the average galactic mass evolution using the stellar mass-to-light ratio and the previously derived average luminosity. We used the FORS Deep Field galaxy survey sample of 5558 galaxies in the redshift range 0.5 < z < 5.0 and its LF Schechter parameters in the B-band as derived by Gabasch et al. (2004), as well as this sample’s stellar masses. We obtained LB / (1 + z)( 2.40 ± 0.03) and Mg / (1 + z)( 1.1 ± 0.2) for the average galactic mass, whose local value is assumed to be Mg0 ⇡ 1011 M . These results lead to a GCMF that behaves as a Salpeter like power law function as given by ⇣(z) / [Mg (z)] 2.3±0.4 in the studied redshift interval, and implicates that on average more massive galaxies were assemble earlier then less massive ones. This result is, however, preliminary and need to be checked against other datasets. B 1 2 3 [email protected] Observatório do Valongo, Universidade Federal do Rio de Janeiro Instituto de Fı́sica, Universidade Federal do Rio de Janeiro Vatican Observatory Research Group, Steward Observatory, University of Arizona 456 Posters Cosmology COS -2: #261 North-South CMB analyses using the Minkowski Functionals Marques, G. A.B1 ; Ferreira, I. S.2 ; Bernui, A.3 Highly precise cosmic background radiation (CMB) data from Planck satellite confirmed the cosmological model ⇤CDM, that is, a spatially flat universe filled in with dark energy, in the form of a cosmological constant (⇤), and cold dark matter (CDM), in addition to the standard baryonic and electromagnetic ingredients. Moreover, these CMB temperature fluctuations data allow to test the statistical isotropy property, a key feature expected to be shared by these data according to the current cosmological model. To examine the statistical isotropy property we use the Minkowski Functionals to analyze antipodal hemispheres in the CMB foreground-cleaned Planck maps. To estimate the confidence level of our results we compare these outcomes with Planck data with the results achieved in a similar procedure using statistically isotropic Gaussian CMB Monte Carlo maps, that is simulated maps generated using the ⇤CDM angular power spectrum which shares these large-scale features. Our results using the perimeter, one of the four Minkowski Functionals, show that the foreground-cleaned Planck maps, namely Smica, Nilc, and Sevem, do not exhibit substantial differences between North and South galactic hemispheres, in contraposition with what had been seen in the WMAP data. B 1 2 3 [email protected] Observatório Nacional Instituto de Fı́sica, Universidade de Brası́lia Observatório Nacional 457 Cosmology Posters COS -2: #262 The red cluster sequence in low X-ray luminosity galaxy clusters Nilo Castellón, J. L.B1 ; Alonso, M. V.2 ; Garcı́a Lambas, D.2 ; Cuevas,H.1 Using g0, r0 and i0 photometry obtained with GMOS at Gemini North and South telescopes, we study the Red Cluster Sequence (RCS) in seven low x-ray luminosity galaxy clusters in the redshift range of z⇠0.18 to 0.70. We found that at low redshifts (z<0.4), a well defined red cluster sequence, extending by more than 4 magnitudes, dominate the cluster color-magnitude diagrams, while at redshifts higher than 0.40, the clusters studied show a less important RCS, with a smaller extension and a clear presence of the blue population of galaxies. Also is interesting, that in those clusters at z>0.4, we find a flatter slope of the RCS, in comparison with clusters with higher X ray emission, at the same redshift range. These results may suggest that at redshift higher than z>0.4, these low x-ray luminosity clusters are still in formation, while at lower redshifts, these clusters have reached a relaxed stage. B 1 2 [email protected] Physics Departament. University of La Serena, La Serena, Chile Institute for Theoretical and Experimental Astronomy (IATE-CONICET), Córdoba, Argentina 458 Posters Cosmology COS -2: #263 Fractal Characteristics in the Lemaı̂tre-Tolman-Bondi Nogueira, Felipe A. M. G.B1 ; Ribeiro, Marcelo B.2 Recent observations indicate that the Universe may not be homogeneous at high redshifts where density variations of cosmological sources are observed. Assuming that those density variations can be described by inhomogeneous cosmological models, this work intends to model these variations by using the most studied of these models, the Lemaı̂tre-Tolman-Bondi (LTB) spacetime. The generality of this model, which includes the standard cosmology as a particular case, allows its arbitrary functions to be specified in a way that the density variations can be modeled as a fractal distribution. We intend to generalize Ribeiro’s (1992) work by using the technique developed by Mustapha, Ellis & Hellaby (1998) which probes the past light cone using the single null geodesic concept and obtaining analytic solutions of the radial past null geodesic in this cosmology, unlike the numerical approach of Ribeiro (1992). Then we obtain inhomogeneous solutions with a fractal behavior that can be compatible with observations from type Ia supernovae without assuming the existence of a dark energy. This is so because the LTB model can determine various mass and energy distributions due to the arbitrariness of undetermined functions freedom in a spacetime without a cosmological constant. The particular solutions obtained for these functions are used to derive observational quantities in the LTB parabolic model, using the single null geodesic approach, and an analytic expression for the redshift as a function of the comoving radial coordinate is obtained. Finally, a discussion of specific fractal dimension values in each redshift range is presented. B 1 2 [email protected] Observatório do Valongo-UFRJ Instituto de Fı́sica-UFRJ 459 Cosmology Posters COS -2: #264 Observational constraints on a coupled quintessence model with a generalized DE EoS Rafael C. NunesB1 ; Edésio M. Barboza Jr.1 In this work we put constraints on a quintessence dark energy model that interacts with the dark matter fluid. By assuming a DE model described by the parameterization w(a) = w0 + w00 ln (a) and that the dark fluids follows the relation ⇢m /⇢x = a ⇠ we use the most recent data of SN Ia, BAO, CMB and H(z) to put constraints on the EoS parameters w0 and w00 for selected values of and ⇠ parameters. Although the standard ⇤CDM model is in good agreement with our results, we show that scenarios with interaction in the dark sector can not be ruled out by currently available data. B 1 [email protected] Departamento de Fı́sica, Universidade do Estado do Rio Grande do Norte 460 Posters Cosmology COS -2: #265 Gravitational waves and stability of cosmological solutions in the Modified Starobinsky inflation Pelinson, Ana M.B1 ; Fabris, Julio C.2 ; Salles, Filipe de O.3 ; Shapiro, Ilya L.3 The dynamics of metric perturbations is explored in the gravity theory with anomaly-induced quantum corrections. Our first purpose is to derive the equation for gravitational waves in this theory on the general homogeneous and isotropic background, and then verify the stability of such background with respect to metric perturbations. The problem under consideration has several interesting applications. Our first purpose is to explore the stability of the classical cosmological solutions in the theory with quantum effects taken into account. There is an interesting literature about stability of Minkowski and de Sitter spaces and here we extend the consideration also to the radiation and matter dominated cosmologies. Furthermore, we analyze the behavior of metric perturbations during inflationary period, in the stable phase of the Modified Starobinsky inflation. B 1 2 3 [email protected] Departamento de Fı́sica, CFM/Universidade Federal de Santa Catarina, Brazil Departamento de Fı́sica, CCE/ Universidade Federal de Vitória Departamento de Fı́sica, ICE/Universidade Federal de Juiz de Fora, Brazil 461 Cosmology Posters COS -2: #266 Measuring galaxy morphologies in the CFHT/MegaCam Stripe-82 Survey Pereira, M. E. S.B1 ; Moraes, B.2 ; Charbonnier, A.3 ; Pereira, R.4 ; Makler, M.5 ; Kneib, J.-P.6 ; Leauthaud, A.7 ; Van Waerbeke, L.8 ; Bundy, K.9 ; Erben, T.10 ; Heymans, C.11 ; Hildebrandt, H.12 ; Miller, L.13 ; Woods, D.14 ; Santiago, B. X.15 We present the determination of galaxy structural parameters in the CFHT/MegaCam Stripe-82 Survey (CS82) stacked images. The CS82 survey covered an area of ⇠ 170 square degrees with the CFHT 3.6m telescope in a field determined by 40 < RA < 45 and 1 < DEC < 1 (within the SDSS stripe-82 region) in i-band to a depth of magAB ⇠ 24. Its excellent image quality (mean seeing of ⇠ 0.6) and uniformity makes CS82 specially suitable for applications involving gravitational lensing and galaxy morphology. In this work we present the determination of galaxy structural parameters which has applications to galaxy evolution studies, weak lensing through the effect of magnification, and the improvement of the photometry in other surveys (e.g. SDSS), through the “forced photometry” method. In this work the morphological analysis of galaxies is performed through a profile fitting method implemented with SExtractor+PSFEx. First, we use SExtractor to perform object detection and obtain basic measurements of objects, then we use PSFEx to model the PSF across the field, and finally, we run SExtractor again to perfom the model-fitting of objects. In this work we use 4 models implemented in SExtractor: Sércic, de Vaucouleurs, exponential and 2-component de Vaucouleurs+exponential. We discuss some applications of these results, such as the evolution of galaxy sizes and the measurement of the lensing magnification signal combining precise photometry, counts and sizes. B [email protected] Centro Brasileiro de Pesquisas Fı́sicas 2 Centro Brasileiro de Pesquisas Fı́sicas 3 Centro Brasileiro de Pesquisas Fı́sicas 4 Centro Brasileiro de Pesquisas Fı́sicas 5 Centro Brasileiro de Pesquisas Fı́sicas 6 Ecole Polytechnique Federale de Lausanne 7 Kavli Institute for the Physics and Mathematics of the Universe 8 University of British Columbia 9 Kavli Institute for the Physics and Mathematics of the Universe 10 University of Bonn 11 University of Edinburgh 12 University of Bonn 13 Oxford University 14 University of British Columbia 15 Universidade Federal do Rio Grande do Sul 1 462 Posters Cosmology COS -2: #267 Gravitational Waves formulation for the Brane Universe and Possible Induced Corrections on an Observational Level C. D. Rodrı́guez-CamargoB1 ; E. A. Larrañaga-Rubio2 The observation of gravitational waves and their effect on different physical systems constitute one of most searched for proofs of the theory of general relativity. In this work, a brief summation on their construction based on general relativity and its observational consequences is presented with the intention of later extending the analysis to obtain the wave equation from the field equations that describe the brane universe. With the obtained results, a discussion is opened around the possibility of distinguishing observationally between general relativity and the brane universe theory. Since brane theory considers that gravity can spread to the extra dimensions (thus appearing weaker than the rest of interactions), it is possible to argue that the expected amplitude of gravitational waves according to the theory differs from the one expected in relativity. In the same way, it is to expect that the effect of energy dissipation that involves gravitational waves emission, as occurs in binary systems, needs to be corrected. B 1 2 [email protected] Physics Deparment, National University of Colombia (UNAL) National Astronomical Observatory (OAN) 463 Cosmology Posters COS -2: #268 2-Pt. Correlation Function for Luminous Red Galaxies Secco, L. F.B1 ; Abramo, L. R. W.1 We have estimated the 2-pt. correlation function for luminous red galaxies from the catalog used by Eisenstein et al (2005), using the method from Landy-Szalay. Although no BAO scale was found, comparing the correlation function estimated with an output from CAMB yields a value of around 2 for the LRG bias. B 1 [email protected] Department of Mathematical Physics, University of São Paulo 464 Posters Cosmology COS -3: #269 Anisotropic Halo Model B1 Sgró, M. A. ; Paz, D. J.1 ; Merchán, M. E.1 ; Rodriguez, F.1 In this work, we present an extended version of the classic halo model for the large-scale matter distribution which includes a triaxial model for the halo density profiles and their alignments. In particular, we derive general expressions for the halo–matter cross-correlation function. Using a Monte Carlo integration method we obtain instances of the cross-correlation function depending on the directions given by halo shape axes. These functions are called anisotropic cross-correlations. With the aim of comparing our theoretical results with the simulations, we compute averaged anisotropic correlations in cones with their symmetry axis along each shape direction of the centre halo. From these comparisons we characterize and quantify the alignment of dark matter haloes on the cold dark matter context by means of the presented anisotropic halo model. B 1 [email protected] Instituto de Astronomı́a Teórica y Experimental (UNC-CONICET), Observatorio Astronómico de Córdoba 465 Cosmology Posters COS -3: #270 The Type Ia Supernova Pipeline for the Javalambre Physics of the Accelerating Universe Astrophysical Survey (J-PAS) Siffert, B. B.B1 ; Reis, R. R. R.1 ; Calvão, M. O.1 The Javalambre Physics of the Accelerating Universe Astrophysical Survey (J-PAS) is an astronomical facility being built in Sierra de Javalambre, Spain. The main goal is to study the expansion of the Universe through different cosmological observables such as baryonic acoustic oscillations, type Ia supernovae and galaxy clusters. The main instrument will be a 2.5 m telescope equipped with a system of 56 narrow band filters in the optical. Here we present a sketch of the pipeline we are developing to detect type Ia supernovae with J-PAS. First we describe each individual step of the pipeline, such as image subtraction and source selection. Then we show some results we obtained when applying our pipeline to images from the Sloan Digital Sky Survey and the Alhambra survey, which had a set of narrow band filters similar to the ones that will be used by J-PAS. B 1 [email protected] Instituto de Fı́sica, Universidade Federal do Rio de Janeiro 466 Posters Cosmology COS -3: #271 Identification and extraction of photometric redshifts of quasars with narrow-band filters Silva, C. Q. A.B1 ; Abramo, L. Raul2 Although quasars are valuable targets for many cosmological applications, imaging surveys employing optical broad-band (ugriz) filter systems are unable to obtain accurate photometric redshifts for these objects. Broad-band imaging surveys also have some difficulty in distinguishing quasars from stars and HII regions of galaxies. However, the construction of a high-purity catalog of quasars, with accurate photometric redshifts, can be much more efficient with medium or narrow-band surveys, such as HETDEX, ALHAMBRA and the upcoming J-PAS. In this work we discuss how to overcome the degeneracies in the color-color and colormagnitude diagrams that hamper the efficient detection of quasars, and how to obtain very good (and, in some cases, near-spectroscopic) photometric redshifts for these objects. In particular, we discuss how to include quasars in some of the most popular photometric redshift codes, and the parallel need for the inclusion of spectral libraries for stars. We also discuss the importance of a good modeling of the distribution of point sources in the sky, and the need for reliable luminosity functions that can inform the Bayesian estimation of types and photometric redshifts. B 1 2 [email protected] Instituto de Fı́sica, USP Instituto de Fı́sica, USP 467 Cosmology Posters COS -3: #272 The red sequence of Abell X-ray underluminous clusters Trejo-Alonso, J. J.B1 ; Caretta, C. A.1 ; Laganá, T. F.2 ; Sodré Jr., L.2 ; Cypriano, E. S.2 ; Lima Neto, G. B.2 ; Mendes de Oliveira, C.2 We present an analysis of a sample of 51 X-ray underluminous Abell clusters based on their colour-magnitude relation, aiming at unveiling properties that may elucidate the evolutionary stages of the galaxy populations which compose such systems. For doing that, we compared the parameters of their colour-magnitude relations with the ones found for another sample of 67 “normal” X-ray emitting Abell clusters, both selected in an objective way. The g and r magnitudes from the SDSS-DR7 were used for constructing the colourmagnitude relations. We found that both samples show the same trend: the red sequence slopes change with redshift, but the slopes for underluminous clusters are always flatter than those for the normal clusters, by a difference of about 46% along the surveyed redshift range of 0.05  z < 0.20. Also, the intrinsic scatter of the colour-magnitude relation as found to grow with redshift for both samples, but for the underluminous clusters, this is systematically larger by about 11%. By combining several results from independent tests we get a 99% probability that the slopes and intercepts of the red sequences are different for underluminous and normal colour-magnitude relations and ⇠ 60% for the scatter. B 1 2 [email protected] Departamento de Astronomı́a, Universidad de Guanajuato Instituto de Astronomia, Geofı́sica e Ciencias Atmosfericas, Universidade de Sao Paulo. 468 Posters Cosmology COS -3: #273 Super-massive black hole growth in the first gigayear of cosmic history Forero, J.1 ; Gómez, M. F.2 ; Velasco, S.B3 As two galaxies collide the super-massive black holes in their centers will merge. The resulting black hole will be ejected with a certain kick velocity. The black hole will move in the galaxy’s potential well while it oscillates and returns to its initial position due to dynamic friction processes. In this work we use semianalytic techniques to follow the amount of mass accreted by the BH since the initial kick until its return to a stationary position at the center of the host galaxy. We focus our study on black holes in the mass range 106 109 Msun. We use these results to re-interpret the observational constraints on the growth of supermassive black holes during the first gigayear of cosmic history. B 1 2 3 [email protected] Universidad de los Andes Universidad de los Andes Universidad de los Andes 469 Cosmology Posters COS -3: #274 Properties of type Ia supernovae inside rich galaxy clusters Henrique S. XavierB1 ; Ravi R. Gupta2 ; Masao Sako2 ; Chris B. D’Andrea3 ; Joshua A. Frieman4,5,6 ; Lluis Galbany7,8 ; Peter M. Garnavich9 ; John Marriner6 ; Robert C. Nichol3 ; Matthew D. Olmstead10 ; Donald P. Schneider11,12 ; Mathew Smith13 We used the GMBCG galaxy cluster catalogue and SDSS–II supernovae data with redshifts measured by the BOSS project to identify 48 SNe Ia residing in rich galaxy clusters and compare its properties with 1015 SNe Ia in the field. Their light curves were parametrised by the SALT2 model and the significance of the observed differences was assessed by a resampling technique. To test our samples and methods, we first looked for known differences between SNe Ia residing in active and passive galaxies. We confirm that passive galaxies host SNe Ia: with smaller stretch; weaker colour–luminosity relation [ of 2.54(22) against 3.35(14)]; and that are ⇠ 0.1 mag more luminous after stretch and colour corrections. We show that only 0.02 per cent of random samples drawn from our set of SNe Ia in active galaxies can reach these values. Reported differences in the Hubble residuals scatter could not be detected, possibly due to the exclusion of outliers. We then show that, while most field and cluster SNe Ia properties are compatible at the current level, their stretch distributions are different (⇠ 3 ): besides having a higher concentration of passive galaxies than the field, the cluster’s passive galaxies host SNe Ia with an average stretch even smaller than those in field passive galaxies (at 95 per cent confidence). We argue that the older age of passive galaxies in clusters is responsible for this effect since, as we show, old passive galaxies host SNe Ia with smaller stretch than young passive galaxies (⇠ 4 ). B [email protected] Instituto de Fisica, Universidade de Sao Paulo 2 Department of Physics & Astronomy, University of Pennsylvania 3 Institute of Cosmology and Gravitation, University of Portsmouth 4 Department of Astronomy and Astrophysics, University of Chicago 5 Kavli Institute for Cosmological Physics, University of Chicago 6 Center for Particle Astrophysics, Fermi National Accelerator Laboratory 7 Institut de Fisica dAltes Energies, Universitat Autonoma de Barcelona 8 Centro Multidisciplinar de Astrofisica, Instituto Superior Tecnico 9 Department of Physics, University of Notre Dame 10 Department of Physics and Astronomy, University of Utah 11 Department of Astronomy and Astrophysics, The Pennsylvania State University 12 Institute for Gravitation and the Cosmos, The Pennsylvania State University 13 Department of Physics, University of the Western Cape 1 470 Posters Cosmology COS -3: #275 The MW and the Local Group mass Gonzalez, RobertoB1,2 ; Kravtsov, Andrey2 ; Gnedin, Nickolay2,3 We use the dynamical properties of the Magellanic Clouds to compute the DM halo mass likelihood of the MW by looking MW-sized halos in the Bolshoi simulation having similar satellite configuration. We also explore the accretion scenario of the MCs. In a similar way, we use recent proper motion measurements of M31 to derive the likelihood of halo mass of the MW-M31 pair using its analogues in the Bolshoi cosmological simulation with known masses. The analogues are identified by pair isolation, separation, relative velocity, maximum distance to a Virgo-like cluster, and the local density which can be associated to the coldness of the local Hubble flow. B 1 2 3 [email protected] Pontificia Universidad Catolica de Chile Department of Astronomy & Astrophysics, University of Chicago, USA Fermi National Acelerator Laboratory, USA 471 Cosmology Posters COS -3: #276 Constraints on the First Ionizing Sources Maldonado, V.B1 ; Dominguez, M.1,2 ; Valotto, C.1,2 The Epoch of Reionization (EoR) is one of the most interesting topics in modern cosmology since it identifies the time that astrophysical sources began to generate photons and became a major influence in the Intergalactic Medium (IGM) and the subsequent formation of structures. A large amount of theoretical and computational effort, guided by very limited observational evidence, is dedicated to understand the physical processes that trigger this epoch and govern its evolution. This is shown in the simulations and semi-analytic models that predict the 21 cm signal at high redshift like the code 21cmFAST (Mesinger et al. 2011). The first observations of the Precision Array for Probing the EoR (PAPER) shows the 21 cm power spectrum at z = 7.7 (Parson et al. 2013) and we have a constraint on the evolution of the ionized fraction during EoR product of observations CMB with South Pole Telescope (SPT) and WMAP (Zahn et al. 2012). Using 21cmFAST, aiming to infer properties of the first ionizing sources, we explore the parameter space (⇣, Mmin ), where ⇣ is the ionization efficiency parameter and Mmin is the minimum mass that can form the first stars. Finally, in this work we show the best fit model to the results of (Parson et al. 2013) and (Zahn et al. 2012). B 1 2 [email protected] Instituto de Astronomı́a Teórica y Experimental (IATE), Consejo de Investigaciones Cientı́ficas y Técnicas (CONICET) Observatorio Astronómico, Universidad Nacional de Córdoba 472 High Energy Astrophysics HEAP-1: #278 Decay of the magnetic field in ”black widow” pulsars Castilho, C. M.B1 ; Benvenuto, O. G.2 ; De Vito, M. A.2 ; Horvath, J. E.1 A small fraction of the binary relativistic systems display the “black widow” effect: the companion is being ablated by the (recycled) pulsar wind. In these binary systems the evolution of the companion star (of the solar-type) reaches the point of filling its Roche lobe, thus initiating the process of mass accretion onto the pulsar. Accretion is generally believed to result in magnetic field decay, while isolated neutron star fields decay very slowly, if at all. We shall show that the very long evolution of the “black widow” system, starting from a solar-type star and lasting > 5 Gyr to reach the observed position in the Porb -Mdonor plane, allows us to conclude that the magnetic field does not decay below the “bottom” value ⇠ 2 ⇥ 108 G, extending the previous conclusions drawn from younger systems. In addition, the masses of the “black widow” pulsars are naturally predicted to be > 2 Mo due to the accretion history, in full agreement with recent measurements. B 1 2 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo Faculdad de Ciencias Astronómicas y Geofı́sicas, Universidad Nacional de La Plata 473 High Energy Astrophysics Posters HEAP-1: #279 Radiation-hydrodynamic Model of High-Mass X-ray Binaries Čechura, J.B1,2 ; Hadrava, P.1 The topic of circumstellar matter in the X-ray binaries and its spectroscopic diagnostics is addressed by method of generating synthetic Dopplerograms for direct comparison with observations. We present the latest results of our improved three-dimensional radiation-hydrodynamic model of the environment close to interacting binaries. We use the model to simulate dynamics, anisotropy and other significant characteristics, e.g. the density distribution and ionization structure, of a stellar wind coming from a donor in highmass X-ray binaries (HMXBs). We introduce a data interpretation method of observed Doppler tomograms through direct comparison with synthetic Dopplerograms obtained from our model. Typically, the donor is a highly-luminous massive OB supergiant with an intense stellar wind. The mechanism that is predominantly responsible for launching gas from the stellar atmosphere and, subsequently, pushing it outwards, is based on a modified version of the line-driven wind theory of Castor, Abbott, and Klein where the wind material is accelerated by the line absorption of the star’s radiation field. The HMXB Cygnus X-1 serves as an example of such a system and its parameters were adopted in our simulations. The results of the numerical model which settings correspond to the parameters of Cygnus X-1 are presented and discussed with regard to phase-resolved optical spectroscopic data. We use the indirect imaging method of Doppler tomography to probe the structure of radiation emitting material in the system, in order to test the reliability of the numerical model as well as to set constrains on various physical parameters and processes, e.g. the accretion rate. We take into account the Coriolis force, the ionization structure of the circumstellar medium, the gravity darkening and we investigate the effect these phenomena might have on the accretion process in such systems. E.g. the Coriolis force substantially influences the mass-loss of the donor and by doing so also the accretion rate of the compact companion. Additionally, the focusing of the stellar wind by the gravitational field of the compact companion leads to the formation of an unstable gaseous tail behind the companion. This tail shows signs of quasi-periodic oscillations and their mere existence can present us with other means to explain the switching mechanisms among the different X-ray states. B 1 2 [email protected] Astronomical Institute, Academy of Sciences, Bočnı́ II 1401, 14131, Praha 4, Czech Republic Faculty of Mathematics and Physics, Charles University, Prague, Czech Republic 474 Posters High Energy Astrophysics HEAP-1: #280 Large-Scale Anisotropies of the Cosmic Rays Detected at the Pierre Auger Observatory and the Telescope Array Fernandes M. C.B1 ; Almeida R. M.3 ; Vasquez, R.2 ; Giaccari, U.2 ; de Mello Neto, J. R. T2 The study of large-scale distribution of arrival directions of cosmic rays is an important observable in attempts to understand their origin. In particular, there is a huge experimental effort led by the Pierre Auger Observatory in the southern hemisphere and the Telescope Array in northern hemisphere. The anisotropy of any angular distribution on the sphere is encoded in their respective set of spherical harmonics moments alm . However, since each observatory has access only to a partial sky coverage, it is necessary to make some assumptions so that we can make a joint analysis of both. In this work, through an iterative method we calculate the alm coefficients, and through them we reconstruct some parameters of interest, such as the declination angle, the angular power spectrum Cl and the amplitude of the dipole. The last two have a special important because they allow us to analyze the efficiency in detecting a dipole anisotropy pattern using this method. B 1 2 3 [email protected] Observatório do Valongo - Universidade Federal do Rio de Janeiro Instituto de Fı́sica - Universidade Federal do Rio de Janeiro Instituto de Fı́sica - Universidade Federal Fluminense 475 High Energy Astrophysics Posters HEAP-1: #281 Magnetic field evolution and jet formation in accreting neutron stars Federico Garcı́aB1 ; Deborah N. Aguilera2 ; Gustavo E. Romero1 In the magneto-centrifugal model neutron stars can form jets only if their superficial magnetic field is weak enough (B ⇠ 108 G) to allow the collimation of the accreted material by the magnetic tower. However, 12 these stars are compact objects born with strong initial magnetic fields (B > ⇠ 10 G). In this work we study necessary conditions in a binary system formed by a neutron star and a high-mass donor, to be able to emit jets after an induced magnetic field decay of the neutron star due to the accretion of the wind from the stellar companion. We solve the induction equation of the magnetohydrodynamics for the diffusion and advection of a dipolar magnetic field in a realistic crust, incorporating the state-of-the-art in the microphysics. Finally, we show that results obtained can be used to explain a connection between Supergiant Fast X-ray Transients (SFXTs) and a group of unidentified MeV/TeV transient sources. B 1 2 [email protected] Instituto Argentino de Astronomı́a (IAR-CONICET) Laboratorio Tandar (CNEA-CONICET) 476 Posters High Energy Astrophysics HEAP-1: #282 The galactic distribution of Fermi point sources Jablonski, F.B1 ; Polido, P.1 The second catalog of high-energy -ray sources detected by the Large Area Telescope (LAT), the primary science instrument on the Fermi Gamma-ray Space Telescope, allows us for the first time to perform a modeling of the galactic distribution of such sources based on the method of summing all counts in a given line of sight. The challenge is to produce reliable estimates of counts from small numbers. The catalog contains 1873 sources over the whole sky, giving an average of 0.036 counts/deg2 for |b| > 60 . In a narrow strip centered at |b| < 0.5 we find 128 sources. In this work, we describe our attempts to estimate the density of -ray sources along both galactic longitude and galactic latitude. The results of the estimated source counts are compared to the predictions of a model that has an exponential distribution in the radial direction as well as an exponential distribution above the galactic plane. Our conclusions point to a radial length scale consistent with that obtained from near-infrared counts and a very short height scale, typical of very young populations in the Galaxy. We tested both Gaussian and Power-Law forms for the luminosity function. The luminosities cover the range 1033 neighborhood) of ⇠ 10 B 1 8 1036 erg/s in the 100 MeV–100 GeV band with space densities (in the solar /pc3 . [email protected] Instituto Nacional de Pesquisas Espaciais 477 High Energy Astrophysics Posters HEAP-1: #283 The role of fast magnetic reconnection in acceleration zones of microquasars and AGNs Kadowaki, L. H. S.B1 ; de Gouveia Dal Pino, E. M.1 Fast magnetic reconnection events, like those associated to solar flares, can be a very powerful mechanism operating at the jet launching region in the core of microquasars and AGNs. We have recently found that the magnetic power released by reconnection between the magnetic field lines of the coronal inner disk region and the lines anchored into the black hole is able to accelerate relativistic particles through a first-order Fermi process and produce the observed radio luminosity from both microquasars and low luminous AGNs. We also found that the observed correlation between the radio luminosity and the mass of these sources, spanning 109 orders of magnitude in mass, is naturally explained by this process. Furthermore, recent observations of gamma-ray emission with strong variability from AGNs and galactic compact sources indicate extremely small emission regions. In this work, assuming that this high energy emission is probably originated in the same acceleration zones that produce the radio emission, we have applied the scenario above to investigate the origin of the high energy outcomes from an extensive number of sources including high and low luminous AGNs, microquasars and GRBs. We find correlation of our model with the gamma-ray emission only for microquasars and a few low luminous AGNs, while none of the high luminous AGNs or GRBs are fitted, neither in radio nor in gamma emission. We attribute the lack of correlation of the gamma emission for most of the low luminous AGNs to the fact that this processed emission does not depend only on the local magnetic field activity around the source accretion disk (as the radio Synchrotron emission), but also on other environmental factors like the photon and density fields. We also find that the emission from both the high luminous AGNs and the GRBs actually anti-correlates with our model indicating that their emission is processed further out in the jet. We conclude from these results that the emission we see from the low luminous AGNs and microquasars comes from the nuclear region of their sources and therefore, can be driven by nuclear magnetic activity connected to the source/accretion disk corona, as in our model. However, in the case of the high luminous AGNs and GRBs, the nuclear emission is blocked by the surrounding density and photon fields and therefore, we can only see the jet emission further out (which has already lost correlation with the nuclear conditions). B 1 [email protected] IAG, Universidade de São Paulo 478 Posters High Energy Astrophysics HEAP-1: #284 A magnetic reconnection model for explaining AGNs and microquasars radiation Khiali, B.B1 ; de Gouveia Dal Pino, E. M.1 ; Del Valle, M. V.2 ; Kowal, G.1 ; Sol, H.3 Very high energy observations of AGNs are challenging current theories of particle acceleration (mostly based on shock acceleration) which have to explain how particles are accelerated to energies above TeV in very compact regions compared to the characteristic scales of their sources. The identification of microquasars and AGNs as sites of particle acceleration raises many fascinating and important questions. Recent magneto-hydrodynamical studies have revealed that cosmic ray acceleration by fast magnetic reconnection can be rather efficient because a first-order Fermi process may occur. In this work, we discuss this acceleration mechanism in the coronal region of the accretion disk around microquasars and AGNs. In addition, the accelerated particles lose substantial amounts of their energy due to non-thermal interactions with the surrounding magnetic field, matter and radiation fields. We will compute the corresponding acceleration rate and the relevant loss rates in order to reproduce the observed spectral energy distribution for a number of AGNs and microquasars (e.g., M87, Cyg-X1, Cyg-X3, etc), considering the model above and leptonic and hadronic processes. B 1 2 3 [email protected] IAG/USP, University of Sao Paulo IAR, CONICET, Argentina Observatoire de Meudon, France 479 High Energy Astrophysics Posters HEAP-2: #285 Classification of long gamma-ray burst using ACF and spectral lag with cosmological corrections Andrès Baquero LarrivaB1 ; Nicolas Vàsquez Pazmiño; David Andrade Gamma-ray bursts (GRBs) are well established as cosmological sources. They have distinct light curves that display a complex temporal structure. The light curve variability time scale parameter is commonly attributed to have a physical origin e.g., central engine activity, circumburst medium, or relativistic turbulence. The Autocorrelation function (ACF) and Cross correlation function (CCF) are versatile tools to quantify thisparameter and contain interesting characteristics. We can determine the spectral lag, an intrinsic property of GRBs, using the CCF in two different energy bands and the ACF of a selected sample of bursts from Swift space telescope with known redshifts. Using these such as temporal estimators with cosmological corrections, we propose the existence of a bimodal distribution that provides evidence of two clases of long GRBs. B 1 [email protected] Escuela Politècnica Nacional del Ecuador 480 Posters High Energy Astrophysics HEAP-2: #286 Highlights on Cas-like stars Ribeiro, E. M.B1 ; Lopes de Oliveira, R.2 ; Dupke, R. A.1 The number of Be stars with unusually hard-thermal and variable X-ray emission like that of -Cassiopeia increased from one to ten in seven years. It is possible that they could be progenitors of magnetars and account for the missing number of Be/WD binaries observed, and this can be further tested through careful characterization of the parameter space in which the X-ray emission occurs. Here, we present a compendium of the optical and X-ray properties of a sample of this new class of X-ray emitters and some very recent results presented by our group. We discuss the current understanding emphasize results that strengthen the interpretation of magnetic activity near the Be star as being the source of the X-ray emission. B 1 2 [email protected] Observatório Nacional Universidade Federal do Sergipe 481 High Energy Astrophysics Posters HEAP-2: #287 Relativistic MHD Simulations of Magnetized Jets Rocha da Silva, G.B1 ; de Gouveia Dal Pino, E. M.1 ; Falceta-Gonçalves, D.2 ; Kowal, G.2 Gamma-Ray Bursts (GRBs) and Active Galactic Nuclei (AGNs) can be modeled from the perspective of relativistic jets. Despite the observational efforts, the composition of these jets is still unknown and also there are evidences suggesting that the jets are strongly magnetized. The difference between jet models can be characterized by the parameter that is the ratio between the Poynting flux and the matter flux. One of the major problems concerning strongly magnetized jets is how to transform the magnetic energy into kinetic energy. In this work we present relativistic MHD (RMHD) numerical simulations in order to study the evolution and dynamic behavior of relativistic jets in the limit where they are strongly magnetized ( >= 1). We discuss our results showing the main differences between the distinct regimes. We compare our results for strongly magnetized jets with previous analytical predictions and discuss the perspective of their applications, both to AGNs and GRBs, aiming in particular, to explain their prompt gamma emission. B 1 2 [email protected] Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, Universidade de São Paulo Escola de Artes Ciências e Humanidades, Universidade de São Paulo 482 Posters High Energy Astrophysics HEAP-2: #288 Searching for near-infrared counterparts of high energy sources: Variability studies from VVV Survey Rojas, A. F.B1 ; Masetti, N.2 ; Minniti, D.3 To investigate the nature of galactic and extragalactic sources that has been detected with INTEGRAL and Swift satellites, we analized the epochs in J-H-Ks-bands of VVV, a public infrared Survey of ESO. The physics of different processes in this sources its reflected as emision at different wavelenght and the activity of high energy sources can be used for the identification comparing with others stars of field. Depending on if the source is in hard or quiescente state, can be used for study of variability and colors of sources comparing the differents epochs in Ks-band of VVV Survey and the infrared colors permited us know the temperature or nature. We analysed sources detected by INTEGRAL and Swift in the VVV fields. The variability studies we permited us found sources probably like HMXB, AGN, Transients and LMXB. B 1 2 3 [email protected] Pontificia Universidad Católica de Chile INAF - Instituto di Astrofisica Spaziale e Fisica Cosmica di Bologna Pontificia Universidad Católica de Chile 483 High Energy Astrophysics Posters HEAP-2: #289 Properties of Galaxies Groups Selected from Chandra X-ray Observations of the Bootes Fields Vajgel, B.B1,2 ; Lopes, P. A. A.1 ; Jones, C.2 ; Forman, W. R.2 ; Murray S. S.2 Galaxy groups have lower masses, lower velocity dispersions, lower luminosities, and smaller extents than galaxy clusters. However, galaxy groups are not simply scaled down versions of rich clusters (e.g. Mulchaey 2000, Ponman 2003, Voit 2005). Due to a group’s shallow gravitational potential, feedback processes (e.g. galactic winds and AGN feedback) play an important role in the group’s evolution. It is important to understand galaxy groups since, in hierarchical clustering, they are the building blocks of large scale structure. Thus, in addition to determining the characteristics of groups, it is important to determine the mass function over the range that includes poor clusters and groups. We will present the properties of the galaxy groups selected in the Chandra X-Boötes survey (Kenter et al. 2005). We used follow-up Chandra observations to better define the group sample and their X-ray properties. Group redshifts were measured from the AGES (Kochanek et al. 2012) spectroscopic data. We used photometric data from the NOAO Deep Wide Field Survey (NDWFS) (Jannuzi & Dey 1999) to estimate the group richness (Ngals ) and the optical luminosity (Lopt ). Our final sample comprises 32 systems at z < 0.60, with 14 below z = 0.35. For these systems we estimate velocity dispersions ( ) and perform a virial analysis to obtain the radius (R200 and R500 ) and mass (M200 and M500 ) for groups with at least five galaxy members. We use the Chandra X-ray observations to derive the X-ray luminosity (LX ). We examine the performance of the group properties , Lopt and LX , as proxies for the group mass. Understanding how these observables measure the total mass is important to estimating how well the cluster/group mass function is determined. By extending the mass function to the group regime, we can predict the number of groups that new X-ray surveys, particularly eROSITA, will detect. B 1 2 [email protected] Observatorio do Valongo, Universidade Federal do Rio de Janeiro Harvard-Smithsonian Center for Astrophysics 484 Posters High Energy Astrophysics HEAP-2: #290 Simulation of Water Cerenkov Detector for detection of cosmic rays Using GEANT4 for the LAGO Project H. Asorey; R. CalderónB1 ; L. A. Núñez; C. Sarmiento; M. Suárez-Durán We present results of computer simulations of the Water Cherenkov detector (WCD) of the LAGO Project (Large Aperture GRB Observatory). This project aims to study the high energy component of GRBs by using Water Cherenkov detector at high altitude sites. This project is operated by an international collaboration constituted by 28 different groups of eight Latin American countries. These simulations have been done using the Geant4 computational tool. We focus this study on the internal surfaces of the detectors, with special emphasis on the reflectivity and diffusivity of the internal coating of the WCD. In this work we correlate the simulated data for different simulated surfaces with data obtained experimentally. After that, we carried out a characterization of the detector response as a function of internal diffusers from the simulations obtained. Finally these results will be used to study the effectiveness of internal diffusers to improve the detection of Cherenkov photons in the PMT(Photomultiplier tube). B 1 [email protected] Escuela de Fisica, Universidad Industrial de Santander 485 High Energy Astrophysics Posters HEAP-2: #291 Analysis and validation of data in the search for GRB Asorey, H.; Calderón, R.; Núñez, L. A.; Sarmiento, C.B1 ; Suárez-Durán M.; LAGO Collaboration The LAGO project, Large Aperture Gamma Ray Burst Observatory, is a collaboration among research groups from Argentina, Bolivia, Colombia, Ecuador, Guatemala, Mexico, Peru and Venezuela. LAGO aims to detect high energy component of Gamma Ray Burst (GRBs), by a Water Cherenkov Detectors (WCDs) network at high altitude sites Our group, LAGO-Colombia, is developing a network data repositories, LAGOData, where the data collected at different sites is catalogued in three types: detected, simulated and processed. We evaluated the temporal continuity of the data collected at Chacaltaya (Bolivia), and Sierra Negra (Mexico), comparing one by one with a mock file generate synthetically from 2005 to 2012. After this evaluation, we found that about 60% of the collected data pass the quality requirements,focusing our criteria on the temporal continuity of data and the correctness of GPS label. Data is then analyzed searching for deviations from the average count rate by using a timing windows average method. Despite that presently we don’t found any significant excess, he data has been depurate in order to look for other physical phenomena such as periodical signals of astrophysics objects. B 1 [email protected] Escuela de Fı́sica, Universidad Industrial de Santander, Bucaramanga, Colombia 486 Instrumentation INST-1: #292 Simulations of atmospheric turbulence with spatiall phase modulators Bernardi, R.B1 ; Kanaan, A.1 ; Mello, A. T.1 ; Guzmán, D.2 Atmospheric turbulence in the optical path of incoming stellar light transforms a plane wavefront into a distorted wavefront. This leads to loss of resolution achievable in a telescope. The correction of these distortions is the goal of adaptive optics. We are designing an experiment to recreate the effects of turbulence on an optical bench. This experiment aims to reproduce the effects observed in an artificial sodium laser star when viewed by a 30m class telescope. The edge of such large telescopes see the sodium artificial star as an elongated rather than a circle. In the bench experiment the turbulence distortions are achieved by directing the light beam through a glass plate whose surface is etched to imitate the phase distortions caused by the atmosphere, this plate is called a phase screen. Phase screens are made much bigger than the incident beam of light and we move this phase plate to simulate the effect of a changing atmosphere. To test new turbulence patterns one needs several different phase screens, which are expensive and hard to make. Our work involves computing numerical simulations of turbulence and testing algorithms to correct the phase distortion (see Mello, A. T. “New algorithm for centroiding in elongated Shack-Hartmann wavefront sensors spots using artificial neural networks” in this conference). We would then like to test these algorithms on our bench before testing on the telescope. To make these tests more realistic we would like to apply the same simulated turbulence patterns to our phase screen. This is almost impossible to do with phase screens, therefore we are planning to replace phase screens with spatial phase modulators, which are solid state devices with typically 800x600 20 µm pixels that can be programmed to introduce a phase shift to the incident light at a time resolution of milliseconds. Integration of spatial phase modulators in optical benches as phase screens will allow for much more flexible experiments permitting a perfect correlation between the numerical simulations and the physical experiments. B 1 2 [email protected] Departamento de Fı́sica, Universidade Federal de Santa Catarina, Brasil Departamento de Ingenierı́a Eléctrica, Pontifı́cia Universidad Católica, Chile 487 Instrumentation Posters INST-1: #293 Star detection and study of atmospheric extinction with an All Sky camera Bortolotto, G. S.B1 ; Kanaan, A.1 All sky cameras are a great alternative to the study of atmospheric conditions in an astronomical site. We show how to compute the instantaneous coefficients of atmospheric extinction for various moments in the same night. The images used were obtained by the camera SASCA (SOAR AllSky Camera) located at Cerro Pachon. To estimate the extinction coefficients we developed a method to measure the brightness of several stars at different air masses for the same instant. We developed a Python program that calculates azimuth and altitude for the stars and then converts them to pixel coordinates on the CCD. Comparing the positions calculated for a group of stars with their actual positions on the images, we can determine the distortion caused by the camera. After finding out the distortions we know exactly in which pixel a star falls on any date and time. At this point we created tables of star positions and did the photometry of them all on each image using the IRAF routine PHOT. These photometry tables are subsequently converted into multiple tables with apparent magnitude versus air mass for each star at a given instant. Our results show that the extinction coefficient calculated for different atmospheric moments is within two sigma of the values of the coefficients obtained through the monitoring of a single star at different air masses, demonstrating the feasibility of our approach. B 1 [email protected] Universidade Federal de Santa Catarina 488 Posters Instrumentation INST-1: #294 Developments with the hard X-Ray detection plane of the protoMIRAX imaging telescope Flavio D’AmicoB1 ; Fernando Gonzalez Blanco; Sérgio Amirábile; João Braga; Bárbara H. G. Rodrigues; Manuel Ávila; Taı́s Maiolino; César Strauss; Luiz Reitano In pursuing the study of the high energy Universe, our group is developing a coded-mask balloon-borne hard X-ray imager, the protoMIRAX experiment (pMRX for short). In achieving imaging at this domain of the electromagnetic spectrum, atomic/nuclear radiation detectors must be used. As a result of the combination of the pixel size in the detection plane as well as the total geometric area, the angular resolution and sensitivity of the telescope are defined. ProtoMIRAX was designed to study the brightest sources, e.g., in the Galactic Center. Sources in this field (the black hole candidate 1E 1740.7-2942 is an example) display a rich spectra temporal variation. In this study we’ll focus in the development of the pMRX hard X-ray camera (pHXC), which consists of an array of 13 ⇥ 13 CZT detectors. We’ll show the pHXC current stage and show our laboratory development of associated electronics for atomic/nuclear radiation detectors (such as CZT). To our knowledge, there’s no similar effort in Brazil, and we’ll highlight how pMRX drove our technical solutions. Estimated sensitivities are also presented in order to strength the scientific capabilities of pMRX. B 1 [email protected] Instituto Nacional de Pesquisas Espaciais 489 Instrumentation Posters INST-1: #295 Advances in the astronomical site testing in Colombia González, D.B1 ; Pinzón, G.1 We present preliminary results concerning the first year of astronomical site testing campaing in Colombia. In particular, the characterization of the Northeast of Colombia. The searching started in 2011 with the careful analysis of GOES imagery in infrared following a novel methodology using metereological data of the wheather stations network of IDEAM. We computed the annual cloud covering over the country and classified the nights as clear or usable based on the definition of a quality factor. Seven regions of interests emerged over the country being the most notable: The Parque de los Nevados at 4000m of altitude with ⇠150 usable nights per year. Other interesting regions are the Sierra Nevada de Santamarta at 3400m and the Sierra Nevada del Cocuy at 4000 with less of 100 usable nights per year. We also present measurements of seeing using a DIMM, coefficient of extinction, brightness of sky and meteorological data that have done at these specific places. B 1 [email protected] Observatorio Astronómico / Facultad de Ciencias, Universidad Nacional de Colombia, Bogotá 490 Posters Instrumentation INST-1: #296 Image reduction of multi-chip near-IR data using the THELI pipeline Holhjem, K.B1 In this this poster I present a step-by-step guide to reducing multi-chip data using the THELI pipeline, focusing on near-infrared data taken with the Spartan camera on the Southern Astrophysical Research (SOAR) telescope. The goal is to provide the reader with sufficient information to reduce data on their own using THELI. For hands-on illustration I reduce 2 different data set. The first seeks to detect an extended object in the near-IR, (which has so far only been seen in narrow-band optical imaging,) thus the images contain a target covering ⇠ 25% of one of Spartan’s 4 detectors. The goal of the second data set is to determine accurate photometric zeropoints for each detector, and is comprised of observations of several photometric standard stars at different airmass. B 1 [email protected] Southern Astrophysical Research (SOAR) telescope, Chile 491 Instrumentation Posters INST-1: #297 Atmospheric and coupling scintillation in optical long-baseline interferometry Lachaume R.B1,2 Scintillation is a time modulation of the flux received from stars due to the diffraction by the turbulent layers in the upper atmosphere. It gets stronger as exposure times become briefer. As a consequence, differential scintillation plays a role in optical interferometers when typical exposure times of a few milliseconds are used to freeze the atmospheric turbulence: the flux received from the different telescopes are not equal and their ratio is time dependent. In addition to atmospheric scintillation, a coupling scintillation is produced by the variations of the coupling efficiency of light beams into optical waveguides. In this poster we report measurements of the time scales and strength of the differential scintillation at the Very Large Telescope Interferometer with the PIONIER afocal instrument and model the interaction between atmosphere and instrument to connect scintillation with the properties of the atmospheric turbulence. B 1 2 [email protected] Centro de Astroingenierı́a, Instituto de Astrofı́sica, P. Universidad Católica de Chile Max-Planck Institut für Astronomie 492 Posters Instrumentation INST-1: #298 Surface Layer turbulence profiling with the SL-SLODAR and LUSCI at ESO Paranal Observatory Lombardi, G.B1 ; Sarazin, M.2 ; Char, F.3 ; González Ávila, C.4 ; Navarrete, J.1 ; Tokovinin, A.5 ; Wilson, R. W.6 ; Butterley, T.6 In the context of the Surface Layer (SL) investigation at ESO Paranal Observatory, a SL Slope Detection And Ranging (SL-SLODAR) instrument prototype has been used at Paranal during 2012, while Lunar Scintillometer (LuSci) measurements campaigns are being carried out since 2008. Simultaneous Surface Layer profiling data from the two instruments are analyzed in order to compare the two instruments to enforce their reliability and finely characterize the Paranal Surface Layer profile. Instruments, data acquisition and analysis, and results are discussed. B 1 2 3 4 5 6 [email protected] European Southern Observatory,Chile European Southern Observatory, Germany Unidad de Astronomia, Universidad de Antofagasta, Chile Las Campanas Observatory, Carnegie Institution of Washington, Chile AURA/CTIO/NOAO, Chile Department of Physics, Centre for Advanced Instrumentation, University of Durham, UK 493 Instrumentation Posters INST-2: #299 Improving INPE’s balloon ground facilities for operation of the protoMIRAX experiment Mattiello-Francisco, M. F.B1 ; Rinke, E.1 ; Fernandes, J. O.1 ; Cardoso, L.1 ; Cardoso P.1 ; Braga, J.1 The development and operations of the balloon-borne protoMIRAX telescope experiment will make use of the ground facilities already available at INPE in order to reduce costs and optimize resources. Aiming at a cost reduction on the development and operations of the balloon-borne protoMIRAX telescope experiment, the system requirement for reusing the ground facilities available at INPE was a challenge to the ground system engineers. Different age technologies were required to interoperate. The existing one decade-old balloon ground station needed little hardware maintenance, but significant effort on software updating was required. Moreover, considering that protoMIRAX is a pathfinder for the MIRAX (Monitor e Imageador de Raios X) scientific satellite mission, a ground infrastructure compatible with INPE’s satellite operation approach would be useful and highly recommended to control and monitor the experiment during the balloon campaigns. This approach will make use of the SATellite Control System (SATCS), a software-based architecture developed at INPE for satellite commanding and monitoring. SATCS complies with particular operational requirements of different satellites by using several customized object-oriented software elements and frameworks. The system had been successful customized for testing the engineering model of the third China Brazil Earth Research Satellite (CBERS3) and was recently integrated to the INPE’s Satellite Control Center to support CBERS3 satellite to be launched this year. Here, we present the ground solution designed for protoMIRAX operation, the Control e Reception System (CRS), focusing on reuse. Driven by SATCS commanding and monitoring framework, the improvements on INPE’s ground facilities comprised only investments on information technology. The standalone computer system available in the balloon ground station rack was modernized both in hardware and software (OPS/ES). In addition, a new server computer, properly configured with Ethernet, has extended the existing ground station facilities with switch, converters and new software (OPS/SERVER) in order to support the available uplink and downlink channels being mapped to TCP/IP gateways required by SATCS. Currently, the CRS development is customizing the SATCS for the kernel functions of protoMIRAX command and telemetry processing. Design-patterns, component-based libraries and metadata are widely used in the SATCS in order to extend the commanding and monitoring frameworks to address the Packet Utilization Standard (PUS) for ground-balloon communication, in compliance with the services provided by the data handling computer onboard the protoMIRAX balloon. B 1 [email protected] National Institute for Space Research - INPE, Brazil 494 Posters Instrumentation INST-2: #300 Fotometrı́a de la luz cenicienta y albedo lunar para la determinacion del espesor optico atmosférico local Ortega, AB1,2 ; Falcón, N1 La temperatura efectiva de la Tierra, puede ser evaluada indirectamente a través de la determinación del albedo terrestre; una medida confiable de este, es la cuantificación de la luz reflejada por la luna en su región no iluminada por el sol (luz cenicienta). Se discute el balance energético de la irradiancia lunar y la luz cenicienta, y se presentan las observaciones realizadas en Valencia (Venezuela) en el bienio 2011-2012, de la fotometrı́a Lunar visible y de la opacidad del cielo nocturno. Para ello se diseñaron y construyeron radiómetros fotoeléctricos, empleando fotoresistores como elementos sensibles, unidos a un amplificador operacional (OP07) y un convertidor analógico digital Minilab1008. Los resultados preliminares obtenidos, muestran que las variaciones locales de la opacidad atmosférica ocasionan un sesgo en las mediciones del albedo y un espesor óptico atmosférico promedio 0.0799 ± 0,0003. Se concluye que los radiómetros telescópicos construidos, junto a los valores del albedo obtenidos por otros métodos pueden ser usados para estimar la opacidad de la atmosfera local y en consecuencia son una medida indirecta de la polución atmosférica de los lugares de observación. Se agradece el financiamiento del FONACIT (Venezuela) a través del Proyecto Estratégico 2011-000326 “Caracterización de fenómenos transitorios en la Troposfera”. B 1 2 [email protected] Laboratorio de fı́sica de la atmosfera y del espacio ultraterrestre, Dpto. de Fı́sica, FACyT, Universidad de Carabobo Dirección de Informática, Universidad de Carabobo. 495 Instrumentation Posters INST-2: #301 The high resolution pixelated CZT detectors for the MIRAX Mission Rodrigues, B. H. G.B1,2 ; Braga, J.1 ; Grindlay, J. E.2 ; Allen, B.2 ; Hong, J2 ; Barthelmy, S.3 ; D’Amico, F.1 ; Rothschild, R. E.4 INPE’s Monitor e Imageador de Raios X (MIRAX) mission will be the first Brazilian astrophysics experiment in space. MIRAX will perform an unprecedented high-cadence, wide-field, wide-band hard X-ray (5-200 keV) survey of Galactic X-ray transient sources MIRAX is scheduled to be launched in near-equatorial low Earth orbit in 2018 as part of the the Lattes satellite payload. MIRAX will carry two coded-mask telescopes with Cadmium Zinc Telluride (CZT) detector planes. One will be a space- qualified version of the Brazilian protoMIRAX telescope (M1); the second telescope (M2) will use an array of 64 closely tiled CZT pixelated detectors developed by the Harvard-Smithsonian Center for Astrophysics (CfA) in close cooperation with INPE and the NASA Goddard Space Flight Center. In this confguration, M2 will have a total detection area of 240 cm2 , large field of view (25 ⇥ 25 ⇥FWHM), high angular resolution (6 arcmin) and good spectral resolution (⇠ 2 keV @ 60 keV). A prototype of M2 telescope has been developed, tested and flown in a stratospheric balloon-borne experiment by CfA as the second generation telescope of the ProtoEXIST program, ProtoEXIST2 (P2). The 64 detector crystal units (DCUs) are made by an ASIC, developed by Caltech for the NuSTAR telescope, hybridized to a CZT crystal with 0.6 mm pixel size. The performance of each detector was evaluated using radioactive sources in the laboratory. The calibration results show that the P2 detectors have average energy resolution of ⇠ 2.1 keV @ 60 keV. Values as low as ⇠ 1.9 keV have been achieved with some individual detectors. P2 was also successfully tested on near-space environment on a balloon flight, demonstrating the detector unit readiness for integration on a space mission telescope, as well as satisfying all MIRAX mission requirements. In this work we show results of validation and calibration tests with individual CZT detectors of P2. B 1 2 3 4 [email protected] Instituto Nacional de Pesquisas Espaciais (INPE) Harvard-Smithsonian Center for Astrophysics (CfA) NASA Goddard Space Flight Center (NASA-GSFC) University of California-San Diego (UCSD) 496 Posters Instrumentation INST-2: #304 Construction of a radiotelescope Ramos, M. LizB1 ; Garcia, C. Miguel1 The research proposal is developed in this paper is the development of a radio telescope through the guidance of NASA project Radio Jove. Using this model will be accessible to the construction of the receiver, antenna and recorder. This will be used for, as well worth the clarification of the size of the antenna, catch the radio waves emitted by the sun and Jupiter. The project methodology includes three stages. The first stage refers to the collection of information, but in turn, this stage has two subdivisions, the electronic level study of the operation and construction steps telescope and recompiling study of astronomy and also information on the origin emissions of the two massive bodies in the solar system, which can capture the radio telescope signals. The second step comprises the construction and completion of an introductory line to new research. And finally, the third stage involves analyzing the location of the telescope to avoid interference, the call for students who want to participate in the research in this line and finally, it is intended to give talks to guests by the seed as a method for extend this knowledge to the public. The result so far is the progress in the first stage, the information collected and the receiver circuit which we are studying and simulating to avoid errors when performing physically. B 1 [email protected] AstroIngenierı́a seedbed research, Distrital Francisco Jose de Caldas University 497 Teaching & Outreach Posters TO -1: #305 Data Acquisition System for Instructional Spectroscopes Almeida, C. B. S.B1 ; Hetem, A.1 This article aims to present a data acquisition software developed in scientific initiation program - IC, for use in the design of a spectrometer built by students. The program was built in C++, a language in wide use today. The origin of spectra used is a simplified model of rustic spectroscope. This equipment basically consists of a box that does not allow light to enter, except through a slit made in the side of it, a diffraction media and a camera for data acquisition. After the image acquisition, one executes the data processing, followed by the usual steps of reduction and analysis of this type of tool. We have implemented a method for calibrating the spectroscope, through which one can compare the incidence of the photons with characteristic of each monochromatic wave. The final result is a one-dimensional spectrum that can be subsequently analyzed. B 1 [email protected] UFABC - Federal University of ABC, CECS 498 Posters Teaching & Outreach TO -1: #306 Astronomy and the interdisciplinary undergraduation formation Alves, V. M.B1 ; Krebs, P. R.; Malvina, A. P.; Lopes, B.; Vieira, E. S.; Amaral, F.; Veronez, G.; Giron, J.; Rodrigues, J.; Zimmermann, L.; Tavares, L.; Sampaio, M.; Britto, T.; Gomes, V. Astronomy is a consensual captivating area which attracts public to all activities and, because of that, is often taken as a door to scientific outreach. The Laboratory of Astronomy of Federal University of Pelotas has been doing outreach activities, like observations, planetarium sessions, continuing teacher formation workshops, lectures, among others, counting with volunteering undergraduation students from many different areas. This year, through financial support, the student group increased in quantity and quality. The Laboratory project involves exploration of Astronomy in many perspectives suitable for those undergraduation courses formation. So, the movie student can contribute for new planetarium sessions, the art and design student can develop visual identities and posters for the activities, the physics students can elaborate the activities contents, the engineering students can dedicate themselves to the use of equipments and other related activities, the philosophy student can explore the subjacent implications of astronomy knowledge, the architecture student can collaborate to the retrieving planetarium project, the anthropology and psychology students can connect the activities to human development and the international relation student can contribute to the group engaging it to worldwide projects as well as administration tasks. This group also works together at many activities, besides their own interest. This presentation will show how the UFPel’s Laboratory of Astronomy is coordinating these activities and a new undergraduation discipline of astronomy opened to all University students as an optional discipline which presents the basic astronomy concepts, observations informations and links to the students areas through seminars presented by them. B 1 [email protected] Laboratory of Astronomy, Federal University of Pelotas 499 Teaching & Outreach Posters TO -1: #307 Parâmetros fotométricos de cometas observados visualmente Amorim, A.B1 Após a oficialização da descoberta de um cometa o Minor Planet Center (MPC/IAU) divulga os elementos orbitais e parâmetros fotométricos do objeto, sendo possı́vel calcular as efemérides para seu futuro acompanhamento. Enquanto que os elementos orbitais são úteis para se conhecer a trajetória aparente do cometa na esfera celeste, os parâmetros fotométricos permitem avaliar o comportamento do brilho do objeto. A fórmula normalmente usada para tal acompanhamento é m1 = H0 + 5 log + n2.5 log r, sendo que os parâmetros fotométricos inseridos na fórmula são a magnitude absoluta H0 e o ı́ndice fotométrico n. Tais parâmetros são calculados com base nas observações fotometricas do cometa e destaca-se neste trabalho o papel da fotometria visual. É comum haver atualização nos valores destes parâmetros conforme o cometa se aproxima do Sol ou quando experimenta outbursts. Nos últimos 3 anos pelo menos quatro cometas foram acompanhados visualmente, a saber: C/2011 C1 McNaught, C/2011 L4 Pan-STARRS, C/2011 W3 Lovejoy e C/2012 F6 Lemmon. No caso dos cometas C/2011 C1 e C/2012 F6 as observações visuais indicaram parâmetros fotométricos diferentes das efemérides inicias do MPC, de modo que estes cometas mostraram-se mais brilhantes do que inicialmente se esperava. Já o C/2011 W3 foi um sungrazer (grupo de Kreutz) e as observações visuais pós-periélio permitiram calcular com relativa precisão seus parâmetros fotométricos (considerando que o último cometa Kreutz observado in ground foi o C/1970 K1). Por sua vez o cometa C/2011 L4 apresentou um comportamento consistente com os parâmetros fotométricos obtidos inicialmente, apesar de algumas variações de brilho na fase pré-periélica. A atualização dos parâmetros fotométricos de um cometa é importante principalmente quando na divulgação de informações ou programação de observações do objeto. Os programas planetários de computador usam os parâmetros fotométricos divulgados pelo MPC/IAU, mas nem sempre tais valores estão atualizados com base nas observações mais recentes, perdendo-se a oportunidade de acompanhar um cometa visualmente brilhante. Em 2013, por exemplo, muito se comenta a respeito do cometa C/2012 S1 ISON cujas efemérides iniciais apontavam para uma magnitude visual total da coma em 13 embora os parâmetros atualizados em julho de 2013 (MPEC 2013-N23) mostram que o cometa não deve ser mais brilhante que magnitude 9, estando o objeto a apenas 0,5 graus de elongação do Sol em 28/11/2013 às 18:00 TU. Este trabalho inclui curvas de luz dos cometas mencionados e tabelas comparativas entre os parâmetros fotométricos calculados com base nos registros visuais e aqueles divulgados pelo MPC/IAU. B 1 [email protected] Núcleo de Estudo e Observação Astronômica ”José Brazilı́cio de Souza” 500 Posters Teaching & Outreach TO -1: #308 Evaluation of Learning of Synchronous Rotation of the Moon Mediated By Computational Resource Fagundes, A. L.B1 ; Silva, T. da1 ; Barroso, M. F.2 We report in this paper an evaluation of learning about the synchronous rotation of the Moon by analyzing results of the use of hypermedia ”The Sun, Earth and Moon” in blended learning intervention of an introductory physics discipline a course in the field of exact sciences. The animation is displayed in a dynamic interactive screen on which the user has control of the progress of the animation sequence. The results are obtained from quantitative and qualitative analysis of issues drawn from a pre-test and a learning assessment applied by the teacher in 2011 counting with 77 students respondents. Learning outcomes indicate that animation helps in learning the phenomenon of synchronous rotation of the Moon and students evaluate the use of animations as a motivator and facilitator of learning. B 1 2 [email protected] Universidade Federal de Santa Catarina Universidade Federal do Rio de Janeiro 501 Teaching & Outreach Posters TO -1: #309 Mostra Astronômica: building the reality as a dream B1 Fonseca, J. E. S. ; Brasil, P. I. O.2,3 ; Molina, M. C.4 ; Ribeiro, F. B.1 ; Livorati, A. L. P.4,5 ; Reiss, M.1 ; Aleixo, C. A. A.1 ; Ottani, V. C. Since 2009 the amateur astronomy group M104 - “Los Sombreros” - have organized the event called “Mostra Astronômica”. In 2013 we have celebrated our 5th anniversary with its fifth Edition. Every year the Mostra Astronômica is hold at UNESP (São Paulo State University), in Rio Claro-SP campus. The aim of our event is creating a whole week dedicated to Astronomy & Astronautics. Many of the best Brazilian professional and amateur astronomers have showed up through the last years. Lots of themes were addressed, from astrophotography to black holes, passing through a trip by the Solar System. Beyond the lectures, we also conducted diurnal and nocturnal observations of the sky, with dozens (sometimes hundreds!) of participants, and technical visits to observatories, planetariums and radio-telescopes. We already sum more than 100 hours of activities, with more than 600 participants in the last five years. As a result, our group is becoming stronger year after year. We have now members as undergrad and grad students in many important universities and research institutes, as for example: São Paulo University (USP), National Institute for Space Research (INPE), São Paulo State University (UNESP), Southwest Research Institute (SwRI) in Boulder-CO, and University of Bristol in Bristol-UK. We are now encouraged to give a step farther and are developing our sixth edition, that most probably will be called “Super Mostra”. We are planning to bring worldwide known scientists from Brazil and abroad. Up to now, we have at least four international scientists confirmed (all with NASA’s grants, and in important positions as Principal Investigator). We look forward to achieve our most audacious endeavour. And we are going to give all details in LARIM 2013. Join us to bring this dream to reality! B 1 2 3 4 5 [email protected] Universidade Estadual Paulista - UNESP Instituto Nacional de Pesquisas Espaciais - INPE Southwest Research Institute - SwRI Universidade de São Paulo - USP University of Bristol 502 Posters Teaching & Outreach TO -1: #310 Brazilian Eratosthenes Project Langhi, R.B1 ; Vilaça, J.2 Introduction and objectives: The objective of Brazilian Eratosthenes Project is the development and application of teaching training actions according the docent autonomy concept (CONTRERAS, 2002) to basic Astronomy teaching. These actions include socials relations with Brazilian schools and international schools using Communication and Information Technologies (TIC). Schools are helped to plan their interdisciplinary experiments with gnomons according the Earth radius measurement done for Eratosthenes (ENGELS, 1985). Argentina coordinates the project in South America (BEKERIS et al., 2011) and Brazil works in this project since 2010 with the theme “Projeto Eratóstenes Brasil” in the homepage http://sites.google. com/site/projetoerato. Methodology: Two schools measure a stick’s shadow and communicate their results. After, they calculate an average radius of Earth. The stick (gnomon) should stay in vertical position in the leveled ground. The measurements must be made at solar midday, like Eratosthenes did in the past. Since 2010, the project received hundreds of Brazilian schools with different experiments that were constructed with autonomy, because our site doesn’t show some itinerary pre-ready to elaborate the experiments (ARAUJO e ABIB, 2003). To collect data we will use interviews via skype with the teachers. These data are useful to researches about Science Education area and the Teaching Formation. Results and Discussions: In three years (2010 to 2012) we had a increase the number of Brazilian schools who submitted their measurements at project’s homepage, while other countries not. Argentine project coordination uses statistics models to choose the pairs of schools to result in a best Earth radius average. However some schools prefer to use their autonomy to choose a pair. But this choice is not mandatory. Then, teaching professional practice could change and we see modifications in the teacher’s work, what depends of their realities and context. This project intents to respect the docent autonomy. This autonomy to responsible modifications during continued formation is called ”activist formative model” according Langhi & Nardi (2012). Considerations: This project discusses about researches in Astronomy Education - still extreme rarely in Brazil, when we compare with other areas in Science Education. We believe that actions like this could motivate the students to learn more Astronomy. Furthermore, this national action can be a rich source of data to investigations about teaching formation and scientific divulgation. With help of researches groups of undergraduate and graduate students, we can produce more researches and papers, contributing to bibliographic academic production about Astronomy Education. B [email protected] UNESP/Bauru. Faculdade de Ciências. Departamento de Fı́sica. Programa de Pós-Graduação em Educação para a Ciência. Apoio: Pró-Reitoria de Extensão Universitária (PROEX) 2 Polo Astronômico Casimiro Montenegro Filho (FPTI/BR). Apoio: Programa de fomento do PTIC&T/FPTI-BR. 1 503 Teaching & Outreach Posters TO -1: #311 Defining our place in the cosmos. Mapping the vision of the brazilian population about the Universe and its origins Leroy, P.B1 ; Diniz, A. C. S. This paper discusses the concepts of different segments of the population with respect to the latest knowledge of cosmology. We intend to make a diagnosis map that portrays the spread of this scientific knowledge in various sections of the population, taking into account the level of education and distance from large urban centers. Our question is: in what extent the standard model of cosmology is present in the lives of ordinary people? The evaluation is done through multiple choice questions seeking to portray people’s knowledge, starting from the size and shape of the earth, passing through the solar system and the galaxy until the size and age of the Universe. In this first part we analyze the conceptions of the academic public in universities, including students and teachers divided into three different areas: Exact, Biological, and Social and Human. After that, will be analyzed different population groups: urban center, metropolitan, inner cities, rural areas and indigenous communities. B 1 [email protected] Museu de Ciências Naturais. Grupo de Astronomia e Astrofı́sica. Pontifı́cia Universidade Católica de Minas Gerais 504 Posters Teaching & Outreach TO -1: #312 Materiais Interativos no Ensino de Astronomia Josué, A. M.B1 ; Marcos, R. V.2 Apesar de fazer parte dos Parâmetros Curriculares Nacionais do Ensino Fundamental (Terra e Universo) e das Orientações Curriculares para o Ensino Médio (PCN+ Universo Terra e Vida), que são os documentos oficiais brasileiros que norteiam a Educação Básica, constar nas propostas dos vários estados brasileiros, contribuir para o desenvolvimento humano e tecnológico, o ensino de Astronomia na maioria das vezes é apresentado como algo estanque dentro de algumas disciplinas e pouca atenção é dedicada a esse assunto. As tecnologias digitais envolvendo materiais interativos são comumente utilizadas pelos jovens e renegados pela maioria dos docentes. Neste sentido, desenvolveu-se uma pesquisa, com o objetivo de apontar as potencialidades da utilização de materiais interativos no ensino de Astronomia. Ofereceu-se um curso de aperfeiçoamento em Astronomia, cuja meta era levar os participantes a compreenderem os fenômenos astronômicos. Seguiram-se as seguintes etapas: i) análise dos projetos pedagógicos dos cursos (PPC) das licenciaturas do Instituto Federal de Educação, Ciência e Tecnologia do Norte de Minas Gerais (IFNMG), Campus Januária, lócus da pesquisa; ii) análise das pré-concepções dos alunos em relação às tecnologias digitais e à Astronomia, identificadas através da aplicação de um questionário inicial; iii) elaboração do curso levandose em consideração os conhecimentos prévios dos alunos; iv) aplicação da proposta de ensino que se desenvolveu na modalidade semipresencial, utilizando várias ferramentas interativas; v) aplicação e análise do questionário final. A amostra foi constituı́da por trinta e dois alunos dos cursos de licenciatura em Fı́sica, Matemática e Biologia. Utilizou-se a metodologia qualiquantitativa, combinada com análise de conteúdo. Entre outros resultados, foi possı́vel verificar que: (i) apenas o curso de licenciatura em Fı́sica contempla alguns conteúdos de Astronomia, mesmo assim de forma fragmentada em várias disciplinas; (ii) a análise do questionário inicial mostrou que o grupo pesquisado possui pouco ou nenhum conhecimento de temas relacionados à Astronomia, o que pode ser explicado pela renegação dessa ciência na educação básica do Brasil; (iii) a análise do questionário final mostrou que ocorreu uma aprendizagem significativa, uma vez que os resultados encontrados apontam para uma melhoria significativa nas respostas dos alunos; (iv) os resultados indicam um alto nı́vel de satisfação dos alunos; (v) percebeu-se ainda a viabilidade da utilização de recursos envolvendo as tecnologias digitais e materiais interativos no ensino de Astronomia, o que pode contribuir para o alargamento das opções metodológicas dos futuros docentes e suprir suas carências formativas. B 1 2 [email protected] Instituto Federal de Educação, Ciência e Tecnologia do Norte de Minas Gerais Universidade Cruzeiro do Sul 505 Teaching & Outreach Posters TO -2: #313 Elementary School Teachers’ Conceptions about the Apparent Movement of the Sun and the Shadows of the Objects Machado, D. I.B1 A research about the astronomical conceptions of 65 elementary school teachers, developed during a didactic module carried out at the end of a continuing education course, in the second half of 2012, is described. The didactic module, with duration of two hours, addressed the apparent movement of the Sun in the celestial sphere and its relation with the shadows of the objects, as well as the functioning of sundials. The activities included the construction and the use of a horizontal sundial and of an analemmatic one. It was also used a concrete didactic model to simulate the apparent movements of the sun and its effects on the shadow of a rod. The research was based on a constructivist framework, considering prior conceptions and the meaningful learning of concepts. A test with five open questions was applied to the participants before and after the activities. Initially, the participants already had notions about the themes treated, because almost all recognized: the existence of variations in the position of the Sun in the celestial sphere both throughout the day as well as during the year; the existence of relations between such apparent movements and changes in the shadows of the objects; the possibility of using the shadows of the objects to measure the time. However, a little more than half of the participants (53.8%) expressed, at first, the misconception that the sun passes daily by zenith. And, in general, the responses had incomplete explanations. After the activities, some development in the explanations of the phenomena, indicating a greater degree of progressive differentiation of concepts was observed. For example, there was an increase in the percentage of responses indicating that the length of the shadows varies throughout the day (from 18.4% to 41.6%) and during the year (from 6.1% to 29.2% ), depending on the position of the sun; an enlargement in the proportion of responses considering sundials as devices that permits the reading of the hours on the basis of the behavior of the shadows (from 3.1% to 29.3%); and an expansion in the percentage of answers with the opinion that the sun is not daily by zenith (from 36.9% to 95.4%). It’s concluded that the theoretical and practical approaches adopted can contribute to the understanding of the topics investigated. However, activities for consolidation of learning seem to be necessary for the participants to achieve a higher degree of elaboration of explanations. B 1 [email protected] Unioeste, Foz do Iguaçu, Brasil 506 Posters Teaching & Outreach TO -2: #314 RECA: A network by students, for students Remolina Gutiérrez, M. C.B1 ; Velasco Moreno, S.1 ; Hoyos Restrepo P.1 RECA (Red de Estudiantes Colombianos de Astronomı́a) is a national network created by Colombian students that needed to be connected by their love for astronomy and astrophysics. It compiles most of the university groups and individuals that are willing to make part of a bigger community that gives benefits such as outreach activities, student links, and resources. This talk will be divided in 3 main parts. The first one is going to be a quick review of the history of RECA since it was proposed in the III Colombian Astronomy Congress until today. After that, there will be a section of all the achievements and activities that the network has made and the people that collaborated to make it possible. Finally, there is going to be an emphasis on the vision that RECA has for the next years and what it can give to the development of astronomy in Latin America regarding to students’ flux, training and research. B 1 [email protected] Universidad de los Andes, Colombia 507 Teaching & Outreach Posters TO -2: #315 A Proposal of Astronomy Teaching on the Museu de Ciencias Naturais Pontificia Universidade Catolica de Minas Gerais Ribeiro, B. A. G.B1 ; Leroy, P.1 On this paper we analyze the non-formal approach of astronomy teaching, done by educators of the Museu de Ciências Naturais of Pontifı́cia Universidade Católica from Minas Gerais, for students of middle school. It has been used the “Para Ver Estrelas” project, which has different approaches for each school. There are lectures, planetary sessions, workshops, demonstrations and observation with telescope. The main objective was to identify the benefits of a non-formal teaching, testing the methodology used on the visits. Data was collected through questionnaires applied before and after the visits, then it is done a comparative analysis of the methodology efficiency and wrong previous knowledge. B 1 [email protected] Museu de Ciências Naturais, Pontifı́cia Universidade Católica de Minas Gerais(Grupo de Astronômia e Astrofı́sica) 508 Posters Teaching & Outreach TO -2: #316 OEI, GTTP and Adventurers of the Universe: training teachers and scientific dissemination at the South of Brazil Pavani, D. B.1 ; Saraiva, M. F. O.B1 ; Dottori, H.1 Itinerant Educative Observatory (OEI) is a permanent program of the Department of Astronomy /Institute of Physics/UFRGS since 1999. It aims to lecture Astronomy to teachers of fundamental and middle levels, using attractive resources such as telescopic observations, audiovisuals, and multimedia. The material resources are a van, Meade 12” telescope, binoculars, experimental kits, and computer and data-shows. The training courses are requested by different cities of Rio Grande do Sul and nearby states, and are organized by a local committee of the requesting city. The OEI goes to the city taking the instructors and the instructional material. OEI was recently selected by the federal government to receive funds in 2014. The funds will finance 10 training courses, outreach activities and scientific literacy for teachers and the general public of the southern states of Brazil. In this new edition of OEI, we are uniting efforts with other extension project in which the Department of Astronomy has been engaged since 2009 – the Galileo Teacher Training Program (GTTP). This is an international program developed to train teachers in the effective use of astronomy education tools and resources in their science classes. The program, that is a legacy of IYA2009, aims to create a worldwide network of Galileo Ambassadors – the promoters of the training worshops – and Galileo Teachers – the teachers who bring the learned methodologies into classroom. To supplement these activities, the Department of Astronomy initiated a new program in 2012 called “Adventurers of the Universe”. University professors, undergraduates students and teachers of highschool and elementary school of social vulnerable communities develops transdiciplinary didatic sequences where Astronomy is the central focus to motivate different processes of teaching and learning, considering different learning levels, designed for direct use in the classroom. The objective of the program is to contribute to the didatic transposition through the discussion about how to relate astronomy with other science and non-science disciplines. We focused on three major questions: (1) How does the Universe look like and what is my place in it? (2) Is the Universe always the same? What changes in it? (3) How do we participate in the transformation of the Universe? The Adventurers began in 2012 through collaboration with 20 teachers of one school, when the activities impacted 900 students. In the current year, the collaborations were expanded to include teachers and students of 3 other schools. B 1 [email protected] Department of Astronomy of Institute of Physics of Federal University of Rio Grande do Sul/UFRGS 509 Teaching & Outreach Posters TO -2: #317 South Africa calls Italy: effective exchange activity through costless (Skype like) connections in the framework of the EU UNAWE Lara Albanese1 ; Alessandra ZanazziB1 In summer 2012 the Italian EU-UNAWE team joined with the South African team in Cape Town, working with the township schools organizing activities at school and also a teachers’ training event at the SAAO Observatory. In order to involve in the exchange not only the project’s experts but also to the teachers and the children, we organized Skype connections between the Cape town teachers participating in the project and the teachers in Sicily (South Italy) that also participated in one of the Italian training sessions and later between the children of the Italian school and those in Zanemfundo School (Cape Town). Thanks to this chance of seeing each other and talking directly, children have - with huge interest and participation - shared and learned methods, experiences, curiosities. They shared their prepared actual science researches, in order to understand why an equal gnomon cast different shadows at the same time in the two countries. The teachers confronted on curricula, didactic methodologies such as working with a background story during the whole school year, interdisciplinary uses of astronomy, languages etc. The EU-UNAWE project and International or Regional conferences such as LARIAM are perfect chances to create exchanges between countries all around the World, and this simple communication model between children and teachers appears like an enormous resource yet to be fully exploited. B 1 [email protected] INAF - OSSERVATORIO ASTROFISICO DI ARCETRI (FLORENCE, iTALY) 510 Posters Teaching & Outreach TO -2: #319 Presentation of the project for the recovery, scientific equipment and automation of Astronomical Observatory of the ITM Torres C., Andres DavidB1,2 ; Ocampo, Luis Fernando2 The Astronomical Observatory of ITM was founded in 1941 by Brother Daniel of the Lasallian Christian Schools, worked for 60 years, as part of the Museum of Natural Sciences to provide services to the scientific communities of Medellin city - Colombia. In the 90’s was closed leaving Medellin without a site for observing the sky that was properly equipped for educational and research activities. The main objective is to recover the Astronomical Observatory to link it to the scientific and educational activities of the Museum and the University. To carry out this project were conducted technical studies (Sky Quality Study, earthquake resistance study and the proper scientific instrumentation). On the other hand the architectural designs were made to build the new building and the dome, to be automated to allow a second phase; the observatory can be robotized and remote controlled from any location that has Internet access. B 1 2 [email protected] National University of Colombia. Physics School. Sciences Faculty Natural Sciences Museum of La Salle, a project of ITM. Astronomical Observatory 511 512 Author index 513 Author index Abadi, M. G. Alcaniz, J. S. The abundance of galaxies and dark matter halos in the ⇤CDM Universe, 103 Abraham, Z. Aleixo, C. A. A. LLAMA Project, 173 Abraham, Z. Multiwavelength study of the young Parsec-scale Activity in BL Lacertae: emission-line region and star-forming , 435 Alencar, S. Studying the kinematics of the jet of 3C279 using the method Cross-entropy, 431 Finding proto-spectroscopic binaries: Precise multi-epoch radial velocities of 7 protostars Abramo, L. R. 2-Pt. Correlation Function for Luminous in Ophiuchus, 332 Alencar, S. Red Galaxies, 464 Abramo, L. R. Molecular hydrogen and [Fe II] in active galactic nuclei - III. Low-ionization nuclear Signature of Relativistic Jet Precession, 146 Abraham, Z. Mostra Astronômica: building the reality as a dream, 502 Aleman, I. stellar cluster [DBS2003]156, 351 Abraham, Z. Testing Fundamental Hypotheses in Cosmology, 20 Identification and extraction of photo- Observational diagnostics of young stellar objects in NGC 2264, 85 Alencar, S. The inner disks of classical T Tauri stars in metric redshifts of quasars with narrow-band filters, NGC 2264, 331 467 Abramo, L. R. Multiple-tracer surveys of the large-scale Alexander, N. C. Chromospheric and Coronal Activity structure of the Universe, 21 in Stars Before the Main Sequence, 333 Abrevaya, X. C. The BIOSUN project:an astrobiological Alexandre, S. T. Contributions of geomorphology for approach to study the origin of life in the context of the understanding of landscape evolution in rocky the young Sun/solar stellar analogs, 235 planets of the Solar System, 226 Afonso, G. B. Small asteroid fragments in earth-crossing Alfaro, E. orbits, 201 A new insight to the O Vz stars within the framework of the GOSS Survey, 71 Afonso, P. M. J. Alfaro, E. Mass and energy of GRB-SN events: OWN Survey: results after seven years of multi-wavelength analysis of three associations in high-resolution spectroscopic monitoring of South- the context of the full sample, 169 ern O and WN stars, 72 Aguayo, G. Alfaro, M. A long-term study of the Be star Mu Centauri in the L-band, 236 Aguayo, G. Allen, B. Emission-line stars in the star-formation region NGC 1850, 334 Aguena da Silva, M. Allen, B. Constraining Cosmological Pa- formation in accreting neutron stars, 476 clusters: the case of the sigma Orionis cluster, 12 Improvement and analysis of the MILES library for stellar population modelling , 55 Almeida, C. B. S. Data Acquisition System for Instruc- population, 318 A study of the recent chemical tional Spectroscopes, 498 Almeida, L. A. evolution of the Large Magellanic Cloud, 41 Albanese, L. Diversity of protoplanetary disks in stellar Allende Prieto, C. White dwarf-main sequence binaries from SDSS DR8: unveiling the cool white dwarf Ahumada, A. V. A Spectro-photometric study if the young stellar cluster sigma Orionis., 328 Allen, L. Magnetic field evolution and jet Agurto-Gangas, C. The high resolution pixelated CZT detectors for the MIRAX Mission, 496 Allen, L. Cosmology from the Angular Correlation Function and Galaxy Clusters , 154 Aguilera, D. N. The hard X-ray telescopes for MIRAX and protoMIRAX, 175 rameters from Galaxy Clusters, 447 Aguena da Silva, M. Metallicity gradients in tidal tails and merging systems, 405 Assessing and evaluating: a case study High-ionization accretion signatures in compact binary candidates from SOAR Telescope in the framework of EU-UNAWE Italy project, 183 observations, 269 Albanese, L. South Africa calls Italy: effective exchange Almeida, L. A. activity through costless (Skype like) connections in MLS110213:022733+130617: A new eclipsing polar above the period gap, 46 Almeida, L. A. the framework of the EU UNAWE, 510 Alcaniz, J. S. Figure of Merit for Dark Energy Parame- Modeling photometric and spectroscopic data of HS 2231+2441: an HW Vir type system terizations, 454 with a brown dwarf companion, 57 515 Almeida, L. A. Amorim de Oliveira, D. Fireworks at the center of the Multi-band characterization of hot jupiters using OPD data, 27 Milky Way, 121 Almeida, R. M. Large-Scale Anisotropies of the Cosmic Amram, P. Rays Detected at the Pierre Auger Observatory and Andernach, H. the Telescope Array, 475 Alonso, M. V. Galaxy Concentration Index in Low comparisons with other measurements, 390 X-ray Luminosity Galaxy Clusters, 366 Andernach, H. using the VVV Survey, 408 evolution of their host Galaxy Clusters, 449 Anderson, J. P. Spectral analysis of type II Supernovae, behind the Galactic bulge using the VVV Survey, 409 171 Andrés F. Ramos, P. Triplets of galaxies: A connection with compact groups?, 412 galaxies, 434 Andrés F. Ramos, P. for variable stars in omega Centauri, 268 Alonso-Garcı́a, J. Variable stars in the VVV globular models, 394 Andrade, D. Asteroseismology of massive pulsating corrections, 480 Andrade, E. 45 Observación de objetos cercanos a la Andrade, I. S. IFU spectroscopic analysis of the active Programa de observación de ocultaciones nucleus NGC 6951 , 419 Andrei, A. H. del Hato, 213 Finding minor Bodies with the Precise stellar occultation predictions for 39 selected TNOs/Centaurs, 33 Andrei, A. H. JPAS/J-PLUS photometric surveys, 229 Alvarez-Candal, A. accretion disc maps of V2051 Oph mass-transfer instability model, 238 de estrellas desde el Observatorio Nacional de Llano Alvarez-Candal, A. H along outburst: additional evidence in favor of the Tierra (Observation of Neos), 214 Alvarez, R. Classification of long gamma-ray burst using ACF and spectral lag with cosmological DA white dwarf stars with fully evolutionary models, Alvarez, R. Physical parameters of galaxies with star formation through mid-infrared SED clusters, 68 Althaus, L. G. Diagnostic diagrams with polycyclic aromatic hydrocarbons in diferent types of Alonso-Garcı́a, J. Near-IR Period-Luminosity relations The VVV Templates Project, 249 New Catalogues of Superclusters of Abell/ACO Galaxy Clusters up to z ⇠ 0.15, 450 Alonso, S. Confirmation of a cluster of galaxies hidden Alonso-Garcı́a, J. Central Dominant Galaxies and the Andernach, H. The red cluster sequence in low X-ray luminosity galaxy clusters, 458 Alonso, S. An approach to measuring the density of the environment of galaxies: results and Alonso, M. V. Galaxy Detection Behind the Milky Way Alonso, M. V. Metallicity gradients in tidal tails and merging systems, 405 Mapping the early distribution Solar astrometry and the heliometer of Rio de Janeiro, 181 Andrei, A. H. Study of Pluto’s atmosphere from stellar of volatiles in the Main Belt with the JPAS/J-PLUS photometric survey, 38 occultation, 200 Alvarez-Candal, A. Stellar occultation by the trans-Neptunian Andrei, A. H. The SDSS quasars as a testbench for the object 2002 KX14, 195 Alvarez-Candal, A. Gaia fundamental reference frame grid-points, 422 Andres, R. V-type asteroids among the Mars crosser population, 220 Alves, V. M. Andrievsky, S. The role of the corotation resonance in Astronomy and the interdisciplinary undergraduation formation, 499 Amaral, F. the secular evolution of disks of spiral galaxies, 124 Andruchow, I. Astronomy and the interdisciplinary undergraduation formation, 499 bands i ’ and r’, 441 Andruchow, I. in Solar type stars of intermediate brightness, 237 Herschel-ATLAS and ALMA: I. A z=1.027 Angelo, M. S. Structure of Bubbles in the Spectroscopy of the open cluster remnant candidate ESO429-SC02, 292 Angeloni, R. South-East region of the Large Magellanic Cloud, 347 Amirábile, S. The incidence of short time scale variability on different types of Blazars, 147 Einstein Ring of Molecular Gas and Dust, 139 Ambrocio-Cruz, P. Characterization blazars environment PG1553 +113 and 3C66A from GMOS data in the Amazo-Gómez, E. M. Determination of Li abundance Amber, S. Study of Pluto’s atmosphere from stellar occultation, 200 BOMBOLO: a Multi-Band, Wide-field, Near UV/Optical Imager for the SOAR 4m Telescope, Developments with the hard X-Ray de- 178 tection plane of the protoMIRAX imaging telescope, Angeloni, R. The VVV Templates Project, 249 489 Angeloni, R. The WFCAM Variable Star Catalog and Amorim, A. Parâmetros fotométricos de cometas New Variability index, 66 observados visualmente, 500 516 Antón, S. Asorey, H. Astronomy and Astrophysics in the Colom- The SDSS quasars as a testbench for the Gaia fundamental reference frame grid-points, 422 bian Andes: the PAS Project, 172 Antonuccio-Delogu, V. Evolution of the Mass-Metallicity Asorey, H. relations in passive and star-forming galaxies from SPH-cosmological simulations, 110 Arévalo, P. LAGO Project , 485 Assafin, M. Active Galactic Nuclei , 11 Aragón-Salamanca, A. Emission line imaging survey GeMS/GSAOI: from commissioning to Envelopes of Evolved Stars: Galactic and Assafin, M. Magellanic Clouds B[e] Supergiants, 276 using ZEUS-3D, 239 catalogue, 298 Assafin, M. on the evolution of low-mass stars, 240 observed events, 29 Assafin, M. contribution to the study of massive stars, 73 Wind study of B supergiants stars, 241 A new insight to the O Vz stars within the occultation, 200 binaries , 304 Assmann, P. high-resolution spectroscopic monitoring of South- Audibert, A. Avila, M. C. Unveiling the nature of an ultra-luminous X-ray source through the kinematics and structure Avila, M. C. The hard X-ray telescopes for MIRAX and Star formation outside the Elliptical protoMIRAX, 175 Avila-Reese, V. Galaxy NGC2865, 137 A new catatalogue of H I supershell Way/Andromeda-sized galaxies, 136 Arnal, E. M. G126.1–0.8–14: A molecular shell related detection in powerful narrow-line radio galaxies, 150 Axon, D. J. to Sh2-187, 341 Arnal, E. M. LLAMA Project, 173 Axon, D. J. The connection between the origins of Azanha, L. GeMS/GSAOI: from commissioning to Properties of galaxies in fossil and non-fossil groups from the maxBCG sample , 358 operations and science results, 180 Bühler, D. The Discrepant Kinematics of ORLs and Baade, D. CELs in NGC 7009 as a Function of Ionization The GalileoMobile Project, 189 A long-term study of the Be star Mu Centauri in the L-band, 236 Structure, 356 Baade, D. Artale, M. C. Stellar feedback from black-hole high-mass Emission-line stars in the star-formation region NGC 1850, 334 X-ray binaries in galaxy formation models, 357 Balbinot, E. Artur, E. Chemical abundances and physical parame- Mapping Triangulum-Andromeda with the SDSS, 392 ters of evolved stars with planets, 288 Balbinot, E. Transit Timing Variations analysis in exo- Self-consistent physical parameters for 5 intermediate-age SMC stellar clusters from CMD planet host stars, 230 Asorey, H. The Multiwavelength Study of OH Mega- maser Galaxy IRAS16399-0937, 148 galaxy, 364 Artur, E. Kinematics and excitation of the nuclear spiral in the active galaxy Arp 102B, 423 globular clusters and the evolution of their host Arrieta, A. The satellite population of Milky Axon, D. J. HST and Spitzer point source and dust lane candidates in the outer part of the Milky Way, 95 Arriagada, G. Developments with the hard X-Ray de- 489 Armaza, C. On magnetic fields in barotropic stars, 242 Arnold, J. Testing the Physical Properties of the tection plane of the protoMIRAX imaging telescope, of its optical counterpart , 168 Arnal, E. M. The Formation of dSph galaxies, 104 Unified Model for AGN, 420 ern O and WN stars, 72 Arnaboldi, M. Phase Mixing in Popping Star Clusters, 296 OWN Survey: results after seven years of Arias, L. Study of Pluto’s atmosphere from stellar Assmann, P. NIP of Stars: early results and new eclipsing Arias, J. Stellar occultations by trans-Neptunian objects, 224 Assafin, M. framework of the GOSS Survey, 71 Arias, J. Stellar Occultations by Transneptunian and Centaurs Objects: results from more than 10 Overview of Stellar Interferometry and its Arias, J. Proper motion determination of the optically visible open clusters based on the UCAC4 Arceo-Diaz, S. Effects of enhanced neutrino emission Arcos, C. Precise stellar occultation predictions for 39 selected TNOs/Centaurs, 33 Araya, I. Fast and slow radiation-driven wind solutions Arcos, C. Improvement of TNO’s Ephemerides in the context of stellar occultations, 199 Assafin, M. operations and science results, 180 Araujo, F. Astrometric positions for the irregular satellites of Jupiter, Saturn and Neptune, 206 Assafin, M. of the Abell 901/902 supercluster, 130 Araujo, C. Simulation of Water Cerenkov Detector for detection of cosmic rays Using GEANT4 for the modelling, 252 Analysis and validation of data in the search for GRB, 486 517 Balbinot, E. The LMC outer disk stellar population in Barbuy, B. Abundâncias de Zinco em estrelas do bojo the light of the Dark Energy Survey, 135 Ballesteros, J. Galáctico, 278 Barbuy, B. Diversity of protoplanetary disks in stellar clusters: the case of the sigma Orionis cluster, Barbuy, B. 12 Bamford, S. Emission line imaging survey of the Abell modelling, 252 Barres de Almeida, U. The connection between the origins of globular clusters and the evolution of their host Accretion and Activity on the Post- Barroso, M. F. Evaluation of Learning of Synchronous Accretion disc mapping of the shortest Rotation of the Moon Mediated By Computational period eclipsing binary SDSS J0926+36, 275 Baptista, R. H Resource, 501 Barthelmy, S. accretion disc maps of V2051 Oph along outburst: additional evidence in favor of the Infrared accretion disc mapping of the Bate, N. F. Probing AGN accretion through microlens- quiescence, 285 ing, 432 Baptista, R. Probing accretion on the high-magnetized Bauer, F. E. Baptista, R. Searching for cyclical period variations in Baptista, R. Time-lapse and flickering mapping of ac- Beamin, J. C. 48 Beamin, J. C. Weather on Other Worlds: Brown Dwarf burst using ACF and spectral lag with cosmological variability and VVV, 84 Beauge, C. corrections, 480 tions and science results, 180 Barba, R. H. A Candidate Globular Cluster Behind the Beers, T. C. Beers, T. C. The formation of stellar haloes of massive A new insight to the O Vz stars within the framework of the GOSS Survey, 71 Spirals in hierarchical scenario, 111 Beghetto Junior, D. Deep infrared extinction maps of the Fourth Galactic Quadrant based on VVV and Dinâmica da Formação de Galáxias com Anel Polar, 359 Belloni, D. T. GLIMPSE surveys, 342 Infrared study of new star clusters Collisions between Globular Clusters, 293 Benı́tez, S. associated to dusty globules, 330 The GalileoMobile Project, 189 Benedetti-Rossi, G. Precise stellar occultation predic- NIP of Stars: early results and new eclipsing binaries , 304 tions for 39 selected TNOs/Centaurs, 33 Barba, R. H. OWN Survey: results after seven years of Benisty, M. high-resolution spectroscopic monitoring of South- Modeling the circumstellar environment of AB Aur using the Halpha line, 325 Benitez, N. ern O and WN stars, 72 A survey of extended H2 emission MagAl: A new tool to analise galaxies photometric data, 402 Benvenuto, O. G. Decay of the magnetic field in black toward a sample of massive YSOs, 327 Figure of Merit for Dark Energy widow pulsars, 473 Bernal, C. G. Parameterizations, 454 Barboza Jr., E. M. Abundance Analysis of CEMP RR Lyrae Stars, 271 Milk Way?, 319 Barboza Jr., E. M. Distribution and Origin of Hot Planets, 3 Bec, M. GeMS/GSAOI: from commissioning to opera- Galaxy Detection Behind the Milky Way using the VVV Survey, 408 Barbosa, C. L. Proper motions and brown dwarfs in the VVV survey, 83 Baquero Larriva, A. Classification of long gamma-ray Barba, R. H. The Multiwavelength Study of OH Mega- maser Galaxy IRAS16399-0937, 148 cretion discs: measuring the disc viscosity parameter, Barba, R. H. Subhalo abundance matching in different Semi Analytic Models, 410 Baum, S. cataclysmic variable stars, 243 Barba, R. H. Galaxies at High Redshift, 15 Baugh, C. M. polar RX J1007.5-2017, 312 Barba, R. H. The high resolution pixelated CZT detectors for the MIRAX Mission, 496 dwarf nova V2051 Ophiuchi in outburst and in Baravalle, L. The hard X-ray telescopes for MIRAX and protoMIRAX, 175 Barthelmy, S. mass-transfer instability model, 238 Baptista, R. The role of the corotation resonance in the secular evolution of disks of spiral galaxies, 124 CommonEnvelope Binary RR Cae, 272 Baptista, R. Cherenkov Telescope Array (CTA), 176 Barros, D. A. galaxy, 364 Baptista, R. Self-consistent physical parameters for 5 intermediate-age SMC stellar clusters from CMD 901/902 supercluster, 130 Bamford, S. R-Process Abundances in Metal-Poor Galactic Halo Stars, 61 Observational constraints on a The Gravitational Drag Force on an Extended Object Moving in a Gas, 166 Bernardes, L. coupled quintessence model with a generalized DE EoS, 460 A New Paradigm for Habitability in Planetary Systems: the Extremophile Zone, 209 518 Bernardi, R. Bonatto, C. Simulations of atmospheric turbulence with spatiall phase modulators, 487 Merger AM 1219-430 with Gemini/GMOS-S, 378 Bernui, A. Gaussian analyses on PLANCK CMB maps, Bonatto, C. 164 Study of Young Stellar Clusters in the Nebular Complex NGC6357 with VVV, 82 Bernui, A. Bonoli, S. North-South CMB analyses using the Bertone, E. The GalileoMobile Project, 189 Borges, B. Minkowski Functionals, 457 Determination of Li abundance in Solar Searching for cyclical period variations in cataclysmic variable stars, 243 Borges, M. type stars of intermediate brightness, 237 Bertout, C. A kinematic study of the Lupus star-forming Envelopes of Evolved Stars: Galactic and Magellanic Clouds B[e] Supergiants, 276 Borges, M. region, 53 Bessell, M. S. The GALEX Nearby Young-Star Survey, Overview of Stellar Interferometry and its contribution to the study of massive stars, 73 Borges, M. White dwarfs in the Javalambre Physics of 64 Best, P. Photometry and Dynamics of the Minor Star formation at the edge of the Universe, the Accelerating Universe Survey, 259 Borissova, J. Old open clusters in the VVV Survey, 295 336 Beuther, H. Deuteration and fragmentation in massive Borissova, J. Proper motions and brown dwarfs in the star-forming regions, 92 VVV survey, 83 Bhatt, M. The GalileoMobile Project, 189 Borissova, J. Bica, E. Galactic Embedded Clusters with 2MASS Borissova, J. Unveiling the nature of an ultra-luminous infrared photometry, 311 X-ray source through the kinematics and structure Bica, E. Study of Young Stellar Clusters in the Nebular of its optical counterpart , 168 Borissova, J. Complex NGC6357 with VVV, 82 Bicalho, I. C. Metal-Poor Active Galactic Nuclei, 360 Birkinshaw, M. Herschel-ATLAS and ALMA: I. A Lactea (VVV) Survey, 303 Borissova, J. 139 Bortolotto, G. S. Magellanic Clouds B[e] Supergiants, 276 Blain, A. W. Boscardin, S. C. First spatially-resolved observations of Bosch, G. L. Blum, R. D. A survey of extended H2 emission toward espectrofotométrica de miembros de Bochum 7, 62 GeMS/GSAOI: from commissioning to New Opportunities with the Gemini Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 Bouvier, J. Observatory, 10 Photostability of Organic Observational diagnostics of young stellar objects in NGC 2264, 85 Bouvier, J. The inner disks of classical T Tauri stars in Molecules in Circumstellar Environment, 96 Boesso, R. Study of clustering in the stellar abundances NGC 2264, 331 Bradburne, J. space, 294 Boffin, H. M. J. Finding ’jumps’ in light curves using change-point algorithms, 227 Bourne, N. operations and science results, 180 Boechat-Roberty, H. M. Primera identificación astrométrica y Boufleur, R. C. a sample of massive YSOs, 327 Boccas, M. Solar astrometry and the heliometer of Rio de Janeiro, 181 starbursts, 118 Boccas, M. Star detection and study of atmospheric extinction with an All Sky camera, 488 ionized gas in submillimeter-selected high-redshift Two rings but no fellowship: LoTr Assessing and evaluating: a case study in the framework of EU-UNAWE Italy project, 183 Braga, J. Developments with the hard X-Ray detection 1 and its relation to planetary nebulae possessing Barium central stars, 49 plane of the protoMIRAX imaging telescope, 489 Boges Fernandes, M. The Study of Physical Parameters Braga, J. of Unclassified Stars with the B[e] Phenomenon, 248 Improving INPE’s balloon ground facilities for operation of the protoMIRAX experiment, 494 Braga, J. The dense gas in M82, 399 Bom, C. R. D. The SOAR Gravitational Arc Survey, 158 The hard X-ray telescopes for MIRAX and protoMIRAX, 175 Braga, J. Galactic Embedded Clusters with 2MASS infrared photometry, 311 Bonatto, C. Weather on Other Worlds: Brown Dwarf variability and VVV, 84 Bjorkman, J. Envelopes of Evolved Stars: Galactic and Bonatto, C. Using MASSCLEAN to Describe Stellar Clusters Found in the Vista Variables in the Via z=1.027 Einstein Ring of Molecular Gas and Dust, Bolatto, A. The VVV Templates Project, 249 The high resolution pixelated CZT detectors for the MIRAX Mission, 496 Braga-Ribas, F. Molecular hydrogen and [Fe II] in active galactic nuclei - III. Low-ionization nuclear Improvement of TNO’s Ephemerides in the context of stellar occultations, 199 Braga-Ribas, F. emission-line region and star-forming , 435 Precise stellar occultation predictions for 39 selected TNOs/Centaurs, 33 519 Braga-Ribas, F. Stellar Occultations by Transneptunian Bundy, K. and Centaurs Objects: results from more than 10 CFHT/MegaCam Stripe-82 Survey, 462 Bundy, K. The CFHT/MegaCam Stripe-82 Survey, 160 observed events, 29 Braga-Ribas, F. Stellar occultations by trans-Neptunian Burkhart, B. New Avenues for Measuring Magnetized objects, 224 Turbulence in the Multiphase Interstellar Medium, Braga-Ribas, F. Study of Pluto’s atmosphere from 339 Bussmann, S. Herschel-ATLAS and ALMA: I. A z=1.027 stellar occultation, 200 Brandt, C. H. The SOAR Gravitational Arc Survey, 158 Brasil, P. I. O. Einstein Ring of Molecular Gas and Dust, 139 Bustamante, S. A dynamical mechanism to produce high-inclinations TNOs, 39 Butterley, T. as a dream, 502 tory, 493 they come from?, 34 Cánovas, H. The Behavior of Regular Satellites during NaCo view, 30 Physical properties of galaxies in the Sloan Córsico, A. H. Digital Sky Survey detected in infrared, 379 45 interferometry: diameters, distances, circumstellar Cúneo, V. envelopes and binarity, 254 Cañada-Assandri, M. Nebulae: CNO Nucleosynthesis in Massive Stars, 99 The Latin American Journal of As- Cabrera, J. Caceres, C. Towards understanding the late evolution Briceño, C. A Spectro-photometric study if the young of protoplanetary disks, 228 stellar cluster sigma Orionis., 328 Caetano, T. C. Estimating metallicities with isochrone Briceño, C. Diversity of protoplanetary disks in stellar fits done by global optimization to photometric data clusters: the case of the sigma Orionis cluster, 12 of open clusters, 56 Astronomy and the interdisciplinary under- Caetano, T. C. graduation formation, 499 catalogue, 298 globular clusters and the evolution of their host Caiafa, C. F. galaxy, 364 Molecular hydrogen and [Fe II] in Caicedo Ortiz, H. E. The internal density structure of Giant HII Regions, 102 emission-line region and star-forming , 435 Calanog, J. A. Herschel-ATLAS and ALMA: I. A z=1.027 How do Brightest Cluster and Group Einstein Ring of Molecular Gas and Dust, 139 galaxies grow? Observations vs Models, 106 Calderón, R. Bruch, A. IOAA 2012: The first scientific international Calderón, R. Two-dimensional kinematics of the central LAGO Project , 485 field spectrocopy, 421 Calderón Espinoza, D. TP-AGB stars and population synthesis Buccino, A. CALIFA Collaboration CALIFA: The local extragalactic Observational Results using BTFi, 177 universe unveiled (survey status), 120 Stelar Activity in stars with planets from CALIFA Collaboration Integral Field Unit spectroscopy CASLEO spectra, 287 Bufano, F. Analysis of the Velocity Data of Cluster A562, 361 models, 113 BTFI Team Simulation of Water Cerenkov Detector for detection of cosmic rays Using GEANT4 for the region of NGC4501 from Gemini/GMOS integral Bruzual, G. Analysis and validation of data in the search for GRB, 486 olympiad in Brasil, opening doors for 2016 , 190 Brum, C. A new catatalogue of H I supershell candidates in the outer part of the Milky Way, 95 active galactic nuclei - III. Low-ionization nuclear Brough, S. Proper motion determination of the optically visible open clusters based on the UCAC4 The connection between the origins of Brotherton, M. S. Detectability of Habitable Planets around Very Low-Mass Stars, 36 perspectives, 191 Brodie, J. P. V-type asteroids among the Mars crosser population, 220 tronomy Education (RELEA): contributions and Britto, T. Transit Timing Variations analysis in exoplanet host stars, 230 The Carbon Content in Galactic Ring Bretones, P. S. Asteroseismology of massive pulsating DA white dwarf stars with fully evolutionary models, Classical Cepheids from long-baseline Bresolin, F. Imaging polarimetry of the potentially planet-forming circumstellar disk HD 142527. The the Nice Model’s Planetary Close Encounters, 215 Breitfelder, J. Surface Layer turbulence profiling with the SL-SLODAR and LUSCI at ESO Paranal Observa- Brasser, R. Large Semimajor Axis Centaurs: where do Braz, F. J. The Local Group in a explicit cosmological context, 153 Brasil, P. I. O. Mostra Astronômica: building the reality Brasser, R. Measuring galaxy morphologies in the of supernova host galaxies, 74 Unveiling Type IIb Supernova Progenitors, Calil, M. R. 244 “Planetário e Teatro Digital Johannes Kepler” and its Institutional Pedagogical Project, 185 520 Calipo, F. “Planetário e Teatro Digital Johannes Kepler” Cappa, C. E. and its Institutional Pedagogical Project, 185 infrared dust bubble S 24, 97 Callegari Jr., N. Rotation of Multi-layered Super-Earths, Cappa, C. E. 196 Caproni, A. Systems Close to Mean-motion Commensurabilities, Parsec-scale Activity in BL Lacertae: Signature of Relativistic Jet Precession, 146 Caproni, A. 219 Calvão, M. O. The Type Ia Supernova Pipeline for hydrodynamical simulations, 112 Carballo-Bello, J. A. Astrophysical Survey (J-PAS), 466 A Spectro-photometric study if the young Globular clusters as tracers of the hierarchical formation of the Milky Way, 156 Carciofi, A. C. stellar cluster sigma Orionis., 328 Diversity of protoplanetary disks in stellar Envelopes of Evolved Stars: Galactic and Magellanic Clouds B[e] Supergiants, 276 Carciofi, A. C. clusters: the case of the sigma Orionis cluster, 12 Camacho, H. O. The effects of dark matter halo on the mass loss process in dwarf galaxies: results from 3D the Javalambre Physics of the Accelerating Universe Calvet, N. Millimeter and Far-IR observations of the IRDC G341.24-0.27, 87 Callegari Jr., N. Spin-Orbit Resonances in Super-Earth Calvet, N. Gas, dust and star formation in the Cosmology from the Angular Corre- The Be star Achernar and its circumstellar environement, 52 Carciofi, A. C. V/R variations in Be shell stars, 253 Camacho, H. O. Improving the Modeling and Cosmo- Carciofi, A. C. Viscous Disks in Be Stars, 51 logical Constraints of the Galaxy Angular Correlation Cardaci, M. V. lation Function and Galaxy Clusters , 154 Function, 448 evolution and stellar population of galaxy pairs, 398 Camargo, J. I. B. Astrometric positions for the irregular Cardoso, L. Improving INPE’s balloon ground facilities satellites of Jupiter, Saturn and Neptune, 206 for operation of the protoMIRAX experiment, 494 Camargo, J. I. B. Improvement of TNO’s Ephemerides Cardoso, P. Improving INPE’s balloon ground facilities in the context of stellar occultations, 199 for operation of the protoMIRAX experiment, 494 Camargo, J. I. B. Precise stellar occultation predictions Cardoso dos Santos, J. for 39 selected TNOs/Centaurs, 33 Camargo, J. I. B. a circular orbit, 197 Stellar Occultations by Transneptu- Caretta, C. A. 10 observed events, 29 objects, 224 Caretta, C. A. Study of Pluto’s atmosphere from New Catalogues of Superclusters of The red sequence of Abell X-ray underluminous clusters, 468 Carigi, L. A Systematic Study of the NFW and Carbon and Oxygen Abundances from Recombination Lines in Low Metallicity HII Regions, SIS Elliptical Lensing Models in the Strong Regime, 159 101 Caminha, G. B. Carlos, M. G. C. C. Dynamical Analyses of z= 0.3, 0.5 Galaxy Clusters from the SOAR Gravitational Arcs Detailed differential chemical analysis of a poor metal star: new evidences about Survey, 363 Caminha, G. B. planet formation, 245 Carneiro, C. M. 3D Modelling of the Bipolar Planetary The SOAR Gravitational Arc Survey, 158 Nebula NGC 2346, 340 Campbell, R. Probing accretion on the high-magnetized Carneiro, C. M. polar RX J1007.5-2017, 312 Carollo, D. The formation of stellar haloes of massive the universe, 157 Canalle, J. B. G. Spirals in hierarchical scenario, 111 Carrasco, E. R. IOAA 2012: The first scientific international olympiad in Brasil, opening doors for A Candidate Globular Cluster Behind the Milk Way?, 319 Carrasco, E. R. GeMS/GSAOI: from commissioning to 2016 , 190 The GalileoMobile Project, 189 Candelaresi, S. Andromeda’s interplay with its dwarf companions, 116 Campusano, L. E. Huge-LQG- the largest structure in operations and science results, 180 Carrasco, E. R. Physical conditions and kinematics of The GalileoMobile Project, 189 Candlish, G. N. Phase Mixing in Popping Star Clusters, an HII galaxy with extraordinary dense nucleus: Mrk 296 Capote, E. Caretta, C. A. Abell/ACO Galaxy Clusters up to z ⇠ 0.15, 450 stellar occultation, 200 Canas, L. Central Dominant Galaxies and the evolution of their host Galaxy Clusters, 449 Camargo, J. I. B. Stellar occultations by trans-Neptunian Caminha, G. B. Stable low-altitude orbits around Ganymede considering a disturbing body in nian and Centaurs Objects: results from more than Camargo, J. I. B. Effects of interaction in chemical 996, 404 Carrasco, E. R. VVV Survey search for distant Cepheids in the inner Milky Way, 286 Star formation outside the Elliptical Galaxy NGC2865, 137 521 Carruba, V. Catelan, M. Identification of families halos in a multi-domain space composed by proper elements, Near-IR Period-Luminosity relations for variable stars in omega Centauri, 268 Catelan, M. Reddening-Free Indices in the VISTA Filter 208 Carvalho, E. A. Probing the Spacial Distribution of System, 80 the Near-infrared Stellar Population in Starburst Catelan, M. The VVV Templates Project, 249 Galaxies, 367 Catelan, M. The general catalog of VISTA variables in Carvalho, J. P. S. Stable low-altitude orbits around the Via Lactea, 70 Catelan, M. Ganymede considering a disturbing body in a circular orbit, 197 Carvalho, M. Clusters Found in the Vista Variables in the Via Internal kinematics of HII galaxies, 362 Lactea (VVV) Survey, 303 Carvano, J. M. Asteroids Atiras: study of stability and Catelan, M. Variable stars in the VVV globular clusters, dynamical analysis of the region , 218 Carvano, J. M. 68 Cavichia, O. Evolution models for spiral and irregular Dynamical evolution of differentiated asteroid families, 211 Carvano, J. M. Using MASSCLEAN to Describe Stellar galaxies, 108 Cavichia, O. Finding minor Bodies with the JPAS/J-PLUS photometric surveys, 229 Planetary nebulae near the Galactic centre: chemical abundances , 43 Carvano, J. M. IOAA 2012: The first scientific interna- Cecatto, J. R. Characterization and search for period- tional olympiad in Brasil, opening doors for 2016 , icities on coronal mass ejections (CME) occurrence, 190 246 Carvano, J. M. Ceccarelli, L. Low surface brightness galaxies and void Mapping the early distribution of volatiles in the Main Belt with the JPAS/J-PLUS walls, 375 Cechura, J. Radiation-hydrodynamic Model of High-Mass photometric survey, 38 Carvano, J. M. Photometry and Spectroscopy of X-ray Binaries, 474 Cellone, S. A. Asteroids Rich in Volatils of the Type Main Belt Comets (MBC), 221 Carvano, J. M. bands i ’ and r’, 441 Shape effects on the spectra of Cellone, S. A. asteroids, 207 Carvano, J. M. The IMPACTON project: rotational variability on different types of Blazars, 147 V-type asteroids among the Mars Physical properties of galaxies in the Sloan Digital Sky Survey detected in infrared, 379 Cerqueira, A. H. crosser population, 220 Casas-Miranda, R. A. Contrast density and mass func- 3D Simulations of the Beehive Proplyd, 321 Cerqueira, A. H. tion for spherical collapse of Lemaitre-Tolman-Bondi Steady-state Accretion Disk Models With Variable Alpha, 326 metric since fractal point of view., 163 Casas-Miranda, R. A. The incidence of short time scale Cendron, M. M. properties of NEAs, 222 Carvano, J. M. Characterization blazars environment PG1553 +113 and 3C66A from GMOS data in the Chacón-Cardona, C. A. Multi-fractal and lacunarity Contrast density and mass spectrum analysis of the galaxy distribution in the function for spherical collapse of Lemaitre-Tolman-Bondi SDSS 9th data release, 162 metric since fractal point of view., 163 Casassus, S. Chacón-Cardona, C. A. Imaging polarimetry of the potentially planet-forming circumstellar disk HD 142527. The NaCo view, 30 SDSS 9th data release, 162 Cassetti, J. A new method to disentangle the rotational Chanamé J. Chaparro, G. velocities of stars: application to main-sequence field Stars, 251 Formation Models of Cometary Ices in Chapman, S. C. First spatially-resolved observations of The internal density structure of Giant HII Regions, 102 Castilho, C. M. ionized gas in submillimeter-selected high-redshift Decay of the magnetic field in black starbursts, 118 Char, F. widow pulsars, 473 The WFCAM Variable Star Catalog and Surface Layer turbulence profiling with the SL-SLODAR and LUSCI at ESO Paranal Observatory, New Variability index, 66 Catelan, M. Star clusters in an infalling galaxy, 42 Protoplanetary Disks, 93 Castañeda, H. O. Catelan, C. Multi-fractal and lacunarity spectrum analysis of the galaxy distribution in the 493 Charbonnier, A. Comparison of optical/near-infrared light-curve properties of the Cepheid Instability Measuring galaxy morphologies in the CFHT/MegaCam Stripe-82 Survey, 462 Charbonnier, A. Strip pulsating variables, 258 vey, 160 522 The CFHT/MegaCam Stripe-82 Sur- Chauvin, G. Cieslinski, D. Revisiting TW Hydrae in light of new astrometric data, 315 MLS110213:022733+130617: A new eclipsing polar above the period gap, 46 Chavarria, C. A photometric study of M67: anchoring Cieslinski, D. Modeling photometric and spectroscopic measurements for the determination of astrophysical data of HS 2231+2441: an HW Vir type system with parameters of bright stars, 63 Chené, A.-N. a brown dwarf companion, 57 Cieslinski, D. Probing accretion on the high-magnetized Photometric analisys of Galactic Stellar Clusters in VVV Survey, 307 Chesneau, O. polar RX J1007.5-2017, 312 Clariá, J. J. Overview of Stellar Interferometry and its contribution to the study of massive stars, 73 Chies-Santos, A. of the Large Magellanic Cloud, 41 Clements, D. Herschel-ATLAS and ALMA: I. A z=1.027 Emission line imaging survey of the Abell 901/902 supercluster, 130 Chies-Santos, A. Einstein Ring of Molecular Gas and Dust, 139 Clocchiatti, A. The connection between the origins of globular clusters and the evolution of their host Clowes, R. G. New Catalogues of Superclusters of Coccato, L. A new method to disentangle the rota- galaxy, 364 Coelho, B. field Stars, 251 Dynamical Analyses of z= 0.3, 0.5 Galaxy Coelho, P. 363 Coenda, V. The SOAR Gravitational Arc Survey, 158 Cichowolski, S. Backsplash Galaxies, 128 Coenda, V. Comparing galaxy populations in compact A new catatalogue of H I supershell candidates in the outer part of the Milky Way, 95 and loose groups of galaxies, 119 Cohen, R. E. G126.1–0.8–14: A molecular shell related to Sh2-187, 341 Near-Infrared Photometric Parameters of Galactic Globular Clusters From the VVV Survey, On the origin of the wind variability of 55 81 Cohen, R. E. Cyg, 247 Cidale, L. A new library of theoretical stellar spectra for stellar population applications, 54 Cichowolski, S. Cidale, L. The SDSS quasars as a testbench for the Gaia fundamental reference frame grid-points, 422 Clusters from the SOAR Gravitational Arcs Survey, Cibirka, N. The connection between the origins of globular clusters and the evolution of their host tional velocities of stars:application to main-sequence Cibirka, N. Huge-LQG- the largest structure in the universe, 157 Abell/ACO Galaxy Clusters up to z ⇠ 0.15, 450 Christen, A. A new method to estimate distances to Type II SNe, 451 galaxy, 364 Chow, M. A study of the recent chemical evolution Overview of Stellar Interferometry and its Colas, F. contribution to the study of massive stars, 73 Cidale, L. Supergiants, Stellar Winds and Mass-loss, 6 Cid Fernandes, R. Coldwell, G. MagAl: A new tool to analise Mapping dust-obscured light in Survey, 409 Collao, F. Physical properties of galaxies in GeMS/GSAOI: from commissioning to operations and science results, 180 Collazo, D. the Sloan Digital Sky Survey detected in infrared, 379 Observación de objetos cercanos a la Tierra (Observation of Neos), 214 Cid Fernandes, R. Condori, C. A. H. The Study of Physical Parameters of Resolving galaxies in time and space: Applying STARLIGHT to CALIFA data cubes, Unclassified Stars with the B[e] Phenomenon, 248 Contreras, M. 369 Cid Fernandes, R. SFH of galaxies using spectroscopy Contreras, M. ultraviolet photometry of the GALEX mission, 383 Cid Fernandes, R. Diversity of protoplanetary disks in stellar clusters: the case of the sigma Orionis cluster, The evolution of galaxies between 12 Contreras, R. Near-IR Period-Luminosity relations for 0.05 < z < 0.8, 365 Cid Fernandes, R. A Spectro-photometric study if the young stellar cluster sigma Orionis., 328 in the optical range of the CALIFA sample and The star formation history of variable stars in omega Centauri, 268 Contreras, R. galaxies in the CALIFA survey, 16 Cieslinski, D. Confirmation of a cluster of galaxies hidden behind the Galactic bulge using the VVV CALIFA galaxies, 122 Cid Fernandes, R. Study of Pluto’s atmosphere from stellar occultation, 200 galaxies photometric data, 402 Cid Fernandes, R. Photometric analisys of Galactic Stellar Clusters in VVV Survey, 307 High-ionization accretion signatures in Variable stars in the VVV globular clusters, 68 Contreras, S. Subhalo abundance matching in different compact binary candidates from SOAR Telescope observations, 269 Semi Analytic Models, 410 Contreras Ramos, R. The VVV Templates Project, 249 523 Cooray, A. CSI2264 Team Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 Copetti, M. V. F. stellar objects in NGC 2264, 85 CSI2264 Team Multiwavelength study of the young stellar cluster [DBS2003]156, 351 Copetti, M. V. F. Observational diagnostics of young The inner disks of classical T Tauri stars in NGC 2264, 331 Spatial variations of physical and CSP team Spectral analysis of type II Supernovae, 171 chemical properties of the planetary nebulae Cuadra, J. Gas dynamics in the Galactic Centre: clump accretion and outflows, 145 NGC 6302 and NGC 2440, 352 Copetti, M. V. F. Cuartas-Restrepo, P. Spectroscopic studies of two supernova remnants in the Large Magellanic Cloud, evolution of terrestrial exoplanets in the habitable 349 zone of dwarf stars, 37 Cora, S. A physical model for AGN feedback: the role Cuevas, H. of BH spin and magnetic field , 443 Cora, S. Tidal, thermal and magnetic Galaxy Concentration Index in Low X-ray Luminosity Galaxy Clusters, 366 Cuevas, H. Submillimeter Galaxy Number Counts in a Semi-analytic Model: the Count Matching Approach, The red cluster sequence in low X-ray luminosity galaxy clusters, 458 Cunha, K. 386 Corradi, W. J. B. Spectroscopy of the open cluster Sample of M dwarfs Hosting Planets, 281 Curé, M. remnant candidate ESO429-SC02, 292 Cortés-Serrano, F. Potential-Density Pairs for Thin A new method to disentangle the rotational velocities of stars: application to main-sequence Disks and Spheroidal Haloes I: Expansion in Chevi- field Stars, 251 Curé, M. Fast and slow radiation-driven wind solutions shev Type I Polinomials, 411 Cortesi, A. Stellar Parameters and Metallicities of a The connection between the origins of using ZEUS-3D, 239 globular clusters and the evolution of their host Curé, M. Mass loss from massive stars, 291 galaxy, 364 Curé, M. On the origin of the wind variability of 55 Corti, M. A. Primera identificación astrométrica y Cyg, 247 Curé, M. espectrofotométrica de miembros de Bochum 7, 62 Cortijo, C. The star formation history of galaxies in contribution to the study of massive stars, 73 Curé, M. the CALIFA survey, 16 Costa, A. Cypriano, E. Dynamical Analyses of z= 0.3, 0.5 Galaxy eclipsing polar above the period gap, 46 Clusters from the SOAR Gravitational Arcs Survey, Costa, J. E. R. Probing accretion on the high-magnetized 363 polar RX J1007.5-2017, 312 Evolution models for spiral and irregular galaxies, 108 Planetary nebulae near the Galactic D’Amico, F. The hard X-ray telescopes for MIRAX and protoMIRAX, 175 0.05 < z < 0.8, 365 D’Amico, F. How do Brightest Cluster and Group The high resolution pixelated CZT detectors for the MIRAX Mission, 496 galaxies grow? Observations vs Models, 106 D’Avila, V. A. Couto, G. S. Kinematics and excitation of the nuclear Solar astrometry and the heliometer of Rio de Janeiro, 181 spiral in the active galaxy Arp 102B, 423 Dékány, I. Comparison of optical/near-infrared light-curve Physical properties of galaxies in the properties of the Cepheid Instability Strip pulsating Sloan Digital Sky Survey detected in infrared, 379 variables, 258 Young Brown Dwarfs as Giant Exoplanet Dékány, I. Analogs, 32 Cruzado, A. Developments with the hard X-Ray de- 489 Costa-Duarte, M. V. The evolution of galaxies between Cruz, K. The red sequence of Abell X-ray under- tection plane of the protoMIRAX imaging telescope, centre: chemical abundances , 43 Crestani, T. The SOAR Gravitational Arc Survey, 158 Cypriano, E. D’Amico, F. line profiles of NGC3918 and NGC6302, 345 Couch, W. Cypriano, E. luminous clusters, 468 Costa, R. D. D. High dispersion spectra and kinematic Costa, R. D. D. The Multiwavelength Study of OH Megamaser Galaxy IRAS16399-0937, 148 MLS110213:022733+130617: A new Costa, R. D. D. Wind study of B supergiants stars, 241 Curran, R. L. On the sensitivity of extrasolar mass–loss rate ranges: HD 209458b a case study, 316 Costa, J. E. R. Overview of Stellar Interferometry and its Near-IR Period-Luminosity relations for variable stars in omega Centauri, 268 Extensive MultiConfiguration calcula- Dékány, I. tions of oscillator strengths useful for Astrophysics Searches for variability in the Milky Way bulge with the VVV Survey, 69 Applications, 250 Dékány, I. 524 The VVV Templates Project, 249 Dékány, I. Delgado-Inglada, G. The WFCAM Variable Star Catalog and New Variability index, 66 Dékány, I. database, 346 Delgado-Inglada, G. The general catalog of VISTA variables in the Via Lactea, 70 Dékány, I. Del Valle, L. VVV Survey search for distant Cepheids in Gap Formation in Circumbinary AGN Disks, 143 Dékány, I. Variable stars in the VVV globular clusters, del Valle, M. V. 68 A magnetic reconnection model for explaining AGNs and microquasars radiation, 479 Démoulin, P. del Valle, M. V. Runaway massive stars as a new class Recurrent solar coronal jets induced by magnetic emergence, 78 Dúmet-Montoya, H. S. of galactic gamma-ray sources, 170 Demarco, R. A Systematic Study of the NFW and SIS Elliptical Lensing Models in the Strong D’Andrea, C. B. Einstein Ring of Molecular Gas and Dust, 139 Properties of type Ia supernovae White dwarfs in the Javalambre Physics of Determination of Li abundance in Precise stellar occultation predictions for 39 selected TNOs/Centaurs, 33 de Amorim, A. L. Solar type stars of intermediate brightness, 237 Dalla-Costa, L. J. Brazilian Participations in the Inter- Physical properties of galaxies in the Sloan Digital Sky Survey detected in infrared, national Astronomical Search Collaboration, 186 379 Dalle Mese, G. A photometric study of M67: anchoring de Amorim, A. L. measurements for the determination of astrophysical Resolving galaxies in time and space: Applying STARLIGHT to CALIFA data cubes, parameters of bright stars, 63 Dametto, N. Z. Improvement of TNO’s Ephemerides in the context of stellar occultations, 199 Desmars, J. the Accelerating Universe Survey, 259 Dagostino, M.C. 369 de Amorim, A. L. The star formation history of galaxies Probing the Spacial Distribution of in the CALIFA survey, 16 the Near-infrared Stellar Population in Starburst de Anda-Suárez, J. Galaxies, 367 A survey of extended H2 emission Central Dominant Galaxies and the evolution of their host Galaxy Clusters, 449 De Araújo, P. P. toward a sample of massive YSOs, 327 Daminelli, A. Modeling photometric and spectroscopic Galactic Embedded Clusters with 2MASS infrared photometry, 311 de Avellar, M. G. B. data of HS 2231+2441: an HW Vir type system with a brown dwarf companion, 57 Dannerbauer, H. Cosmology from the Angular Correlation Function and Galaxy Clusters , 154 Desmars, J. inside rich galaxy clusters, 470 Daminelli, A. Herschel-ATLAS and ALMA: I. A z=1.027 DES-Brazil consortium Regime, 159 Time lags of the kilohertz quasi-periodic oscillations in the low-mass X-ray Herschel-ATLAS and ALMA: I. A binaries 4U 1608-52 and 4U 1636-53, 167 De Biasi, M. S. z=1.027 Einstein Ring of Molecular Gas and Dust, 139 Alfabetización en Astronomı́a de docentes de Educación Primaria y de Educación Dantas, M. L. The relation between the spectral Secundaria en La Plata, 187 De Biasi, M. S. synthesis of galaxies in the visible region and their UV emission, 368 astrométricos, 310 Davies, R. The Role of AGN Feedback in the Evolution de Carvalho, J. B. of Seyfert Galaxies, 152 The SACY view of the Sco-Cen complex, 90 De Cos, F. J. The SONYC survey: Towards a complete census of brown dwarfs in star forming regions, 86 New algorithm for centroiding in elongated Shack-Hartmann wavefront sensors spots da Costa, L. N. Mapping Triangulum-Andromeda with using artificial neural networks, 179 de Freitas, D. B. Time-dependent nonextensivity aris- the SDSS, 392 da Costa, L. N. The LMC outer disk stellar population ing from the rotational evolution of solar-type stars, in the light of the Dark Energy Survey, 135 da Costa, L. N. Detección de cúmulos abiertos en regiones extensas del cielo usando parámetros Dası́ Espuig, M. The GalileoMobile Project, 189 Dawson, P. Ionization Correction Factors in Planetary Nebulae, 100 the inner Milky Way, 286 Daflon, S. 3MdB: Mexican million models 277 de Gouveia Dal Pino, E. M. The SOAR Gravitational Arc Survey, 158 A magnetic reconnection model for explaining AGNs and microquasars da Silva Neto, D. N. Precise stellar occultation predic- radiation, 479 de Gouveia Dal Pino, E. M. tions for 39 selected TNOs/Centaurs, 33 da Silva Neto, D. N. Study of Pluto’s atmosphere from Acceleration of Cosmic Rays in the FERMI and CTA Era, 165 stellar occultation, 200 525 de Gouveia Dal Pino, E. M. De Zotti, G. Cherenkov Telescope Ar- ray (CTA), 176 Einstein Ring of Molecular Gas and Dust, 139 de Gouveia Dal Pino, E. M. Galaxy evolution-Star for- Dhillon, V. S. Stellar occultation by the trans-Neptunian mation connection: from pc to kpc scales, 138 de Gouveia Dal Pino, E. M. object 2002 KX14, 195 Dias, B. LLAMA Project, 173 de Gouveia Dal Pino, E. M. Relativistic MHD Simulations of Magnetized Jets, 482 modelling, 252 Dias, R. A. reconnection in acceleration zones of microquasars de Gouveia Dal Pino, E. M. star cluster Pismis 24, 299 The role of reconnection done by global optimization to photometric data of diffusion in the gravitational collapse of turbulent open clusters, 56 Dias, W. S. cloud cores, 89 de Graauw, T. Mmtron, 22 solar neighborhood and the Sun: a connection?, 79 type stars of intermediate brightness, 237 from observations at Observatório Pico Dos Dias, Finding ’jumps’ in light curves using 372 Dias, W. S. change-point algorithms, 227 Stellar Parameters and Metallicities of Proper motion determination of the optically visible open clusters based on the UCAC4 a Sample of M dwarfs Hosting Planets, 281 catalogue, 298 de la Reza, R. The SACY view of the Sco-Cen complex, Dias, W. S. 90 The role of the corotation resonance in the secular evolution of disks of spiral galaxies, 124 de la Rosa, I. G. Dias de Oliveira, A. Precise stellar occultation predic- Constraining Galaxy Evolution with Scaling Relations, 105 De Medeiros, J. R. tions for 39 selected TNOs/Centaurs, 33 Dias de Oliveira, A. Study of Pluto’s atmosphere from The WFCAM Variable Star Catalog stellar occultation, 200 and New Variability index, 66 de Mello, D. F. Dicken, D. HST and Spitzer point source and dust lane Metallicity gradients in tidal tails and merging systems, 405 de Mello, D. F. detection in powerful narrow-line radio galaxies, 150 Diggs, S. GeMS/GSAOI: from commissioning to oper- Star formation outside the Elliptical Galaxy NGC2865, 137 de Mello Neto, J. R. T. ations and science results, 180 Dijkstra, M. Rotation effects on the Lyman-alpha line Large-Scale Anisotropies of the Cosmic Rays Detected at the Pierre Auger morphology in distant galaxies, 376 Ding, M. D. Observatory and the Telescope Array, 475 de Oliveira, A. S. Probing accretion on the high-magnetized Searching for cyclical period varia- about the Universe and its origins, 504 de Paula, L. A. Disk-planet interactions, 198 Diniz, M. R. Asteroids Atiras: study of stability and Diniz, M. R. Finding minor Bodies with the Unveling the LINER nature of NGC1052, 425 Diniz, S. I. F. Spectral Synthesis of Star-forming Galax- JPAS/J-PLUS photometric surveys, 229 Mapping the early distribution of ies in the Near-Infrared, 114 Diniz, S. I. F. Unveling the LINER nature of NGC1052, volatiles in the Main Belt with the JPAS/J-PLUS photometric survey, 38 de Souza, C. C. Two-dimensional Kinematics of the Central Region of NGC 2110 , 424 dynamical analysis of the region , 218 De Prá, M. N. Defining our place in the cosmos. Mapping the vision of the brazilian population tions in cataclysmic variable stars, 243 De Prá, M. N. Recurrent solar coronal jets induced by magnetic emergence, 78 Diniz, A. C. S. polar RX J1007.5-2017, 312 de Oliveira, A. S. De Prá, M. N. Mass extinctions, galactic orbits in the Dias, W. S. Open Cluster Radial Velocity determination Determination of Li abundance in Solar de la Reza, R. An psf-fitting pipeline for VVV-ESO: The Dias, W. S. Estimating metallicities with isochrone fits and AGNs, 478 de la Reza, R. Self-consistent physical parameters for 5 intermediate-age SMC stellar clusters from CMD de Gouveia Dal Pino, E. M. The role of fast magnetic de la Luz, V. Herschel-ATLAS and ALMA: I. A z=1.027 425 Di Rocco, H. O. Checking the consistency of physical Extensive MultiConfiguration calcu- parameters of open clusters: the case of NGC188 lations of oscillator strengths useful for Astrophysics and M67, 297 Applications, 250 de Souza, R. Spectral Synthesis of Star-forming Galax- Domı́nguez, M. ies in the Near-Infrared, 114 De Vito, M. A. Sagittarius dwarf galaxy population from the VVV behind the galactic bulge, 417 Domiciano de Souza, A. Decay of the magnetic field in black widow pulsars, 473 Envelopes of Evolved Stars: Galactic and Magellanic Clouds B[e] Supergiants, 276 526 Domiciano de Souza, A. The Be star Achernar and its Dumas, C. circumstellar environement, 52 Domingos, R. C. occultation, 200 Dunne, L. Identification of families halos in a multi-domain space composed by proper elements, Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 Dupke, R. A. 208 Dominguez, H. Survey, 409 Duplancic, F. Sources, 472 Duronea, N. U. GeMS/GSAOI: from commissioning to Dors, O. L. AM2217-490: Uma galáxia com anel polar Dors, O. L. Effects of interaction in chemical evolution Eales, S. Molecular hydrogen and [Fe II] in Ederoclite, A. White dwarfs in the Javalambre Physics emission-line region and star-forming , 435 of the Accelerating Universe Survey, 259 The effects of the interaction on the Eigenthaler, P. Probing the assembly of galaxy groups kinematics and abundance of AM 2229-735, 374 with intragroup light, 127 The IMPACTON project: rotational Elitzur, M. properties of NEAs, 222 A Point of View from Dust Geometric Distribution, early phases in grand-design, spiral galaxies, 370 430 Dottori, H. Discriminating Local Group embedded star Elliott, J. clusters from older ones using near-IR photometric indexes, 313 the context of the full sample, 169 Emerson, J. The wide view of the Bulge from the VVV training teachers and scientific dissemination at the survey, 123 South of Brazil, 509 Emilio, M. Dougados, C. Modeling the circumstellar environment An study of v sin i distribution of Be stars, 279 of AB Aur using the Halpha line, 325 Emilio, M. Two-dimensional Stellar Kinematics Finding ’jumps’ in light curves using change-point algorithms, 227 and Dynamical Models for NGC 4258 and NGC 1052, Eracleous, M. 371 Correlating X-rays, UV and optical emission from the accretion disk in the nucleus of A kinematic study of the Lupus NGC1097, 439 star-forming region, 53 Proper motions of pre-main sequence Erben, T. Revisiting TW Hydrae in light of new Erben, T. Measuring galaxy morphologies in the CFHT/MegaCam Stripe-82 Survey, 462 stars, 300 Ducourant, C. Mass and energy of GRB-SN events: multi-wavelength analysis of three associations in Dottori, H. OEI, GTTP and Adventurers of the Universe: Ducourant, C. AGN torus properties with WISE, 149 Elitzur, M. Evolutionary Sequence for Seyfert Galaxies: Detection and modelling of star cluster Ducourant, C. Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 active galactic nuclei - III. Low-ionization nuclear Drehmer, D. A. Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 and stellar population of galaxy pairs, 398 Dottori, H. Abundâncias de Zinco em estrelas do bojo Galáctico, 278 Dye, S. em formação, 396 Dos Santos, E. Gas, dust and star formation in the infrared dust bubble S 24, 97 Dutra, N. operations and science results, 180 Dors, O. L. Triplets of galaxies: A connection with compact groups?, 412 stellar occultation, 200 Dors, O. L. Confirmation of a cluster of galaxies hidden behind the Galactic bulge using the VVV Constraints on the First Ionizing Doressoundiram, A. Study of Pluto’s atmosphere from Dorgeville, C. Highlights on Cas-like stars, 481 Duplancic, F. Constraining Galaxy Evolution with Scaling Relations, 105 Dominguez, M. The CFHT/MegaCam Stripe-82 Survey, 160 Escala, A. Gap Formation in Circumbinary AGN Disks, astrometric data, 315 143 Duffard, R. Stellar occultation by the trans-Neptunian Escolano, C. object 2002 KX14, 195 V/R variations in Be shell stars, 253 Espailat, C. A Spectro-photometric study if the young Dufour, P. Accretion and Activity on the PostCommon- stellar cluster sigma Orionis., 328 Envelope Binary RR Cae, 272 Duha, J. Study of Pluto’s atmosphere from stellar Espaillat, C. Diversity of protoplanetary disks in stellar Small asteroid fragments in earth-crossing clusters: the case of the sigma Orionis cluster, 12 orbits, 201 Espinoza, L. Dultzin, D. Evolutionary Sequence for Seyfert Galaxies: Study of Pluto’s atmosphere from stellar occultation, 200 A Point of View from Dust Geometric Distribution, Esteban, C. Carbon abundances in the disk of NGC300 430 from faint CII recombination lines, 355 527 Esteban, C. Faria, R. Z. Carbon and Oxygen Abundances from Recombination Lines in Low Metallicity HII Regions, Kepler” and its Institutional Pedagogical Project, 185 Feitosa, J. A. 101 Esteban, C. The Carbon Content in Galactic Ring Fellhauer, M. The SOAR Gravitational Arc Survey, 158 Faúndez-Abans, M. Fellhauer, M. Ferle, O. L. anel polar em formação, 396 373 Galáxias com Anel Polar, 359 Fernadez Lajus, E. NIP of Stars: early results and new The effects of the interaction on eclipsing binaries , 304 the kinematics and abundance of AM 2229-735, 374 Fabregat, J. Fernandes, B. A long-term study of the Be star Mu Fernandes, J. O. Improving INPE’s balloon ground fa- Gravitational waves and stability of cilities for operation of the protoMIRAX experiment, cosmological solutions in the Modified Starobinsky 494 inflation, 461 Fernandes, M. C. Large-Scale Anisotropies of the Cos- Two rings but no fellowship: LoTr 1 and mic Rays Detected at the Pierre Auger Observatory its relation to planetary nebulae possessing Barium and the Telescope Array, 475 central stars, 49 Fernandes, R. C. The mass–metallicity–star formation Faes, D. M. The Be star Achernar and its circumstellar rate relation under the STARLIGHT microscope, 401 environement, 52 Ferrari, F. Fagundes, A. L. Evaluation of Learning of Synchronous Ferraz-Mello, S. Creep tides. A new model to study the Resource, 501 tidal evolution of close-in satellites and exoplanets, The GALEX Nearby Young-Star Survey, 28 64 Ferreira, A. C. S. Proper motions of pre-main sequence Faherty, J. K. Young Brown Dwarfs as Giant Exoplanet stars, 300 Analogs, 32 Falcón, N. Ferreira, I. S. Fotometrı́a de la luz cenicienta y albedo Ferreira Lopes, C. E. atmosférico local, 495 Ferreiro, D. Spectral Properties of Narrow Line Seyfert MILES library for stellar population modelling , 55 1 galaxies, 433 Relativistic MHD Simulations Ferreras, I. Constraining Galaxy Evolution with Scaling of Magnetized Jets, 482 Relations, 105 Falceta-Gonçalves, D. The effects of dark matter halo Ferrero, G. NIP of Stars: early results and new eclipsing on the mass loss process in dwarf galaxies: results binaries , 304 from 3D hydrodynamical simulations, 112 Ferrero, L. Falco, E. Estimating the size of the emitting region in Fesquet, V. 437 Resolving galaxies in time and Fidêncio, M. Proper motions of pre-main sequence stars, 300 369 Figueira, P. Palaeogeographic reconstruction of Finding proto-spectroscopic binaries: Precise multi-epoch radial velocities of 7 protostars Minchin palaeolake system, South America: the in Ophiuchus, 332 influence of astronomical forcing, 232 Faria, M. A. F. GeMS/GSAOI: from commissioning to operations and science results, 180 space: Applying STARLIGHT to CALIFA data cubes, Fariña, R. A. Transit Timing Variations analysis in exoplanet host stars, 230 the lens quasars HE0047-1756 and SDSS1155+6346, Falcon Barroso, J. The WFCAM Variable Star Catalog and New Variability index, 66 Improvement and analysis of the Falceta-Gonçalves, D. North-South CMB analyses using the Minkowski Functionals, 457 lunar para la determinacion del espesor optico Falcón Barroso, J. Two-dimensional Stellar Kinematics and Dynamical Models for NGC 4258 and NGC 1052, 371 Rotation of the Moon Mediated By Computational Faherty, J. K. The nature of X-ray sources associated to young clusters around Sh2-296, 301 Centauri in the L-band, 236 Fabris, J. C. The Formation of dSph galaxies, 104 Effects of dark matter and energy on the chemical enrichment of Dwarf Spheroidal Galaxies, Dinâmica da Formação de Faúndez-Abans, M. Phase Mixing in Popping Star Clusters, 296 AM2217-490: Uma galáxia com Faúndez-Abans, M. 3D Simulations of the Beehive Proplyd, 321 Nebulae: CNO Nucleosynthesis in Massive Stars, 99 Estrada, J. Faedi, F. “Planetário e Teatro Digital Johannes Filgas, R. Open Cluster Radial Velocity determi- Mass and energy of GRB-SN events: multi-wavelength analysis of three associations in nation from observations at Observatório Pico Dos the context of the full sample, 169 Dias, 372 Fioretto Aguero, N. Use of Mathematica software in the study of planetary dynamics, 202 528 Firpo, V. Deep infrared extinction maps of the Fourth Friaça, A. C. S. Galactic Quadrant based on VVV and GLIMPSE able Zone to the Galactic Habitable Zone, 223 Friaça, A. C. S. Life in the Cosmic Context. An Astrobi- surveys, 342 Firpo, V. Gas, dust and star formation in the infrared ology Course as an Experiment in Transdisciplinarity, dust bubble S 24, 97 184 Firpo, V. Infrared study of new star clusters associated Friaça, A. C. S. to dusty globules, 330 Fleuren, S. evolution marker, 400 Einstein Ring of Molecular Gas and Dust, 139 rich galaxy clusters, 470 Fu, H. Integral Field Unit spectroscopy of supernova host galaxies, 74 Flores, H. Fuentes-Carrera, I. Unveiling the nature of an ultra-luminous and structure of its optical counterpart , 168 Furlanetto, C. The SOAR Gravitational Arc Survey, 158 Stelar Activity in stars with planets from CASLEO spectra, 287 Gómez, A. Abundâncias de Zinco em estrelas do bojo Flores-Durán, S. A kinematic study of different stellar Galáctico, 278 populations in the irregular NGC 6822, 391 Gómez, M. Probing AGN accretion through mi- Gómez, M. F. Spectral analysis of type II Supernovae, Gabbasov, R. Mostra Astronômica: building the Rotation Curve Decomposition of NGC 5278, 395 Accretion and Activity on the Post- Galante, D. CommonEnvelope Binary RR Cae, 272 Forbes, D. the young Sun/solar stellar analogs, 235 globular clusters and the evolution of their host Galaz, G. galaxy, 364 Galaz, G. gigayear of cosmic history, 469 Halo-based reconstruction of line morphology in distant galaxies, 376 The Local Group in a explicit Properties of type Ia supernovae inside rich galaxy clusters, 470 Solar System, 35 Gallenne, A. Forman, W. R. Properties of Galaxies Groups Selected Classical Cepheids from long-baseline interferometry: diameters, distances, circumstellar from Chandra X-ray Observations of the Bootes envelopes and binarity, 254 Fields, 484 Galli, P. A. B. The Janus-Epimetheus Ring, 31 A kinematic study of the Lupus star-forming region, 53 The connection between the origins of Galli, P. A. B. globular clusters and the evolution of their host Proper motions of pre-main sequence stars, 300 galaxy, 364 Galli, P. A. B. Asteroseismology of massive pulsating DA Revisiting TW Hydrae in light of new astrometric data, 315 white dwarf stars with fully evolutionary models, 45 Freitas, C. F. Galbany, L. Gallardo, T. Atlas of the three body resonances in the cosmological context, 153 Fraga, L. Integral Field Unit spectroscopy of supernova host galaxies, 74 Forero-Romero, J. E. Rotation effects on the Lyman-alpha Foster, C. The dense gas in M82, 399 Galbany, L. the cosmic mass density field, 155 Foryta, D. Low surface brightness galaxies and void walls, 375 Forero, J. Super-massive black hole growth in the first Forero-Romero, J. E. The BIOSUN project:an astrobiological approach to study the origin of life in the context of The connection between the origins of Forero-Romero, J. E. Disk Mass-to-light Ratio Distribution from Stellar Population Synthesis: Application to reality as a dream, 502 Fontaine, G. Super-massive black hole growth in the first gigayear of cosmic history, 469 171 Fonseca, J. E. S. Transit Timing Variations analysis in exoplanet host stars, 230 crolensing, 432 Folatelli, G. Unveiling the nature of an ultra-luminous X-ray source through the kinematics of its optical counterpart , 168 Floyd, D. J. E. Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 X-ray source through the kinematics and structure Flores, M. PAH lines at high redshift as galaxy Frieman, J. A. Properties of type Ia supernovae inside Herschel-ATLAS and ALMA: I. A z=1.027 Flores, H. Connecting the Circumstellar Habit- Galliani, S. Finding new planets around solar twins El Catalogo Bibliografico de Velocidades Radiales, 264 using the HARPS/ESO spectrograph, 203 Gallimore, J. Freitas-Lemes, P. AM2217-490: Uma galáxia com anel The Multiwavelength Study of OH Megamaser Galaxy IRAS16399-0937, 148 polar em formação, 396 Galvez, R. Freitas-Lemes, P. The effects of the interaction on the GeMS/GSAOI: from commissioning to operations and science results, 180 kinematics and abundance of AM 2229-735, 374 Gama, D. 529 A bolha infravermelha N10, 343 GAMA team Galaxy And Mass Assembly (GAMA): The Garcia da Silva, C. connection between metals, specific SFR and H I clusters, 452 Garnavich, P. M. gas in galaxies: the Z-SSFR relation, 109 Gameiro, J. F. Finding proto-spectroscopic binaries: Garrido, F. in Ophiuchus, 332 Garrido, H. E. Emission-line stars in the star-formation A new insight to the O Vz stars within the region NGC 1850, 334 Garzón, A. G126.1–0.8–14: A molecular shell related to Sh2-187, 341 434 Gausachs, G. binaries , 304 OWN Survey: results after seven years of GeMS/GSAOI: from commissioning to operations and science results, 180 Gavignaud, I. high-resolution spectroscopic monitoring of Southern O and WN stars, 72 Gansicke, B. T. Diagnostic diagrams with polycyclic aromatic hydrocarbons in diferent types of galaxies, Gamen, R. NIP of Stars: early results and new eclipsing Gamen, R. A physical model for AGN feedback: the role of BH spin and magnetic field , 443 framework of the GOSS Survey, 71 Gamen, R. Properties of type Ia supernovae inside rich galaxy clusters, 470 Precise multi-epoch radial velocities of 7 protostars Gamen, R. J-PAS: Cosmology with galaxy Integral Field Spectroscopy SINFONI observation of AGN at z ⇠ 1.6, 445 White dwarf-main sequence binaries Gawiser, E. Submillimeter Galaxy Number Counts in a from SDSS DR8: unveiling the cool white dwarf Semi-analytic Model: the Count Matching Approach, population, 318 386 Garavito-Camargo, N. Rotation effects on the Lyman-alpha line morphology in distant galaxies, 376 Garcı́a, F. Geisler, D. Magnetic field evolution and jet formation A study of the recent chemical evolution of the Large Magellanic Cloud, 41 Geisler, D. A kinematic study of different stellar populations in the irregular NGC 6822, 391 Garcı́a-Rojas, J. The SONYC survey: Towards a complete census of brown dwarfs in star forming regions, 86 in accreting neutron stars, 476 Garcı́a-Rojas, J. Geers, V. C. Near-Infrared Photometric Parameters of Galactic Globular Clusters From the VVV Survey, 81 Geisler, D. Carbon abundances in the disk of Photometric analisys of Galactic Stellar Clusters in VVV Survey, 307 NGC300 from faint CII recombination lines, 355 Garcı́a-Rojas, J. Carbon and Oxygen Abundances from Geisler, D. Recombination Lines in Low Metallicity HII Regions, The Origin and Chemical Evolution of the Exotic Globular Cluster NGC 3201, 309 Georgiev, L. 101 Garcı́a-Rojas, J. The Carbon Content in Galactic Ring Nebulae: CNO Nucleosynthesis in Massive Stars, 99 Garcı́a-Varela, A. The Discrepant Kinematics of ORLs and CELs in NGC 7009 as a Function of Ionization Structure, 356 Germanà, C. A Study on the Universality and High-frequency quasi-periodic oscilla- Linearity of the Leavitt Law in the LMC and SMC tions in X-ray binaries: clues from their amplitude Galaxies, 255 and coherence, 256 Garcı́a-Varela, A. Search for Southern Galactic Be star Ghezzi, L. candidates, 50 Garcı́a Benito, R. Resolving galaxies in time and space: Giacani, E. Applying STARLIGHT to CALIFA data cubes, 369 Garcı́a Benito, R. Stellar Parameters and Metallicities of a Sample of M dwarfs Hosting Planets, 281 Study of triggered star formation in a bright-rimmed cloud, 322 Giaccari, U. SFH of galaxies using spectroscopy Large-Scale Anisotropies of the Cosmic in the optical range of the CALIFA sample and Rays Detected at the Pierre Auger Observatory and ultraviolet photometry of the GALEX mission, 383 the Telescope Array, 475 Garcı́a Benito, R. The star formation history of galaxies Gianninas, A. in the CALIFA survey, 16 Garcı́a Lambas, D. Low surface brightness galaxies and void walls, 375 Garcı́a Lambas, D. The red cluster sequence in low IFU spectroscopic analysis of M81, 426 Gibson, B. K. Phase Mixing in Popping Star Clusters, Gieren, W. Triplets of galaxies: A connection Classical Cepheids from long-baseline interferometry: diameters, distances, circumstellar with compact groups?, 412 envelopes and binarity, 254 Garcia, C. M. Construction of a radiotelescope, 497 Garcia, G. Giansante, L. 296 X-ray luminosity galaxy clusters, 458 Garcı́a Lambas, D. Accretion and Activity on the Post- CommonEnvelope Binary RR Cae, 272 Gil-Hutton, R. A photometric study of M67: anchoring Asteroids in the quasi-Hilda comet group, 204 Gil-Hutton, R. measurements for the determination of astrophysical parameters of bright stars, 63 V-type asteroids among the Mars crosser population, 220 530 Giménez de Castro, G. LLAMA Project, 173 Giovanni, P. E. Gonçalves, D. R. Chromospheric and Coronal Activity Physics of the Accelerating Universe Survey, 259 Gonçalves, T. S. First spatially-resolved observations of in Stars Before the Main Sequence, 333 Girard, J. H. Study of Pluto’s atmosphere from stellar ionized gas in submillimeter-selected high-redshift occultation, 200 starbursts, 118 Girardi, L. Mapping Triangulum-Andromeda with the Gonçalves, T. S. SDSS, 392 Girardi, L. Lyman-Break Galaxies, 389 Gonçalves, T. S. the light of the Dark Energy Survey, 135 Contrasting distances using Type Ia super- Quenching Star Formation Now and Then: Downsizing of the Mass Flux Density in the novae and gamma ray events in the local universe, Green Valley, 107 Gonçalves, T. S. 453 Giron, J. Low-redshift compact UV luminous starbursts: a door to understand high-redshift The LMC outer disk stellar population in Girola, R. White dwarfs in the Javalambre Astronomy and the interdisciplinary under- González, D. Advances in the astronomical site testing graduation formation, 499 Giuliatti Winter, S. M. Dust production of the small in Colombia, 490 González, F. satellites immersed in the arcs/ring of Saturn, 205 Giuliatti Winter, S. M. The Evolution of the G Ring González, G. A. Potential-Density Pairs for Thin Disks and the Solar Radiation Force, 212 and Spheroidal Haloes I: Expansion in Chevishev The Janus-Epimetheus Ring, Type I Polinomials, 411 González, G. A. Potential-Density Pairs for Thin Disks 31 Gledhill, T. M. Imaging polarimetry of the potentially and Spheroidal Haloes II: Expansion in Chevishev planet-forming circumstellar disk HD 142527. The Type II Polynomials, 414 González, G. A. Potential-Density Pairs for Thin Disks NaCo view, 30 Gnedin, N. The MW and the Local Group mass, 471 Goldes, G. V. and Spheroidal Haloes III: Expansion in Gegenbauer Polynomials, 415 Structure of Bubbles in the South-East González, J. E. region of the Large Magellanic Cloud, 347 Gomes, N. The GalileoMobile Project, 189 Gomes, R. S. Gomes, R. S. Large Semimajor Axis Centaurs: where Distribution, 430 González Avila, C. Gomes, R. S. The Behavior of Regular Satellites during Observatory, 493 González Delgado, R. M. Astronomy and the interdisciplinary undergraduation formation, 499 Resolving galaxies in time and space: Applying STARLIGHT to CALIFA data High-ionization accretion sig- cubes, 369 González Delgado, R. M. natures in compact binary candidates from SOAR Telescope observations, 269 SFH of galaxies using spectroscopy in the optical range of the CALIFA sample Gomes Jr, A. R. Astrometric positions for the irregular and ultraviolet photometry of the GALEX mission, satellites of Jupiter, Saturn and Neptune, 206 383 González Delgado, R. M. Chemical abundances and physical parameters of evolved stars with planets, 288 Gomez, P. Surface Layer turbulence profiling with the SL-SLODAR and LUSCI at ESO Paranal the Nice Model’s Planetary Close Encounters, 215 Gomez, M. Evolutionary Sequence for Seyfert Galaxies: A Point of View from Dust Geometric do they come from?, 34 Gomes da Silva, K. M. Figure of Merit for Dark Energy Parameterizations, 454 González, J. J. A dynamical mechanism to produce high-inclinations TNOs, 39 Gomes, V. Stelar Activity in stars with planets from CASLEO spectra, 287 Arc under the Effects of the Resonance with Mimas Giuliatti Winter, S. M. Secular Evolution in Green Valley Galaxies, 388 The star formation history of galaxies in the CALIFA survey, 16 Analysis of the Velocity Data of Cluster Gonzales, J. Shape effects on the spectra of asteroids, Gonçalves, D. R. 3D Modelling of the Bipolar Planetary Gonzales, J. The IMPACTON project: rotational prop- A562, 361 207 Nebula NGC 2346, 340 erties of NEAs, 222 Gonçalves, D. R. Andromeda’s interplay with its dwarf Gonzalez, O. A. companions, 116 The wide view of the Bulge from the VVV survey, 123 Gonçalves, D. R. Unveiling the nature of an ultra-luminous Gonzalez, R. The MW and the Local Group mass, 471 Gonzalez-Gaitán, S. X-ray source through the kinematics and structure of its optical counterpart , 168 Supernovae, 171 531 Spectral analysis of type II Gonzalez-Gaitán, S. Subluminous type Ia supernovae, Gunthardt, G. 75 eclipsing binaries , 304 Gonzalez Blanco, F. Guo, Y. Developments with the hard X-Ray detection plane of the protoMIRAX imaging Gupta, R. R. The Local Group in a explicit cosmo- Gurovich, S. Sagittarius dwarf galaxy population from The IAU Office of Astronomy for the VVV behind the galactic bulge, 417 Development: Opportunities for Latin America, 188 Gurovich, S. Graham, M. J. Huge-LQG- the largest structure in the data, 377 Searches for variability in the Milky Way 171 Guzmán, D. bulge with the VVV Survey, 69 The VVV Templates Project, 249 Gregorio-Hetem, J. 178 Guzmán, D. On the association of young star using artificial neural networks, 179 Guzmán, D. analysis, 323 Gregorio-Hetem, J. The nature of X-ray sources Guzmán, E. Mass and energy of GRB-SN events: Guzmán, E. Programa de observación de ocultaciones the context of the full sample, 169 de estrellas desde el Observatorio Nacional de Llano Emission line imaging survey of the Abell del Hato, 213 901/902 supercluster, 130 Hägele, G. F. The hard X-ray telescopes for MIRAX Hadrava, P. Radiation-hydrodynamic Model of High-Mass The high resolution pixelated CZT X-ray Binaries, 474 detectors for the MIRAX Mission, 496 Hajdu, G. Comparison of optical/near-infrared light-curve Proper motions and brown dwarfs in properties of the Cepheid Instability Strip pulsating the VVV survey, 83 Gromadzki, M. variables, 258 Weather on Other Worlds: Brown Hales, A. Dwarf variability and VVV, 84 Grosbol, P. NaCo view, 30 Hamuy, M. Grosbol, P. Discriminating Local Group embedded star Hamuy, M. indexes, 313 Hanslmeier, A. The BIOSUN project:an astrobiological Grupe, D. Correlating X-rays, UV and optical emission approach to study the origin of life in the context of from the accretion disk in the nucleus of NGC1097, the young Sun/solar stellar analogs, 235 439 Hanson, M. M. Using MASSCLEAN to Describe Stellar Characterization and search for Clusters Found in the Vista Variables in the Via periodicities on coronal mass ejections (CME) Lactea (VVV) Survey, 303 occurrence, 246 Hao, J. Stellar parameters and metallicity in Huge-LQG- the largest structure in the universe, 157 Contributions of geomorphology for Hartmann, L. the understanding of landscape evolution in rocky Diversity of protoplanetary disks in stellar clusters: the case of the sigma Orionis cluster, planets of the Solar System, 226 Guimarães, M. M. The SOAR Gravitational Arc Survey, 158 Harris, K. A. Orion Association F and G stars, 302 Guerra, A. J. T. Spectral analysis of type II Supernovae, 171 Rotational Properties of A-Type Stars, 257 Guerço, R. F. A new method to estimate distances to Type II SNe, 451 clusters from older ones using near-IR photometric Guedes, M. R. G. Imaging polarimetry of the potentially planet-forming circumstellar disk HD 142527. The Detection and modelling of star cluster early phases in grand-design, spiral galaxies, 370 Grosso, M. Effects of interaction in chemical evolution and stellar population of galaxy pairs, 398 and protoMIRAX, 175 Gromadzki, M. Observación de objetos cercanos a la Tierra (Observation of Neos), 214 multi-wavelength analysis of three associations in Grindlay, J. E. Simulations of atmospheric turbulence with spatiall phase modulators, 487 associated to young clusters around Sh2-296, 301 Grindlay, J. E. New algorithm for centroiding in elongated Shack-Hartmann wavefront sensors spots clusters and their parental clouds: a statistical fractal Grey, M. BOMBOLO: a Multi-Band, Wide-field, Near UV/Optical Imager for the SOAR 4m Telescope, A X-ray view of young star population in CMa R1, 88 Gregorio-Hetem, J. Greiner, J. Visualizing VVV catalogue and image Gutiérrez, C. P. Spectral analysis of type II Supernovae, universe, 157 Gran, F. Properties of type Ia supernovae inside rich galaxy clusters, 470 logical context, 153 Govender, K. Recurrent solar coronal jets induced by magnetic emergence, 78 telescope, 489 Gottloeber, S. Gran, F. NIP of Stars: early results and new 12 Time-series JHK Photometry of Stars in the center of Cygnus OB2, 329 532 Hasselmann, P. H. The IMPACTON project: rotational Hicks, E. properties of NEAs, 222 Haubois, X. The Role of AGN Feedback in the Evolution of Seyfert Galaxies, 152 Hidalgo-Gàmez, A. M. Viscous Disks in Be Stars, 51 Haucke, M. On the origin of the wind variability of 55 SFR in dwarf spiral galaxies, 380 Higuera-G., M. A. Physical parameters of galaxies with Cyg, 247 Heinze, A. Weather on Other Worlds: Brown Dwarf star formation through mid-infrared SED models, variability and VVV, 84 394 Hellmich, S. Stellar occultation by the trans-Neptunian Hildebrandt, H. object 2002 KX14, 195 Hempel, M. the CFHT/MegaCam Stripe-82 Survey, 462 Hildebrandt, H. Confirmation of a cluster of galaxies hidden behind the Galactic bulge using the VVV Hill, V. Survey, 409 Hoffman, Y. The Local Group in a explicit cosmological survey, 123 context, 153 Holhjem, K. Assesing systematics with XSHOOTER data, 438 A nuclear molecular ring in Mrk 1066 Image reduction of multi-chip near-IR data using the THELI pipeline, 491 Hong, J. revealed by PCA tomography, 427 A Spectro-photometric study if the The hard X-ray telescopes for MIRAX and protoMIRAX, 175 Hong, J. young stellar cluster sigma Orionis., 328 Hernández, J. Abundâncias de Zinco em estrelas do bojo Galáctico, 278 Hennawi, J. The Proximity Effect toward z > 3.5 QSOs: Hernández, J. The CFHT/MegaCam Stripe-82 Sur- vey, 160 Hempel, M. The wide view of the Bulge from the VVV Hennig, M. G. Measuring galaxy morphologies in Diversity of protoplanetary disks in The high resolution pixelated CZT detectors for the MIRAX Mission, 496 Hopkins, A. M. stellar clusters: the case of the sigma Orionis cluster, 12 Galaxy And Mass Assembly (GAMA): The connection between metals, specific SFR and H Hernández-Aguayo, C. Central Dominant Galaxies I gas in galaxies: the Z-SSFR relation, 109 Horvath, J. E. and the evolution of their host Galaxy Clusters, 449 Hernández-Martı́nez, L. A kinematic study of different widow pulsars, 473 Horvath, J. E. stellar populations in the irregular NGC 6822, 391 Hernandez-Aguila, B. Determination of Li abundance The BIOSUN project:an astrobiological approach to study the origin of life in the context of in Solar type stars of intermediate brightness, 237 Hernandez-Jimenez, J. A. Decay of the magnetic field in black the young Sun/solar stellar analogs, 235 Horvath, J. E. Photometry and Dynamics The Latin American Journal of As- of the Minor Merger AM 1219-430 with Gemini/GMOS-S, tronomy Education (RELEA): contributions and 378 perspectives, 191 Hernandez-Jimenez, J. A. Probing the Spacial Dis- Horvath, J. E. Time lags of the kilohertz quasi-periodic tribution of the Near-infrared Stellar Population in oscillations in the low-mass X-ray binaries 4U Starburst Galaxies, 367 Herpich, F. R. 1608-52 and 4U 1636-53, 167 Hoyos, J. Physical properties of galaxies in the Sloan Digital Sky Survey detected in infrared, 379 Herrera-Camus, R. Low surface brightness galaxies stars, 37 Hoyos Restrepo, P. and void walls, 375 Herrera-Camus, R. Hetem, A. The dense gas in M82, 399 208 Huang, J.-S. and their parental clouds: a statistical fractal analysis, 323 Chile, 5 Hurley, J. R. The CFHT/MegaCam Stripe-82 Survey, Husemann, B. Photometry of Hot-Jupiters Type Exo- Resolving galaxies in time and space: Applying STARLIGHT to CALIFA data cubes, 369 planets in Transiting Systems, 233 Hickel, G. R. Metallicity effects on globular clusters: size and colour, 60 160 Hickel, G. R. A New Chinese Astronomy Center in Hunt-Walker, N. AGN torus properties with WISE, 149 Measuring galaxy morphologies in the CFHT/MegaCam Stripe-82 Survey, 462 Heymans, C. Identification of families halos in a multi-domain space composed by proper elements, On the association of young star clusters Heymans, C. RECA: A network by students, for students, 507 Huaman, M. E. Data Acquisition System for Instructional Spectroscopes, 498 Hetem, A. Tidal, thermal and magnetic evolution of terrestrial exoplanets in the habitable zone of dwarf Ibar, E. The magnetic field and dust properties Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 in the direction of the dark cloud CG12, 344 533 Ibarra Medel, H. J. Jaffé, Y. L. The use of rendering techniques in Galaxy Cluster Finding, 455 Iglesias, D. mental Survey, 129 Janot-Pacheco, E. A New Paradigm for Habitability in Searches for variability in the Milky Way bulge with the VVV Survey, 69 Illiev, I. K. Planetary Systems: the Extremophile Zone, 209 Janot-Pacheco, E. a observations of three globular clusters: NGC 104 NGC 6205 NGC 7099, 58 Janot-Pacheco, E. UV/Optical Imager for the SOAR 4m Telescope, 178 Finding ’jumps’ in light curves using change-point algorithms, 227 Janot-Pacheco, E. Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 Life in the Cosmic Context. An Astrobiology Course as an Experiment in Transdis- Iribarrem, A. The Galaxy Cosmological Mass Function, ciplinarity, 184 Jaque Arancibia, M. 456 Islas-Islas, J. M. Central Dominant Galaxies and the Jasmin, F. L. Confirmation of a cluster of galaxies Jasmin, F. L. V-type asteroids among the Mars crosser Survey, 409 population, 220 Ivanov, V. D. Proper motions and brown dwarfs in the Jatenco-Pereira, V. VVV survey, 83 Alfvén Waves, 324 Jayawardhana, R. occultation, 200 Ivanov, V. D. Using MASSCLEAN to Describe Stellar regions, 86 Jenkins, J. S. Close-in planets around giant stars, 210 Lactea (VVV) Survey, 303 Jincheng, Y. U. Weather on Other Worlds: Brown Dwarf Jofre, E. AGN torus properties with WISE, 149 First spatially-resolved observations of ters of evolved stars with planets, 288 starbursts, 118 host stars, 230 Jones, C. Properties of Galaxies Groups Selected from Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 Chandra X-ray Observations of the Bootes Fields, Morphological analysis of the tail 484 Jones, D. structures of comet 1P/Halley 1910 II, 225 Izotov, Y. I. Metal-Poor Active Galactic Nuclei, 360 Izotov, Y. I. Chemical abundances and physical parame- Jofre, E. Transit Timing Variations analysis in exoplanet ionized gas in submillimeter-selected high-redshift Izaguirre, L. S. Mass segregation for the young star clusters, 305 variability and VVV, 84 Ivison, R. The SONYC survey: Towards a complete census of brown dwarfs in star forming Clusters Found in the Vista Variables in the Via Ivison, R. Increase of Ionization Fraction of Dusty Proto-Stellar Accretion Disks by Damping of Study of Pluto’s atmosphere from stellar Ivanov, V. D. The IMPACTON project: rotational properties of NEAs, 222 hidden behind the Galactic bulge using the VVV Ivanov, V. D. NIP of Stars: early results and new eclipsing binaries , 304 evolution of their host Galaxy Clusters, 449 Ivanov, V. D. Ivezic, Z. An study of v sin i distribution of Be stars, 279 Infante, L. BOMBOLO: a Multi-Band, Wide-field, Near Inohara, A. BUDHIES: a Blind Ultra Deep HI Environ- Two rings but no fellowship: LoTr 1 and its relation to planetary nebulae possessing Barium Physical conditions and kinematics of an central stars, 49 HII galaxy with extraordinary dense nucleus: Mrk Jones, M. I. Close-in planets around giant stars, 210 996, 404 Jordán, A. J-PAS Team Finding minor Bodies with the JPAS/J-PLUS NaCo view, 30 photometric surveys, 229 Jablonski, F. Galaxy Model in Infrared, 393 Jablonski, F. High-ionization accretion signatures in Jordán, A. Joshi, J. Materiais Interativos no Ensino de JPAS Collaboration Multi-band characterization of hot White dwarfs in the Javalambre Physics of the Accelerating Universe Survey, 259 jupiters using OPD data, 27 Junqueira, T. C. The galactic distribution of Fermi point The role of the corotation resonance in the secular evolution of disks of spiral galaxies, sources, 477 Jafelice, L. C. The GalileoMobile Project, 189 Astronomia, 505 observations, 269 Jablonski, F. The VVV Templates Project, 249 Josué, A. M. compact binary candidates from SOAR Telescope Jablonski, F. Imaging polarimetry of the potentially planet-forming circumstellar disk HD 142527. The 124 The Latin American Journal of As- Künzel, R. ALS 2883: Analysis of spectroscopic features, tronomy Education (RELEA): contributions and perspectives, 191 314 534 Kadowaki, L. H. S. Kharb, P. The role of fast magnetic reconnection in acceleration zones of microquasars and maser Galaxy IRAS16399-0937, 148 Khiali, B. A magnetic reconnection model for explain- AGNs, 478 Kafka, S. Accretion and Activity on the PostCommon- ing AGNs and microquasars radiation, 479 Kitamura, J. R. Envelope Binary RR Cae, 272 Kalmus, A. T. Brazilian Participations in the Interna- Klein, V. B. Physical properties of galaxies in the Sloan Formation Models of Cometary Ices in Digital Sky Survey detected in infrared, 379 Klose, S. Protoplanetary Disks, 93 Kanaan, A. BOMBOLO: a Multi-Band, Wide-field, Near the context of the full sample, 169 Kanaan, A. New algorithm for centroiding in elongated Kneib, J.-P. Shack-Hartmann wavefront sensors spots using Kneib, J.-P. Simulations of atmospheric turbulence Kobel, P. extinction with an All Sky camera, 488 population, 318 Kowal, G. the Accelerating Universe Survey, 259 Overview of Stellar Interferometry and its Wind study of B supergiants stars, 241 and CTA Era, 165 Kepler” and its Institutional Pedagogical Project, 185 Jets, 482 Krühler, T. Mass and energy of GRB-SN events: multi-wavelength analysis of three associations in Mass and energy of GRB-SN events: multi-wavelength analysis of three associations in the context of the full sample, 169 the context of the full sample, 169 Krabbe, A. C. The GALEX Nearby Young-Star Survey, 64 Kaufer, A. Acceleration of Cosmic Rays in the FERMI Kowal, G. Relativistic MHD Simulations of Magnetized “Planetário e Teatro Digital Johannes Kastner, J. H. A magnetic reconnection model for explaining AGNs and microquasars radiation, 479 Kowal, G. contribution to the study of massive stars, 73 Kann, D. A. White dwarf-main sequence binaries from SDSS DR8: unveiling the cool white dwarf Kanaan, A. White dwarfs in the Javalambre Physics of Kanashiro, M. The GalileoMobile Project, 189 Koester, D. Star detection and study of atmospheric Kanaan, S. The CFHT/MegaCam Stripe-82 Survey, 160 with spatiall phase modulators, 487 Kanaan, S. Measuring galaxy morphologies in the CFHT/MegaCam Stripe-82 Survey, 462 artificial neural networks, 179 Kanaan, A. Mass and energy of GRB-SN events: multi-wavelength analysis of three associations in UV/Optical Imager for the SOAR 4m Telescope, 178 Kanaan, A. Line Identification in the Sun’s Spectrum, 260 tional Astronomical Search Collaboration, 186 Kamp, I. The Multiwavelength Study of OH Mega- Effects of interaction in chemical evolution and stellar population of galaxy pairs, 398 Krabbe, A. C. Photometry and Dynamics of the Minor ESO: Present and Future, 17 Kennedy, C. Abundance Analysis of CEMP RR Lyrae Merger AM 1219-430 with Gemini/GMOS-S, 378 Krabbe, A. C. Spatial variations of physical and chem- Stars, 271 Kennicutt, R. Mapping dust-obscured light in CALIFA ical properties of the planetary nebulae NGC 6302 galaxies, 122 Kepler, S. O. and NGC 2440, 352 Kraus, M. Asteroseismology of massive pulsating DA white dwarf stars with fully evolutionary models, 45 Kepler, S. O. White Dwarf Stars, 13 Kerber, L. O. On the origin of the wind variability of 55 Cyg, 247 Checking the consistency of physical Kravtsov, A. The MW and the Local Group mass, 471 Krebs, P. R. Astronomy and the interdisciplinary undergraduation formation, 499 parameters of open clusters: the case of NGC188 Kromer, M. and M67, 297 Krone-Martins, A. G. O. Revisiting TW Hydrae in light Kerber, L. O. Present-day Mass Function of Four LMC of new astrometric data, 315 Krongold, Y. Evolutionary Sequence for Seyfert Galax- Star Clusters with Multiple Stellar Populations, 306 Kerber, L. O. Self-consistent physical parameters for ies: A Point of View from Dust Geometric Distribu- 5 intermediate-age SMC stellar clusters from CMD tion, 430 Kroth, E. C. modelling, 252 Kervella, P. A new class of type Ia Supernovae, 77 Classical Cepheids from long-baseline Brazilian Participations in the Interna- tional Astronomical Search Collaboration, 186 interferometry: diameters, distances, circumstellar Kroupa, P. Phase Mixing in Popping Star Clusters, 296 envelopes and binarity, 254 Kurczynski, P. Kharb, P. Kinematics and excitation of the nuclear Submillimeter Galaxy Number Counts in a Semi-analytic Model: the Count Matching spiral in the active galaxy Arp 102B, 423 Approach, 386 535 Kurtev, R. Lancçon, A. The Next Generation Virgo Cluster Survey Proper motions and brown dwarfs in the VVV survey, 83 Kurtev, R. - Infrared (NGVS-IR), 131 Landin, N. R. Using MASSCLEAN to Describe Stellar Clusters Found in the Vista Variables in the Via Landin, N. R. Lactea (VVV) Survey, 303 Kurtev, R. Weather on Other Worlds: Brown Dwarf imposed parametric magnetic field, 266 Lanfranchi, G. A. Lépine, J. R. D. A bolha infravermelha N10, 343 Galaxies, 373 Lépine, J. R. D. Mass extinctions, galactic orbits in the Lanfranchi, G. A. solar neighborhood and the Sun: a connection?, 79 3D hydrodynamical simulations, 112 nation from observations at Observatório Pico Dos Langhi, R. Dias, 372 Proper motion determination of the The connection between metals, specific SFR and H I gas in galaxies: the Z-SSFR relation, 109 catalogue, 298 Lara-López, M. A. The use of rendering techniques in The role of the corotation resonance Galaxy Cluster Finding, 455 in the secular evolution of disks of spiral galaxies, Larrañaga-Rubio, E. A. 124 Corrections on an Observational Level, 463 High-redshift translucent clouds: detection of neutral species in QSO absorbers, 382 SFH of galaxies using spec- and CTA Era, 165 Lazarian, A. and ultraviolet photometry of the GALEX mission, 339 The star formation history of Lazarian, A. The role of reconnection diffusion in the galaxies in the CALIFA survey, 16 gravitational collapse of turbulent cloud cores, 89 López Cruz, O. A photometric study of M67: anchoring Lazzaro, D. Finding minor Bodies with the JPAS/J-PLUS measurements for the determination of astrophysical photometric surveys, 229 parameters of bright stars, 63 Lazzaro, D. Mapping the early distribution of volatiles The use of rendering techniques in in the Main Belt with the JPAS/J-PLUS photometric Galaxy Cluster Finding, 455 survey, 38 Labrie, K. Probing AGN accretion through microlens- Lazzaro, D. ing, 432 Leão, M. R. M. 89 in optical long-baseline interferometry, 492 Leauthaud, A. The red sequence of Abell X-ray Leauthaud, A. The CFHT/MegaCam Stripe-82 Survey, Photostability of Organic Molecules in 160 Circumstellar Environment, 96 LeCoarer, E. High dispersion spectra and kinematic Structure of Bubbles in the South-East region of the Large Magellanic Cloud, 347 line profiles of NGC3918 and NGC6302, 345 LAGO Collaboration Measuring galaxy morphologies in the CFHT/MegaCam Stripe-82 Survey, 462 underluminous clusters, 468 Lago, P. J. A. The role of reconnection diffusion in the gravitational collapse of turbulent cloud cores, Lachaume, R. Atmospheric and coupling scintillation Lago, A. F. The IMPACTON project: rotational properties of NEAs, 222 Physical properties of galaxies in the Sloan Digital Sky Survey detected in infrared, 379 Laganá, T. F. New Avenues for Measuring Magnetized Turbulence in the Multiphase Interstellar Medium, 383 Lacerda, E. A. Using MASSCLEAN to Describe Stellar Lazarian, A. Acceleration of Cosmic Rays in the FERMI troscopy in the optical range of the CALIFA sample López Cruz, O. LLAMA Project, 173 Larsen, S. S. Lactea (VVV) Survey, 303 of neutral species in QSO absorbers, 382 López-Fernández, R. Larrarte, J. J. Clusters Found in the Vista Variables in the Via High-redshift translucent clouds: detection López-Fernández, R. Gravitational Waves formulation for the Brane Universe and Possible Induced The deceleration of nebular shells in evolved planetary nebulae, 98 López, S. Brazilian Eratosthenes Project, 503 Lara-López, M. A. Galaxy And Mass Assembly (GAMA): optically visible open clusters based on the UCAC4 López, P. The effects of dark matter halo on the mass loss process in dwarf galaxies: results from Lépine, J. R. D. Open Cluster Radial Velocity determi- López, J. A. Effects of dark matter and energy on the chemical enrichment of Dwarf Spheroidal Lépine, J. R. D. LLAMA Project, 173 Lépine, J. R. D. Stellar models of low-mass, rotating pre-main sequence stars and the effects of an variability and VVV, 84 Lépine, J. R. D. Pre-main sequence evolutionary tracks and isochrones in color-magnitude diagrams, 261 Leister, N. V. Analysis and validation of data features, 314 in the search for GRB, 486 536 ALS 2883: Analysis of spectroscopic Leitzinger, M. Lombardi, G. The BIOSUN project:an astrobiological approach to study the origin of life in the context of with the SL-SLODAR and LUSCI at ESO Paranal the young Sun/solar stellar analogs, 235 Observatory, 493 Leiva, R. E+A galaxies in SDSS. Stellar population and Lopes, A. morphology, 381 Lellouch, E. 456 graduation formation, 499 Lopes, P. A. A. A Proposal of Astronomy Teaching on the Museu de Ciencias Naturais Pontificia Universidade Scaling Relations, 105 Defining our place in the cosmos. Mapping from Chandra X-ray Observations of the Bootes the vision of the brazilian population about the Fields, 484 Lopes, P. A. A. Universe and its origins, 504 Levato, H. 3 Atmospheric stratificatfication in NLTE of Lopes, P. A. A. El Catalogo Bibliografico de Velocidades Green Valley, 107 Lopes de Oliveira, R. Rotational Properties of A-Type Stars, 257 Levenhagen, R. S. ALS 2883: Analysis of spectroscopic Reddening-Free Indices in the VISTA Filter observed by the Swift satellite, 270 Lopes de Oliveira, R. Le Campion, J. F. Proper motions of pre-main se- from spectroscopy, 262 Lopez, A. Revisiting TW Hydrae in light of Lopez, J. A. How do Brightest Cluster and Group galaxies grow? Observations vs Models, 106 central stars, 49 Lopez, S. Lima, G. H. R. A. Modeling the circumstellar environ- The Proximity Effect toward z > 3.5 QSOs: Assesing systematics with XSHOOTER data, 438 Lorenz-Martins, S. ment of AB Aur using the Halpha line, 325 Lima, M. Constraining Cosmological Parameters from Photometry and Spectroscopy of Asteroids Rich in Volatils of the Type Main Belt Galaxy Clusters, 447 Comets (MBC), 221 Lorenzo-Oliveira, D. Cosmology from the Angular Correlation Function and Galaxy Clusters , 154 Lima, M. Two rings but no fellowship: LoTr 1 and its relation to planetary nebulae possessing Barium Study of Young Stellar Clusters in the Nebular Complex NGC6357 with VVV, 82 Lima, M. GeMS/GSAOI: from commissioning to operations and science results, 180 new astrometric data, 315 Lima, E. F. Unveiling optical properties of the high mass X-ray binary XMMU J054134.7-682550 quence stars, 300 Le Campion, J. F. Cas-like stars, 481 System, 80 Lidman, C. Highlights on Lopes de Oliveira, R. In the wake of ultraviolet sources features, 314 Leyton, P. Quenching Star Formation Now and Then: Downsizing of the Mass Flux Density in the Radiales, 264 Levato, H. Properties of Galaxies and Groups at z < 1.4, 387 He and 4 He in the Bp star a Cen, 265 Levato, H. Constraining Galaxy Evolution with Lopes, P. A. A. Properties of Galaxies Groups Selected Catolica de Minas Gerais, 508 Leroy, P. The Galaxy Cosmological Mass Function, Lopes, B. Astronomy and the interdisciplinary under- Study of Pluto’s atmosphere from stellar occultation, 200 Leroy, P. Surface Layer turbulence profiling In search of precise isochronal ages: Monte Carlo and Bayesian Approach, 263 Lorenzo-Oliveira, D. Improving the Modeling and Cosmologi- Mass extinctions, galactic or- cal Constraints of the Galaxy Angular Correlation bits in the solar neighborhood and the Sun: a Function, 448 connection?, 79 Lima, M. P. The SOAR Gravitational Arc Survey, 158 Lima Neto, G. B. Lucas, P. The red sequence of Abell X-ray Lucas, P. Deep infrared extinction maps of the Fourth underluminous clusters, 468 Lin, H. The SOAR Gravitational Arc Survey, 158 Galactic Quadrant based on VVV and GLIMPSE Littlefair, S. Stellar occultation by the trans-Neptunian surveys, 342 Lucas, P. Infrared study of new star clusters associated object 2002 KX14, 195 Liu, Y. Recurrent solar coronal jets induced by to dusty globules, 330 Lucas, P. magnetic emergence, 78 Livorati, A. L. P. Mostra Astronômica: building the Proper motions and brown dwarfs in the VVV survey, 83 Lucas, P. reality as a dream, 502 Lloyd, M. A Candidate Globular Cluster Behind the Milk Way?, 319 Two rings but no fellowship: LoTr 1 and The wide view of the Bulge from the VVV survey, 123 Lucas, P. its relation to planetary nebulae possessing Barium central stars, 49 Using MASSCLEAN to Describe Stellar Clusters Found in the Vista Variables in the Via Lactea (VVV) Survey, 303 537 Luhrs, J. GeMS/GSAOI: from commissioning to oper- Maia, F. F. S. Spectroscopy of the open cluster remnant ations and science results, 180 Luna, G. J. M. candidate ESO429-SC02, 292 Maia, M. A. G. Mapping Triangulum-Andromeda with In the wake of ultraviolet sources observed by the Swift satellite, 270 the SDSS, 392 Luna, G. J. M. Symbiotic stars in X-rays and UV, 47 Lupu, R. Maia, M. A. G. The LMC outer disk stellar population Herschel-ATLAS and ALMA: I. A z=1.027 in the light of the Dark Energy Survey, 135 Maia, M. A. G. Einstein Ring of Molecular Gas and Dust, 139 Luque, E. F. Present-day Mass Function of Four LMC Maiolino, T. Star Clusters with Multiple Stellar Populations, 306 Müller, A. S. Two-dimensional kinematics of the 489 Maiz Apellaniz, J. integral field spectrocopy, 421 Halo-based reconstruction of the cosmic of Southern O and WN stars, 72 Makler, M. Imaging polarimetry of the potentially Makler, M. NaCo view, 30 Time lags of the kilohertz quasi-periodic 363 Makler, M. 1608-52 and 4U 1636-53, 167 Makler, M. The CFHT/MegaCam Stripe-82 Survey, 160 interferometry: diameters, distances, circumstellar Makler, M. envelopes and binarity, 254 A new insight to the O Vz stars Radiales, 264 Maldonado, V. Elementary School Teachers’ Concep- Malkan, M. The Role of AGN Feedback in the Evolution the Shadows of the Objects, 506 of Seyfert Galaxies, 152 Planetary nebulae near the Galactic Malvina, A. P. centre: chemical abundances , 43 Maddox, S. Mancillas-Vaquera, B. L. Einstein Ring of Molecular Gas and Dust, 139 Mandrini, C. H. Manso-Sainz, R. Abundance determinations in ionized and Magellanic Clouds B[e] Supergiants, 276 nebulae and their sensitivity to temperature, 7 Magalhães, A. M. SOUTH POL: Revealing the Polarized Marchant, C. Southern Sky, 174 Marchant, P. Musca Dark Cloud, 353 On magnetic fields in barotropic stars, 242 Magalhães, A. M. The Magnetic Field Structure of the Marchiano, P. E. Interstellar Medium From the observations Open Extensive MultiConfiguration calculations of oscillator strengths useful for Astrophysics Clusters, 354 Applications, 250 Magnetic Fields dispersion and YSO Marcolino, W. White dwarfs in the Javalambre Physics properties on nearby Bok globules, 335 of the Accelerating Universe Survey, 259 Steady-state Accretion Disk Marcos, R. V. Models With Variable Alpha, 326 Materiais Interativos no Ensino de Astronomia, 505 Andromeda’s interplay with its dwarf Marinello, M. A. O. companions, 116 Magris, G. GeMS/GSAOI: from commissioning to operations and science results, 180 Magalhães, A. M. The Magnetic Field Structure in the Magrini, L. Solar Transient Activity: Magnetic Energy Release and Topology, 8 Magalhães, A. M. Envelopes of Evolved Stars: Galactic Magalhaes, E. R. S. O. The galaxy-halo connection and scale relations for disks galaxies, 413 SFR in dwarf spiral galaxies, 380 Magalhães, V. S. Astronomy and the interdisciplinary undergraduation formation, 499 Herschel-ATLAS and ALMA: I. A z=1.027 Magaña-Serrano, M. A. Constraints on the First Ionizing Sources, 472 tions about the Apparent Movement of the Sun and Maciel, W. J. The SOAR Gravitational Arc Survey, 158 Malaroda, S. El Catalogo Bibliografico de Velocidades within the framework of the GOSS Survey, 71 Machado, D. I. Measuring galaxy morphologies in the CFHT/MegaCam Stripe-82 Survey, 462 Classical Cepheids from long-baseline Maı́z Apellániz, J. Dynamical Analyses of z= 0.3, 0.5 Galaxy Clusters from the SOAR Gravitational Arcs Survey, oscillations in the low-mass X-ray binaries 4U Mérand, A. A Systematic Study of the NFW and SIS Elliptical Lensing Models in the Strong Regime, 159 planet-forming circumstellar disk HD 142527. The Méndez, M. OWN Survey: results after seven years of high-resolution spectroscopic monitoring mass density field, 155 Ménard, F. Developments with the hard X-Ray detection plane of the protoMIRAX imaging telescope, central region of NGC4501 from Gemini/GMOS Müller, V. The SOAR Gravitational Arc Survey, 158 Physical properties of FeII emission in active galactic nuclei, 428 Assessment of the SFH retrieved from Mario-A. Higuera-G. synthetic u’g’r’i’z’ photometry of galaxies, 117 Diagnostic diagrams with polycyclic aromatic hydrocarbons in diferent types of galaxies, 434 538 Marques, G. A. Mast, D. Resolving galaxies in time and space: Applying North-South CMB analyses using the Minkowski Functionals, 457 Marriner, J. STARLIGHT to CALIFA data cubes, 369 Mateus, A. Physical properties of galaxies in the Sloan Properties of type Ia supernovae inside rich galaxy clusters, 470 Marsh, T. Digital Sky Survey detected in infrared, 379 Mateus, A. Stellar occultation by the trans-Neptunian object 2002 KX14, 195 Martı́n, E. L. Detectability of Habitable Planets around Mateus, A. Very Low-Mass Stars, 36 Martı́nes-Galarza, J. R. Matos, M. F. Diagnostic diagrams with Matos, S. Martı́nes-Galarza, J. R. Physical parameters of galaxies 336 models, 394 experiment, 494 Mattiuci, A. C. exoplanet host stars, 230 Martı́nez, S. M. Potential-Density Pairs for Thin Disks Mauas, P. Chemical abundances and physical param- Type II Polynomials, 414 Martı́nez-Delgado, D. eters of evolved stars with planets, 288 Mauas, P. Globular clusters as tracers of the hierarchical formation of the Milky Way, 156 Stelar Activity in stars with planets from CASLEO spectra, 287 Martı́nez-Garcı́a, E. E. Disk Mass-to-light Ratio Distri- Mauas, P. bution from Stellar Population Synthesis: Application Transit Timing Variations analysis in exoplanet host stars, 230 Mauco, K. to Rotation Curve Decomposition of NGC 5278, 395 A long-term study of the Be star Mu Diversity of protoplanetary disks in stellar clusters: the case of the sigma Orionis cluster, 12 Mauro, F. Centauri in the L-band, 236 Martayan, C. Emission-line stars in the star-formation Near-Infrared Photometric Parameters of Galactic Globular Clusters From the VVV Survey, 81 Mauro, F. region NGC 1850, 334 Two rings but no fellowship: LoTr 1 and Photometric analisys of Galactic Stellar Clusters in VVV Survey, 307 May, D. The Architecture of the Active Galactic Nuclei its relation to planetary nebulae possessing Barium central stars, 49 of NGC 1068, 429 Maza, N. L. Atmospheric stratificatfication in NLTE of Quenching Star Formation Now and 3 Then: Downsizing of the Mass Flux Density in the He and 4 He in the Bp star a Cen, 265 Mazzalay, Z. Green Valley, 107 Martinez, H. J. An observational overview of the rotation in binary systems, 290 and Spheroidal Haloes II: Expansion in Chevishev Comparing galaxy populations in Coronal Emission in the Active Galactic Nuclei and its relationship to outflows , 144 McGinnis, P. T. compact and loose groups of galaxies, 119 Martins, L. P. Line Identification in the Sun’s Spectrum, The inner disks of classical T Tauri stars in NGC 2264, 331 McKay, T. M. The SOAR Gravitational Arc Survey, 158 260 Martins, L. P. Modeling Blue Horizontal Branch Stars, Mediavilla, E. 289 Estimating the size of the emitting region in the lens quasars HE0047-1756 and Martins, L. P. Spectral Synthesis of Star-forming SDSS1155+6346, 437 Meilland, A. Galaxies in the Near-Infrared, 114 Martins, S. L. White dwarfs in the Javalambre Physics Mejı́a, A. J. Martins-Filho, W. S. Dynamical evolution of differen- Assessment of the SFH retrieved from synthetic u’g’r’i’z’ photometry of galaxies, 117 Meléndez, J. tiated asteroid families, 211 Martins-Novais, P. Overview of Stellar Interferometry and its contribution to the study of massive stars, 73 of the Accelerating Universe Survey, 259 The distribution of stellar popula- Detailed differential chemical analysis of a poor metal star: new evidences about planet tions within galaxies, 384 formation, 245 Martioli, E. Detectability of Habitable Planets around Meléndez, J. Very Low-Mass Stars, 36 Masetti, N. Improving INPE’s balloon ground facilities for operation of the protoMIRAX Transit Timing Variations analysis in Martin, D. C. Star formation at the edge of the Universe, Mattiello-Francisco, M. F. with star formation through mid-infrared SED Martell, S. Brazilian Participations in the Interna- tional Astronomical Search Collaboration, 186 of galaxies, 434 Martayan, C. The lost population of post-starburst galaxies, 407 polycyclic aromatic hydrocarbons in diferent types Martı́nez, C. The environmental properties of galaxies probed by marked statistics, 385 Differential chemical abundances of heavy elements in solar twins, 283 Meléndez, J. Searching for near-infrared counterparts of high energy sources: Variability studies from VVV Finding new planets around solar twins using the HARPS/ESO spectrograph, 203 Survey, 483 539 Melendez, B. E. Mendoza, E. F. Photostability of Organic Molecules in New axion bounds from the white dwarf luminosity function, 44 Melgarejo Yrupailla, R. Circumstellar Environment, 96 Mendoza-Castrejón, S. Envelopes of Evolved Stars: Galactic and Magellanic Clouds B[e] Supergiants, 276 Melioli, C. Distribution, 430 Menezes, R. B. Collimation and scattering of the AGN Galaxy evolution-Star formation connection: from pc to kpc scales, 138 Melita, M. Evolutionary Sequence for Seyfert Galaxies: A Point of View from Dust Geometric emission in the Sombrero galaxy, 151 Menezes, R. B. Tidal, thermal and magnetic evolution of terrestrial exoplanets in the habitable zone of dwarf Way, 121 Menezes, R. B. IFU properties of 10 Early-type galactic stars, 37 Mello, A. T. New algorithm for centroiding in elongated nuclei, 141 Menezes, R. B. The Architecture of the Active Galactic Shack-Hartmann wavefront sensors spots using artificial neural networks, 179 Mello, A. T. Fireworks at the center of the Milky Nuclei of NGC 1068, 429 Mennickent, R. E. Simulations of atmospheric turbulence with spatiall phase modulators, 487 Melo, C. H. F. Close-in planets around giant stars, 210 Melo, C. H. F. Mennickent, R. E. Emission-line stars in the star-formation Finding proto-spectroscopic binaries: region NGC 1850, 334 Mennickent, R. E. Precise multi-epoch radial velocities of 7 protostars in Ophiuchus, 332 Merchán, M. E. Anisotropic Halo Model, 465 Merchán, M. E. 90 Menéndez-Delmestre, K. First spatially-resolved ob- Merrifield, M. high-redshift starbursts, 118 galaxy, 364 Mesa-Delgado, A. minous starbursts:a door to understand high-redshift Lyman-Break Galaxies, 389 Quenching Star Formation Regions, 101 Mesa-Delgado, A. in the Green Valley, 107 Secular Evolution in Green Stars, 99 Messias, H. BOMBOLO: a Multi-Band, Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 Metchev, S. Wide-field, Near UV/Optical Imager for the SOAR 4m Telescope, 178 Weather on Other Worlds: Brown Dwarf variability and VVV, 84 Meza, E. Pre-main sequence evolutionary tracks and isochrones in color-magnitude diagrams, Study of Pluto’s atmosphere from stellar occultation, 200 Michalowski, M. 261 Stellar models of low-mass, rotating 139 Michtchenko, T. A. Disk-planet interactions, 198 imposed parametric magnetic field, 266 Michtchenko, T. A. Metallicity gradients in tidal tails and merging systems, 405 Mendes de Oliveira, C. Mieske, S. Observational Results using BTFi, 177 A new class of galaxies (?): ultra-compact dwarfs, 115 Miller, L. and non-fossil groups from the maxBCG sample , Measuring galaxy morphologies in the CFHT/MegaCam Stripe-82 Survey, 462 Miller, L. 358 The CFHT/MegaCam Stripe-82 Survey, 160 Miller Bertolami, M. M. Star formation outside the Elliptical Galaxy NGC2865, 137 Mendes de Oliveira, C. Use of Mathematica software in the study of planetary dynamics, 202 Mendes de Oliveira, C. Properties of galaxies in fossil Mendes de Oliveira, C. Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, pre-main sequence stars and the effects of an Mendes de Oliveira, C. The Carbon Content in Galactic Ring Nebulae: CNO Nucleosynthesis in Massive Valley Galaxies, 388 Mendes, L. T. S. Carbon and Oxygen Abundances from Recombination Lines in Low Metallicity HII Now and Then: Downsizing of the Mass Flux Density Mendes, L. T. S. The connection between the origins of globular clusters and the evolution of their host Menéndez-Delmestre, K. Low-redshift compact UV lu- Menéndez-Delmestre, K. Determination of Halo Occupation Distribution, 397 servations of ionized gas in submillimeter-selected Mendes de Oliveira, C. Search for Southern Galactic Be star candidates, 50 Melo, C. H. F. The SACY view of the Sco-Cen complex, Menéndez-Delmestre, K. A long-term study of the Be star Mu Centauri in the L-band, 236 New axion bounds from the white dwarf luminosity function, 44 Millour, F. The red sequence of Abell X-ray underluminous clusters, 468 Overview of Stellar Interferometry and its contribution to the study of massive stars, 73 540 Milone, A. C. Monfredini, T. Detailed differential chemical analysis of a poor metal star: new evidences about planet Circumstellar Environment, 96 Moni Bidin, C. Near-Infrared Photometric Parameters formation, 245 Milone, A. C. Improvement and analysis of the MILES of Galactic Globular Clusters From the VVV Survey, library for stellar population modelling , 55 Minniti, D. 81 Moni Bidin, C. Photometric analisys of Galactic Stellar A Candidate Globular Cluster Behind the Milk Way?, 319 Clusters in VVV Survey, 307 Minniti, D. Abundâncias de Zinco em estrelas do bojo Moni Bidin, C. Monteiro, H. Galáctico, 278 Minniti, D. Confirmation of a cluster of galaxies Monteiro, H. Mapping of the Physicochemical Condi- Survey, 409 tions of the Planetary Nebula Menzel 1, 274 Monteiro, H. Galactic Quadrant based on VVV and GLIMPSE surveys, 342 Infrared study of new star clusters Dias, 372 Monteiro, H. Proper motions and brown dwarfs in the Monteiro, H. Searches for variability in the Milky Way catalogue, 298 Montes, V. Searching for near-infrared counterparts of high energy sources: Variability studies from VVV GeMS/GSAOI: from commissioning to operations and science results, 180 Montmerle, T. Survey, 483 Minniti, D. The VVV Survey, 67 Minniti, D. The general catalog of VISTA variables in A X-ray view of young star population in CMa R1, 88 Montmerle, T. the Via Lactea, 70 Supernova remnants colliding with molecular clouds: From high- to low-energy inter- The wide view of the Bulge from the VVV actions, 76 Montmerle, T. The nature of X-ray sources associated survey, 123 Minniti, D. Proper motion determination of the optically visible open clusters based on the UCAC4 bulge with the VVV Survey, 69 Minniti, D. Parsec-scale Activity in BL Lacertae: Signature of Relativistic Jet Precession, 146 VVV survey, 83 Minniti, D. Open Cluster Radial Velocity determination from observations at Observatório Pico Dos associated to dusty globules, 330 Minniti, D. Estimating metallicities with isochrone of open clusters, 56 Minniti, D. Deep infrared extinction maps of the Fourth Minniti, D. The local dark matter density, 308 fits done by global optimization to photometric data hidden behind the Galactic bulge using the VVV Minniti, D. Photostability of Organic Molecules in Using MASSCLEAN to Describe Stellar to young clusters around Sh2-296, 301 Clusters Found in the Vista Variables in the Via Mora, M. D. Star clusters in an infalling galaxy, 42 Lactea (VVV) Survey, 303 Moraes, B. Minniti, D. VVV Survey search for distant Cepheids in CFHT/MegaCam Stripe-82 Survey, 462 Moraes, B. The CFHT/MegaCam Stripe-82 Survey, 160 the inner Milky Way, 286 Minniti, D. Variable stars in the VVV globular clusters, Morales, N. Stellar occultation by the trans-Neptunian 68 object 2002 KX14, 195 Minniti, D. Moreno, C. Weather on Other Worlds: Brown Dwarf variability and VVV, 84 Mirabel, I. F. operations and science results, 180 of the Universe, 161 Unveiling the nature of an ultra-luminous X-ray source through the kinematics and structure of its optical counterpart , 168 Morisset, C. 3MdB: Mexican million models database, axes stars in open cluster Pleiades, 267 Miszalski, B. Two rings but no fellowship: LoTr 1 and 346 Morisset, C. Ionization Correction Factors in Planetary its relation to planetary nebulae possessing Barium central stars, 49 Nebulae, 100 Morisset, C. The Multiwavelength Study of OH Mega- maser Galaxy IRAS16399-0937, 148 The Carbon Content in Galactic Ring Nebulae: CNO Nucleosynthesis in Massive Stars, 99 Molina, M. C. Mostra Astronômica: building the reality Morisset, C. Morras, R. as a dream, 502 Mollá, M. GeMS/GSAOI: from commissioning to Moreno-Mendez, E. High Mass X-ray Binaries at the Dawn Miranda, D. Estimating the slope of average rotational Mittal, R. Measuring galaxy morphologies in the The NEBULATOM cookbook, 403 LLAMA Project, 173 Morrell, N. NIP of Stars: early results and new eclipsing Evolution models for spiral and irregular galaxies, 108 binaries , 304 Mollá, M. Planetary nebulae near the Galactic centre: Morrell, N. I. chemical abundances , 43 A new insight to the O Vz stars within the framework of the GOSS Survey, 71 541 Morrell, N. I. OWN Survey: results after seven years of Murphy, S. J. high-resolution spectroscopic monitoring of South- 64 Murray, S. S. ern O and WN stars, 72 Mota, B. C. Viscous Disks in Be Stars, 51 Fields, 484 Muzic, K. asteroid families, 211 Finding minor Bodies with the Núñez, L. A. IOAA 2012: The first scientific Núñez, L. A. 2016 , 190 Núñez, L. A. LAGO Project , 485 Motta, V. Estimating the size of the emitting region in Nagar, N. the lens quasars HE0047-1756 and SDSS1155+6346, Napolitano, N. R. Studying the kinematics of the jet of SPH-cosmological simulations, 110 Mottola, S. Stellar occultation by the trans-Neptunian Naranjo, O. object 2002 KX14, 195 Naranjo, O. Programa de observación de ocultaciones nova host galaxies, 74 de estrellas desde el Observatorio Nacional de Llano Mourão, D. C. The Evolution of the G Ring Arc under del Hato, 213 the Effects of the Resonance with Mimas and the Nardini, M. Solar Radiation Force, 212 the context of the full sample, 169 Moyano, M. Multi-band characterization of hot jupiters Nascimento, J. using OPD data, 27 , 190 the evolution of their host Galaxy Clusters, 449 Nascimento, M. The Origin and Chemical Evolution of the Nascimento, R. S. Estimating the size of the emitting Navarete, F. A survey of extended H2 emission toward SDSS1155+6346, 437 a sample of massive YSOs, 327 Globular clusters as tracers of the hierar- Navarrete, C. Near-IR Period-Luminosity relations for chical formation of the Milky Way, 156 variable stars in omega Centauri, 268 Halo-based reconstruction of the cosmic mass density field, 155 Submillimeter Galaxy Num- Surface Layer turbulence profiling with the SL-SLODAR and LUSCI at ESO Paranal Observa- Evolution of Seyfert Galaxies, 152 tory, 493 Navarro, E. A. White dwarfs in the Javalambre Physics of the Accelerating Universe Survey, 259 - Infrared (NGVS-IR), 131 Navas, G. Observación de objetos cercanos a la Tierra Backsplash Galaxies, 128 (Observation of Neos), 214 Muriel, H. Comparing galaxy populations in compact Navas, G. and loose groups of galaxies, 119 Muro, G. Submillimeter Galaxy Number Counts Navarrete, J. Mueller-Sanchez, F. The Role of AGN Feedback in the Muriel, H. The VVV Templates Project, 249 Navarrete, F. Approach, 386 Matching Approach, 386 The Next Generation Virgo Cluster Survey Navarrete, C. in a Semi-analytic Model: the Count Matching ber Counts in a Semi-analytic Model: the Count Munoz, R. Properties of Galaxies and Groups at z < 1.4, 387 region in the lens quasars HE0047-1756 and Symbiotic stars in X-rays and UV, 47 The IMPACTON project: rotational properties of NEAs, 222 Exotic Globular Cluster NGC 3201, 309 Mukai, K. IOAA 2012: The first scientific international olympiad in Brasil, opening doors for 2016 Central Dominant Galaxies and Muñoz Arancibia, A. M. Mass and energy of GRB-SN events: multi-wavelength analysis of three associations in Mourão, D. C. The Janus-Epimetheus Ring, 31 Muñoz-Cuartas, J. C. Observación de objetos cercanos a la Tierra (Observation of Neos), 214 Mourão, A. Integral Field Unit spectroscopy of super- Muñoz, R. Evolution of the Mass-Metallicity relations in passive and star-forming galaxies from 3C279 using the method Cross-entropy, 431 Muñoz, J. A. Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 437 Muñoz, C. Simulation of Water Cerenkov Detector for detection of cosmic rays Using GEANT4 for the photometric survey, 38 Muñiz-Torres, M. A. Astronomy and Astrophysics in the Colombian Andes: the PAS Project, 172 Mapping the early distribution of volatiles in the Main Belt with the JPAS/J-PLUS Motter, J. C. Analysis and validation of data in the search for GRB, 486 international olympiad in Brasil, opening doors for Mothé-Diniz, T. The SONYC survey: Towards a complete census of brown dwarfs in star forming regions, 86 JPAS/J-PLUS photometric surveys, 229 Mothé-Diniz, T. Properties of Galaxies Groups Selected from Chandra X-ray Observations of the Bootes Mothé-Diniz, T. Dynamical evolution of differentiated Mothé-Diniz, T. The GALEX Nearby Young-Star Survey, Programa de observación de ocultaciones de estrellas desde el Observatorio Nacional de Llano Searches for variability in the Milky Way del Hato, 213 bulge with the VVV Survey, 69 542 Negrello, M. Nunes, R. C. Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 Neichel, B. quintessence model with a generalized DE EoS, 460 GeMS/GSAOI: from commissioning to O’Mill, A. L. operations and science results, 180 Nelson, T. O’Dea, C. AGN torus properties with WISE, 149 O’Dowd, M. ity arising from the rotational evolution of solar-type Ocampo, L. F. Probing AGN accretion through Astronomical Observatory of the ITM, 511 A dynamical mechanism to produce Oddone, M. A. Structure of Bubbles in the South-East high-inclinations TNOs, 39 region of the Large Magellanic Cloud, 347 Identification of families halos in a Odert, P. multi-domain space composed by proper elements, the young Sun/solar stellar analogs, 235 Neto, A. F. The SOAR Gravitational Arc Survey, 158 Oio, G. A. NGVS collaboration The Next Generation Virgo Cluster Olave, D. Properties of type Ia supernovae inside Olguin, L. Mass and energy of GRB-SN Olguin, L. tions in the context of the full sample, 169 Oliva-Altamirano, P. Spheroidal Haloes III: Expansion in Gegenbauer Olivares E., F. Nieva, M. F. Atmospheric stratificatfication in NLTE of He and He in the Bp star a Cen, 265 the context of the full sample, 169 AGN torus properties with WISE, 149 Oliveira, A. F. Galaxy Concentration Index in of open clusters, 56 Galaxy Detection Behind the Oliveira, A. S. High-ionization accretion signatures in Milky Way using the VVV Survey, 408 compact binary candidates from SOAR Telescope The red cluster sequence in low observations, 269 X-ray luminosity galaxy clusters, 458 Nogueira, E. C. Oliveira, A. S. The Behavior of Regular Satellites Oliveira, C. S. 215 Low-redshift compact UV luminous starbursts: a door to understand high-redshift Fractal Characteristics in the Lyman-Break Galaxies, 389 Lemaı̂tre-Tolman-Bondi, 459 Olmstead, M. D. Nogueira-Cavalcante, J. P. Quenching Star Formation Properties of type Ia supernovae inside rich galaxy clusters, 470 Now and Then: Downsizing of the Mass Flux Density Omont, A. in the Green Valley, 107 Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 Nogueira-Cavalcante, J. P. Secular Evolution in Green Orellana, G. Valley Galaxies, 388 Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, 139 Norberg, P. Subhalo abundance matching in different Orellana, R. B. Semi Analytic Models, 410 Alfabetización en Astronomı́a de docentes de Educación Primaria y de Educación Nuñez, N. E. Symbiotic stars in X-rays and UV, 47 Nunes, N. A. MLS110213:022733+130617: A new eclipsing polar above the period gap, 46 during the Nice Model’s Planetary Close Encounters, Nogueira, F. A. M. G. Estimating metallicities with isochrone fits done by global optimization to photometric data Low X-ray Luminosity Galaxy Clusters, 366 Nilo Castellón, J. L. Mass and energy of GRB-SN events: multi-wavelength analysis of three associations in 4 Nilo Castellón, J. L. How do Brightest Cluster and Group galaxies grow? Observations vs Models, 106 Polynomials, 415 Nilo Castellón, J. L. Diversity of protoplanetary disks in stellar clusters: the case of the sigma Orionis cluster, 12 Potential-Density Pairs for Thin Disks and Nikutta, R. A Spectro-photometric study if the young stellar cluster sigma Orionis., 328 events: multi-wavelength analysis of three associa- 3 Metallicity gradients in tidal tails and merging systems, 405 rich galaxy clusters, 470 Nieto, O. Spectral Properties of Narrow Line Seyfert 1 galaxies, 433 Survey - Infrared (NGVS-IR), 131 Nicuesa Guelbenzu, A. The BIOSUN project:an astrobiological approach to study the origin of life in the context of 208 Nichol, R. C. Presentation of the project for the recovery, scientific equipment and automation of microlensing, 432 Nesvorný, D. Probing AGN accretion through microlensing, 432 stars, 277 Nesvorný, D. The Multiwavelength Study of OH Mega- maser Galaxy IRAS16399-0937, 148 Nepomuceno, M. M. F. Time-dependent nonextensiv- Neri-Larios, D. M. Triplets of galaxies: A connection with compact groups?, 412 Symbiotic stars in X-rays and UV, 47 Nenkova, M. Observational constraints on a coupled Secundaria en La Plata, 187 Contributions of geomorphology for Orellana, R. B. the understanding of landscape evolution in rocky Detección de cúmulos abiertos en regiones extensas del cielo usando parámetros planets of the Solar System, 226 astrométricos, 310 543 Orellana, R. B. Primera identificación astrométrica y Padilla, N. Submillimeter Galaxy Number Counts in a espectrofotométrica de miembros de Bochum 7, 62 Semi-analytic Model: the Count Matching Approach, Ortega, A. Fotometrı́a de la luz cenicienta y albedo 386 Paez Tagliaferro, T. Weak lensing measurements from lunar para la determinacion del espesor optico atmosférico local, 495 radio data, 416 Ortega, M. E. G126.1–0.8–14: A molecular shell related Pakmor, R. Palma, T. A study of the recent chemical evolution of to Sh2-187, 341 Ortega, M. E. Study of triggered star formation in a the Large Magellanic Cloud, 41 Parize, M. M. bright-rimmed cloud, 322 Ortega-Minakata, R. A. An approach to measuring Paron, S. and comparisons with other measurements, 390 bright-rimmed cloud, 322 and Centaurs Objects: results from more than 10 Stellar occultation by the trans-Neptunian emission-line region and star-forming , 435 Pastoriza, M. G. Study of Pluto’s atmosphere from stellar occultation, 200 378 Pastoriza, M. G. Multiwavelength study of the young stellar Galaxies, 367 Pastoriza, M. G. Testing the Physical Properties of the Abundâncias de Zinco em estrelas do bojo Galáctico, 278 Ortolani, S. Unified Model for AGN, 420 Pastoriza, M. G. Self-consistent physical parameters for 5 intermediate-age SMC stellar clusters from CMD Pauletti, D. modelling, 252 Paunzen, E. Pavani, D. B. Galactic Embedded Clusters with 2MASS stellar cluster sigma Orionis., 328 infrared photometry, 311 Diversity of protoplanetary disks in stellar Pavani, D. B. clusters: the case of the sigma Orionis cluster, 12 at the South of Brazil, 509 Paz, D. J. Anisotropic Halo Model, 465 SFH of galaxies using spectroscopy in the Peña, M. optical range of the CALIFA sample and ultraviolet photometry of the GALEX mission, 383 Peimbert, A. in H II regions and their implications, 350 The effects of the interaction on Peimbert, M. the kinematics and abundance of AM 2229-735, 374 in H II regions and their implications, 350 extensas del cielo usando parámetros astrométricos, Pelinson, A. M. 310 Gravitational waves and stability of cosmological solutions in the Modified Starobinsky A physical model for AGN feedback: the inflation, 461 role of BH spin and magnetic field , 443 Pellizza, L. J. Low surface brightness galaxies and void Stellar feedback from black-hole high-mass X-ray binaries in galaxy formation models, walls, 375 Padilla, N. Densities, temperatures, pressures, and abundances derived from O II recombination lines Paı́z, L. G. Detección de cúmulos abiertos en regiones Padilla, N. Densities, temperatures, pressures, and abundances derived from O II recombination lines CALIFA survey, 16 Padilla, N. A kinematic study of different stellar populations in the irregular NGC 6822, 391 Pérez, E. The star formation history of galaxies in the Pérez-Montero, E. OEI, GTTP and Adventurers of the Uni- verse: training teachers and scientific dissemination Resolving galaxies in time and space: Applying STARLIGHT to CALIFA data cubes, 369 Pérez, E. a observations of three globular clusters: NGC 104 NGC 6205 NGC 7099, 58 A Spectro-photometric study if the young Pérez, E. Spectroscopic studies of two supernova remnants in the Large Magellanic Cloud, 349 as a dream, 502 Pérez, A. Unveling the LINER nature of NGC1052, 425 Ottani, V. C. Mostra Astronômica: building the reality Pérez, A. Probing the Spacial Distribution of the Near-infrared Stellar Population in Starburst cluster [DBS2003]156, 351 Ortolani, S. Photometry and Dynamics of the Minor Merger AM 1219-430 with Gemini/GMOS-S, A new distance scale of planetary nebulae, 348 Ortiz, R. Molecular hydrogen and [Fe II] in active galactic nuclei - III. Low-ionization nuclear object 2002 KX14, 195 Ortiz, R. Effects of interaction in chemical evolution and stellar population of galaxy pairs, 398 Pastoriza, M. G. observed events, 29 Ortiz, J. L. Study of triggered star formation in a Pastoriza, M. G. Stellar Occultations by Transneptunian Ortiz, J. L. Physical properties of galaxies in the Sloan Digital Sky Survey detected in infrared, 379 the density of the environment of galaxies: results Ortiz, J. L. A new class of type Ia Supernovae, 77 357 Subhalo abundance matching in different Penna, J. L. Semi Analytic Models, 410 Solar astrometry and the heliometer of Rio de Janeiro, 181 544 Penteado, E. M. Penteado, P. Pichardo, B. Pitch Angle Restrictions in Normal Spiral The GalileoMobile Project, 189 Small-body colors from the UV to the Galaxies Based on Ordered and Chaotic Orbital IR: bringing together all space and ground-based Behavior, 126 Pignata, G. observations, 216 Pereira, C. B. Pignata, G. High-resolution spectroscopic of red giants stars in NGC 2360, 273 the context of the full sample, 169 Pineault, S. of the Accelerating Universe Survey, 259 Measuring galaxy morphologies in to Sh2-187, 341 The CFHT/MegaCam Stripe-82 Sur- Pinho, A. rotators, 217 Pintado, O. I. CFHT/MegaCam Stripe-82 Survey, 462 Pereira Santos, J. Pinte, C. In the wake of ultraviolet sources NaCo view, 30 Pinzón, G. Envelopes of Evolved Stars: Galactic and Magellanic Clouds B[e] Supergiants, 276 Pinzón, G. Rotation and activity of Post T Tauri Stars, Magnetic Fields dispersion and YSO 337 Pereyra, A. The Magnetic Field Structure in the Musca Placco, V. M. The deceleration of nebular shells in spectroscopy, 262 Plana, H. evolved planetary nebulae, 98 Kepler” and its Institutional Pedagogical Project, 185 Poggianti, B. M. Pitch Angle Restrictions in Normal Polido, P. sources, 477 with the SDSS, 392 Modeling the circumstellar environment central stars, 49 Popescu, B. GeMS/GSAOI: from commissioning to Lactea (VVV) Survey, 303 Portilla, J. G. Correlating X-rays, UV and optical emission from the accretion disk in the nucleus of Porto de Mello, G. F. Study of triggered star formation in a In search of precise isochronal ages: Monte Carlo and Bayesian Approach, 263 Porto de Mello, G. F. bright-rimmed cloud, 322 Chemical abundances and physical Mass extinctions, galactic orbits in the solar neighborhood and the Sun: a parameters of evolved stars with planets, 288 connection?, 79 Porto de Mello, G. F. The BIOSUN project:an astrobi- Transit Timing Variations analysis in exoplanet host stars, 230 Pichardo, B. FHILs in Seyferts and Liners in the optical spectra, 442 NGC1097, 439 Petrucci, R. Using MASSCLEAN to Describe Stellar Clusters Found in the Vista Variables in the Via operations and science results, 180 Petrucci, R. Two rings but no fellowship: LoTr 1 and its relation to planetary nebulae possessing Barium of AB Aur using the Halpha line, 325 Petriella, A. The galactic distribution of Fermi point Pollacco, D. Mapping Triangulum-Andromeda Peterson, B. M. Galaxy Model in Infrared, 393 Polido, P. The internal density structure of Giant HII Regions, 102 Pessev, P. BUDHIES: a Blind Ultra Deep HI Environmental Survey, 129 Behavior, 126 Perrault, K. Metallicity gradients in tidal tails and merging systems, 405 Spiral Galaxies Based on Ordered and Chaotic Orbital Perottoni, H. D. Internal kinematics of HII galaxies, 362 Plana, H. “Planetário e Teatro Digital Johannes Perez Oregón, J. Unveiling optical properties of the high mass X-ray binary XMMU J054134.7-682550 from Dark Cloud, 353 Perez-Viilegas, A. Advances in the astronomical site testing in Colombia, 490 properties on nearby Bok globules, 335 Perez, E. R. Imaging polarimetry of the potentially planet-forming circumstellar disk HD 142527. The observed by the Swift satellite, 270 Pereyra, M. a observations of three globular clusters: NGC 104 NGC 6205 NGC 7099, 58 rotational axes stars in open cluster Pleiades, 267 Pereyra, A. The most common habitable planets – atmospheric characterization of the subgroup of fast Measuring galaxy morphologies in the Pereira da Silva, J. R. Estimating the slope of average Pereyra, A. The Janus-Epimetheus Ring, 31 Pinotti, R. The SOAR Gravitational Arc Survey, 158 Pereira, R. Multiwavelength study of the young stellar cluster [DBS2003]156, 351 vey, 160 Pereira, M. E. S. G126.1–0.8–14: A molecular shell related Pinheiro, M. C. the CFHT/MegaCam Stripe-82 Survey, 462 Pereira, M. E. S. Mass and energy of GRB-SN events: multi-wavelength analysis of three associations in Pereira, C. B. White dwarfs in the Javalambre Physics Pereira, M. E. S. A new class of type Ia Supernovae, 77 ological approach to study the origin of life in the Galactic Dynamics: Origin, History, context of the young Sun/solar stellar analogs, 235 Present and Prospect, 18 545 Pota, V. Rebassa-Mansergas, A. The connection between the origins of globular clusters and the evolution of their host binaries from SDSS DR8: unveiling the cool white galaxy, 364 dwarf population, 318 Proctor, R. N. Reggiani, H. Properties of galaxies in fossil and non-fossil groups from the maxBCG sample , 358 Reina, J. I. Potential-Density Pairs for Thin Disks and simulations, 125 Spheroidal Haloes I: Expansion in Chevishev Type I The general catalog of VISTA variables in Polinomials, 411 Reina, J. I. Potential-Density Pairs for Thin Disks and the Via Lactea, 70 Puzia, T. H. BOMBOLO: a Multi-Band, Wide-field, Spheroidal Haloes II: Expansion in Chevishev Type Near UV/Optical Imager for the SOAR 4m Telescope, II Polynomials, 414 Reina, J. I. 178 Puzia, T. H. Dynamical Properties of Blue Straggler Polynomials, 415 Reis, R. R. R. Cen and NGC6218, 59 Puzia, T. H. Star clusters in an infalling galaxy, 42 Astrophysical Survey (J-PAS), 466 Reisenegger, A. On magnetic fields in barotropic stars, - Infrared (NGVS-IR), 131 242 The SACY view of the Sco-Cen complex, Reiss, M. 90 Reis Neto, E. IOAA 2012: The first scientific 190 2016 , 190 Reis Neto, E. Diagnostic diagrams with polycyclic Reitano, L. 434 489 formation through mid-infrared SED models, 394 Rejkuba, M. The wide view of the Bulge from the VVV survey, 123 Magnetic Fields dispersion and YSO Remolina Gutiérrez, M. C. properties on nearby Bok globules, 335 Renzini, A. Abundâncias de Zinco em estrelas do bojo ranges: HD 209458b a case study, 316 Galáctico, 278 Huge-LQG- the largest structure in Repetto, P. Disk Mass-to-light Ratio Distribution from the universe, 157 Stellar Population Synthesis: Application to Rotation A Study on the Universality Curve Decomposition of NGC 5278, 395 and Linearity of the Leavitt Law in the LMC and Rial, D. F. A new method to disentangle the rotational SMC Galaxies, 255 Rambold, W. velocities of stars: application to main-sequence GeMS/GSAOI: from commissioning to field Stars, 251 operations and science results, 180 Ramirez, E. A. Ribas, I. HST and Spitzer point source and the young Sun/solar stellar analogs, 235 galaxies, 150 Ribeiro, A. L. B. Properties of Galaxies and Groups at Ramos, M. L. Construction of a radiotelescope, 497 z < 1.4, 387 Mass and energy of GRB-SN events: Ribeiro, A. O. multi-wavelength analysis of three associations in Asteroids Atiras: study of stability and dynamical analysis of the region , 218 the context of the full sample, 169 Ribeiro, A. O. Rauber, A. B. Spatial variations of physical and chem- The IMPACTON project: rotational properties of NEAs, 222 ical properties of the planetary nebulae NGC 6302 Ribeiro, A. O. V-type asteroids among the Mars crosser and NGC 2440, 352 Ray, T. P. The BIOSUN project:an astrobiological approach to study the origin of life in the context of dust lane detection in powerful narrow-line radio Rau, A. RECA: A network by students, for students, 507 Raga, A. On the sensitivity of extrasolar mass–loss rate Ramı́rez-Tannus, M. C. Developments with the hard X-Ray detection plane of the protoMIRAX imaging telescope, Quintero, S. Physical parameters of galaxies with star Raghunathan, S. Solar astrometry and the heliometer of Rio de Janeiro, 181 aromatic hydrocarbons in diferent types of galaxies, Racca, G. A. IOAA 2012: The first scientific international olympiad in Brasil, opening doors for 2016 , international olympiad in Brasil, opening doors for Quintero, S. Mostra Astronômica: building the reality as a dream, 502 Observational Results using BTFi, 177 Quintanilha, C. E. The Type Ia Supernova Pipeline for the Javalambre Physics of the Accelerating Universe Puzia, T. H. The Next Generation Virgo Cluster Survey Quast, G. R. Potential-Density Pairs for Thin Disks and Spheroidal Haloes III: Expansion in Gegenbauer Stars in Galactic Globular Clusters: NGC3201, Omega Quint, B. Abundance Analysis of CEMP RR Lyrae Stars, 271 Puerari, I. Bar and spiral arms dynamics in numerical Pullen, J. White dwarf-main sequence population, 220 The SONYC survey: Towards a complete census of brown dwarfs in star forming regions, 86 546 Ribeiro, B. A. G. Riffel, R. Testing the Physical Properties of the Unified A Proposal of Astronomy Teaching on the Museu de Ciencias Naturais Pontificia Model for AGN, 420 Riffel, R. Unveling the LINER nature of NGC1052, 425 Universidade Catolica de Minas Gerais, 508 Ribeiro, E. M. Highlights on Cas-like stars, 481 Riffel, R. A. Ribeiro, F. B. Mostra Astronômica: building the reality revealed by PCA tomography, 427 Riffel, R. A. as a dream, 502 Ribeiro, F. B. A nuclear molecular ring in Mrk 1066 Spin-Orbit Resonances in Super-Earth Feeding and Feedback around the active nucleus of the Seyfert galaxy Mrk766, 440 Riffel, R. A. Systems Close to Mean-motion Commensurabilities, 219 Kinematics and excitation of the nuclear spiral in the active galaxy Arp 102B, 423 Ribeiro, M. B. Fractal Characteristics in the Lemaı̂tre-Tolman-Bondi, Riffel, R. A. 459 Ribeiro, M. B. Riffel, R. A. The Galaxy Cosmological Mass Func- tion, 456 Riffel, R. A. The Magnetic Field Structure in the Musca Dark Cloud, 353 Riffel, R. A. Two-dimensional kinematics of the central Envelope Binary RR Cae, 272 region of NGC4501 from Gemini/GMOS integral field Ribeiro, T. Probing accretion on the high-magnetized spectrocopy, 421 Riffel, R. A. polar RX J1007.5-2017, 312 Ribeiro, T. White dwarfs in the Javalambre Physics of Rigaut, F. Collimation and scattering of the AGN Rimulo, L. R. Rincón, A. IFU properties of 10 Early-type galactic nuclei, 141 Rinke, E. IFU spectroscopic analysis of the active Rivero González, J. Rivinius, T. The Architecture of the Active Galactic Nuclei of NGC 1068, 429 Young Brown Dwarfs as Giant Exoplanet The Multiwavelength Study of OH Megamaser Galaxy IRAS16399-0937, 148 Robinson, A. Herschel-ATLAS and ALMA: I. A Two-dimensional kinematics of the central region of NGC4501 from Gemini/GMOS z=1.027 Einstein Ring of Molecular Gas and Dust, integral field spectrocopy, 421 Rocco, M. L. M. 139 Coronal Emission in the Active Galactic Photostability of Organic Molecules in Circumstellar Environment, 96 Rocha-Pinto, H. J. Nuclei and its relationship to outflows , 144 Riffel, R. Molecular hydrogen and [Fe II] in ac- Collisions between Globular Clus- ters, 293 Rocha-Pinto, H. J. tive galactic nuclei - III. Low-ionization nuclear emission-line region and star-forming , 435 IOAA 2012: The first scientific international olympiad in Brasil, opening doors for Riffel, R. Nuclear outflows in the Seyfert 2 galaxy NGC 2016 , 190 Rocha-Pinto, H. J. 5929, 436 Probing the Spacial Distribution of the Mapping Triangulum-Andromeda with the SDSS, 392 Rocha-Pinto, H. J. Near-infrared Stellar Population in Starburst Galaxies, 367 Riffel, R. Viscous Disks in Be Stars, 51 Robinson, A. The deceleration of nebular shells in evolved planetary nebulae, 98 Riffel, R. V/R variations in Be shell stars, 253 Rivinius, T. spiral in the active galaxy Arp 102B, 423 Structure, 356 Riechers, D. A. Rivinius, T. Robinson, A. Kinematics and excitation of the nuclear The Discrepant Kinematics of ORLs and CELs in NGC 7009 as a Function of Ionization Richer, M. G. The GalileoMobile Project, 189 A long-term study of the Be star Mu Centauri in the L-band, 236 Analogs, 32 Richer, M. G. Improving INPE’s balloon ground facilities for operation of the protoMIRAX experiment, 494 nucleus NGC 6951 , 419 Ricci, T. V. Viscous Disks in Be Stars, 51 About Hohmann Transfer with Orbital Plane Change, 231 Ricci, T. V. IFU spectroscopic analysis of M81, 426 Ricci, T. V. GeMS/GSAOI: from commissioning to operations and science results, 180 emission in the Sombrero galaxy, 151 Ricci, T. V. Unveling the LINER nature of NGC1052, 425 the Accelerating Universe Survey, 259 Ricci, T. V. Two-dimensional Stellar Kinematics and Dynamical Models for NGC 4258 and NGC 1052, 371 Ribeiro, T. Accretion and Activity on the PostCommon- Riffel, R. Two-dimensional Kinematics of the Central Region of NGC 2110 , 424 Ribeiro, N. L. Rice, E. Nuclear outflows in the Seyfert 2 galaxy NGC 5929, 436 Study of clustering in the stellar abundances space, 294 Rocha da Silva, G. Spectral Synthesis of Star-forming Galaxies in the Near-Infrared, 114 Relativistic MHD Simulations of Magnetized Jets, 482 547 Rodón, J. A. Deuteration and fragmentation in massive Rodrigues, J. star-forming regions, 92 undergraduation formation, 499 Rodrı́guez, O. A new method to estimate distances to Rodrigues, M. Type II SNe, 451 Rodrı́guez-Ardila, A. Rodrigues, T. Coronal Emission in the Active Rodriguez, A. M. Molecular hydrogen and [Fe II] Rodriguez, D. R. Optical stellar and emission gas Rodriguez, F. Rodrı́guez-Ardila, A. Physical properties of FeII emis- Anisotropic Halo Model, 465 Rodriguez, F. sion in active galactic nuclei, 428 Determination of Halo Occupation Distribution, 397 Rodrı́guez-Ardila, A. Probing the Spacial Distribution Rodriguez, M. of the Near-infrared Stellar Population in Starburst Abundance determinations in ionized nebulae and their sensitivity to temperature, 7 Rodriguez-Puebla, A. The satellite population of Milky Galaxies, 367 Rodrı́guez-Ardila, A. Spectral Synthesis of Star-forming Way/Andromeda-sized galaxies, 136 Rodriguez del Pino, B. Galaxies in the Near-Infrared, 114 Rodrı́guez-Camargo, C. D. Gravitational Waves for- Induced Corrections on an Observational Level, 463 Rodrigues, B. H. G. dynamical analysis of the region , 218 families, 211 Roig, F. telescope, 489 The hard X-ray telescopes for Roig, F. Identification of families halos in a multi-domain MIRAX and protoMIRAX, 175 space composed by proper elements, 208 Roig, F. detectors for the MIRAX Mission, 496 High-ionization accretion signatures survey, 38 Roig, F. The IMPACTON project: rotational properties observations, 269 MLS110213:022733+130617: A new of NEAs, 222 Roig, F. eclipsing polar above the period gap, 46 Rodrigues, C. V. Rojas, A. F. properties on nearby Bok globules, 335 Modeling photometric and spectro- Searching for near-infrared counterparts of high energy sources: Variability studies from VVV scopic data of HS 2231+2441: an HW Vir type system Survey, 483 Rojas, G. A. with a brown dwarf companion, 57 Rodrigues, C. V. Probing accretion on the high-magnetized Brazilian Participations in the Interna- tional Astronomical Search Collaboration, 186 Rojas, K. Estimating the size of the emitting region in polar RX J1007.5-2017, 312 Rodrigues, F. P. V-type asteroids among the Mars crosser population, 220 Magnetic Fields dispersion and YSO Rodrigues, C. V. Mapping the early distribution of volatiles in the Main Belt with the JPAS/J-PLUS photometric in compact binary candidates from SOAR Telescope Rodrigues, C. V. Finding minor Bodies with the JPAS/J-PLUS photometric surveys, 229 Rodrigues, B. H. G. The high resolution pixelated CZT Rodrigues, C. V. Asteroids Atiras: study of stability and Roig, F. Dynamical evolution of differentiated asteroid Developments with the hard X-Ray detection plane of the protoMIRAX imaging Rodrigues, B. H. G. Emission line imaging survey of the Abell 901/902 supercluster, 130 Roig, F. mulation for the Brane Universe and Possible Optical stellar and emission gas the lens quasars HE0047-1756 and SDSS1155+6346, kinematics of the Seyfert 2 Circinus galaxy, 444 437 Rojo, P. AM2217-490: Uma galáxia com anel polar em formação, 396 About Hohmann Transfer with Orbital Plane Change, 231 Rojo, P. Bar and spiral arms dynamics in Close-in planets around giant stars, 210 Román-Zúñiga, C. G. The Role of Local Environment numerical simulations, 125 Rodrigues, I. Dinâmica da Formação de Galáxias com in Stellar Cluster Formation, 91 Roman-Lopes, A. A Candidate Globular Cluster Behind Anel Polar, 359 Rodrigues, I. Photometry and Dynamics of the Minor the Milk Way?, 319 Roman-Lopes, A. Merger AM 1219-430 with Gemini/GMOS-S, 378 Rodrigues, I. The GALEX Nearby Young-Star Survey, 64 kinematics of the Seyfert 2 Circinus galaxy, 444 Rodrigues, I. FHILs in Seyferts and Liners in the optical spectra, 442 emission-line region and star-forming , 435 Rodrigues, I. The IMPACTON project: rotational properties of NEAs, 222 in active galactic nuclei - III. Low-ionization nuclear Rodrı́guez-Ardila, A. Integral Field Unit spectroscopy of supernova host galaxies, 74 Galactic Nuclei and its relationship to outflows , 144 Rodrı́guez-Ardila, A. Astronomy and the interdisciplinary The effects of the interaction on the Deep infrared extinction maps of the Fourth Galactic Quadrant based on VVV and kinematics and abundance of AM 2229-735, 374 GLIMPSE surveys, 342 548 Roman-Lopes, A. Rossi, S. Abundance Analysis of CEMP RR Lyrae Stars, Infrared study of new star clusters associated to dusty globules, 330 Roman-Lopes, A. 271 Rothschild, R. E. The hard X-ray telescopes for MIRAX NIP of Stars: early results and new eclipsing binaries , 304 and protoMIRAX, 175 Romanowsky, A. The connection between the origins Rothschild, R. E. of globular clusters and the evolution of their host Rubinho, M. S. galaxy, 364 Romeo, A. D. Evolution of the Mass-Metallicity re- Clusters, 354 Rubio, M. Gas, dust and star formation in the infrared SPH-cosmological simulations, 110 Asteroseismology of massive pulsating dust bubble S 24, 97 Rubio, M. DA white dwarf stars with fully evolutionary models, 45 Ruiz, A. IRDC G341.24-0.27, 87 Romero, G. A. Gas, dust and star formation in the Romero, G. E. 386 Ruiz, L. O. Magnetic field evolution and jet hydrodynamical simulations, 112 Runaway massive stars as a new class Sánchez, P. High-redshift translucent clouds: detection of galactic gamma-ray sources, 170 Romero, G. E. of neutral species in QSO absorbers, 382 The incidence of short time scale Sánchez, P. The Proximity Effect toward z > 3.5 QSOs: variability on different types of Blazars, 147 Assesing systematics with XSHOOTER data, 438 Rondón, E. Photometry and Spectroscopy of Asteroids Sánchez, S. F. CALIFA: The local extragalactic universe Rich in Volatils of the Type Main Belt Comets (MBC), unveiled (survey status), 120 221 Sánchez, S. F. Study of Pluto’s atmosphere from stellar Sánchez, S. F. Time-series JHK Photometry of Sánchez-Blázquez, P. Rosa, D. A. Effects of interaction in chemical evolution 55 Rosado, M. Disk Mass-to-light Ratio Distribution from Sánchez-Blázquez, P. Stellar Population Synthesis: Application to Rotation 369 Rosado, M. Unveiling the nature of an ultra-luminous Sánchez-Salcedo, F. J. X-ray source through the kinematics and structure The Gravitational Drag Force on an Extended Object Moving in a Gas, 166 of its optical counterpart , 168 Sánchez-Saldı́as, A. CALIFA: The local extragalactic Palaeogeographic reconstruction of Minchin palaeolake system, South America: the universe unveiled (survey status), 120 influence of astronomical forcing, 232 HST and Spitzer point source and dust lane Sabogal, B. E. detection in powerful narrow-line radio galaxies, 150 A Study on the Universality and Linearity of the Leavitt Law in the LMC and SMC Observación de objetos cercanos a la Galaxies, 255 Tierra (Observation of Neos), 214 Sabogal, B. E. Programa de observación de oculta- Search for Southern Galactic Be star candidates, 50 ciones de estrellas desde el Observatorio Nacional Saffe, C. Chemical abundances and physical parame- de Llano del Hato, 213 Rossi, A. Resolving galaxies in time and space: Applying STARLIGHT to CALIFA data cubes, Curve Decomposition of NGC 5278, 395 Rosenzweig, P. Improvement and analysis of the MILES library for stellar population modelling , and stellar population of galaxy pairs, 398 Rosenzweig, P. The star formation history of galaxies in the CALIFA survey, 16 Stars in the center of Cygnus OB2, 329 Rosales-Ortega, F. F. Resolving galaxies in time and space: Applying STARLIGHT to CALIFA data cubes, 369 occultation, 200 Roquette, J. M. T. The effects of dark matter halo on the mass loss process in dwarf galaxies: results from 3D formation in accreting neutron stars, 476 Romero, G. E. Submillimeter Galaxy Number Counts in a Semi-analytic Model: the Count Matching Approach, infrared dust bubble S 24, 97 Rose, M. Millimeter and Far-IR observations of the IRDC G341.24-0.27, 87 Romero, G. Millimeter and Far-IR observations of the Roques, F. The Magnetic Field Structure of the Interstellar Medium From the observations Open lations in passive and star-forming galaxies from Romero, A. D. The high resolution pixelated CZT detectors for the MIRAX Mission, 496 ters of evolved stars with planets, 288 Mass and energy of GRB-SN events: Saffe, C. multi-wavelength analysis of three associations in Stelar Activity in stars with planets from CASLEO spectra, 287 the context of the full sample, 169 Saito, R. K. Rossi, L. L. Physical properties of galaxies in the Sloan Proper motions and brown dwarfs in the VVV survey, 83 Digital Sky Survey detected in infrared, 379 549 Saito, R. K. Santos, J. H. B. Searches for variability in the Milky Way bulge with the VVV Survey, 69 Saito, R. K. evolution marker, 400 Santos, N. C. Study of Young Stellar Clusters in the Nebular Complex NGC6357 with VVV, 82 in Ophiuchus, 332 Saito, R. K. The wide view of the Bulge from the VVV Santos, P. Mapping of the Physicochemical Conditions survey, 123 of the Planetary Nebula Menzel 1, 274 Santos, R. G. Chemical abundances and physical parameters of evolved stars with planets, 288 Saker, L. 289 planet host stars, 230 the gravitational collapse of turbulent cloud cores, Properties of type Ia supernovae inside rich 89 Santos-Silva, T. A X-ray view of young star population galaxy clusters, 470 Salas, P. The dense gas in M82, 399 Sales, D. A. in CMa R1, 88 Santos Jr., J. F. C. Testing the Physical Properties of the Unified Model for AGN, 420 Sales, D. A. photometric indexes, 313 Santos Jr., J. F. C. maser Galaxy IRAS16399-0937, 148 High-resolution spectroscopic of red Unveiling the nature of an ultra-luminous of its optical counterpart , 168 from the VVV behind the galactic bulge, 417 Saraiva, M. F. O. The dense gas in M82, 399 Astronomy and the interdisciplinary nation at the South of Brazil, 509 Sarazin, M. Surface Layer turbulence profiling with the Time lags of the kilohertz quasi-periodic SL-SLODAR and LUSCI at ESO Paranal Observatory, oscillations in the low-mass X-ray binaries 4U 493 Sarmiento, C. 1608-52 and 4U 1636-53, 167 Sansom, A. Improvement and analysis of the MILES search for GRB, 486 Santander Garcia, M. Two rings but no fellowship: LoTr for detection of cosmic rays Using GEANT4 for the 1 and its relation to planetary nebulae possessing LAGO Project , 485 Savaglio, S. Barium central stars, 49 Santiago, B. X. Mapping Triangulum-Andromeda with the context of the full sample, 169 Santiago, B. X. Measuring galaxy morphologies in the Scannapieco, C. CFHT/MegaCam Stripe-82 Survey, 462 The formation of stellar haloes of massive Spirals in hierarchical scenario, 111 Santiago, B. X. Self-consistent physical parameters for Scarano Jr., S. 5 intermediate-age SMC stellar clusters from CMD Metallicity gradients in tidal tails and merging systems, 405 Scarano Jr., S. The role of the corotation resonance in modelling, 252 Santiago, B. X. The LMC outer disk stellar population the secular evolution of disks of spiral galaxies, 124 Schönell, A. J. J. in the light of the Dark Energy Survey, 135 The SOAR Gravitational Arc Survey, Feeding and Feedback around the active nucleus of the Seyfert galaxy Mrk766, 440 Schady, P. 158 Fast and slow radiation-driven wind Mass and energy of GRB-SN events: multi-wavelength analysis of three associations in solutions using ZEUS-3D, 239 Santos, H. B. S. Mass and energy of GRB-SN events: multi-wavelength analysis of three associations in the SDSS, 392 Santillán, A. Analysis and validation of data in the Sarmiento, C. Simulation of Water Cerenkov Detector library for stellar population modelling , 55 Santiago, B. X. OEI, GTTP and Adventurers of the Universe: training teachers and scientific dissemi- undergraduation formation, 499 Sanna, A. Integral Field Spectroscopy SINFONI observation of AGN at z ⇠ 1.6, 445 inflation, 461 Sampaio, M. Sagittarius dwarf galaxy population San Martı́n, A. Gravitational waves and stability of cosmological solutions in the Modified Starobinsky Salter, D. Central Dominant Galaxies and the evolution of their host Galaxy Clusters, 449 Santucho, M. V. X-ray source through the kinematics and structure Salles, F. O. Spectroscopy of the open cluster remnant candidate ESO429-SC02, 292 Santoyo-Ruiz, H. giants stars in NGC 2360, 273 Salinas, A. Discriminating Local Group embedded star clusters from older ones using near-IR The Multiwavelength Study of OH Mega- Sales Silva, J. V. Modeling Blue Horizontal Branch Stars, Santos-Lima, R. The role of reconnection diffusion in Transit Timing Variations analysis in exo- Sako, M. Finding proto-spectroscopic binaries: Precise multi-epoch radial velocities of 7 protostars Saito, R. K. The VVV Templates Project, 249 Saker, L. PAH lines at high redshift as galaxy the context of the full sample, 169 Schilke, P. An observational overview of the rotation in binary systems, 290 Deuteration and fragmentation in massive star-forming regions, 92 550 Schimoia, J. S. Sfair, R. Correlating X-rays, UV and optical emission from the accretion disk in the nucleus of The Evolution of the G Ring Arc under the Effects of the Resonance with Mimas and the Solar NGC1097, 439 Radiation Force, 212 Schlickmann, M. S. The mass–metallicity–star forma- Sfair, R. The Janus-Epimetheus Ring, 31 tion rate relation under the STARLIGHT microscope, Sgró, M. A. Anisotropic Halo Model, 465 401 Sgró, M. A. Determination of Halo Occupation Distri- Schlindwein, W. Accretion disc mapping of the bution, 397 Shahbaz, T. Stellar occultation by the trans-Neptunian shortest period eclipsing binary SDSS J0926+36, 275 Schmidl, S. Mass and energy of GRB-SN events: object 2002 KX14, 195 multi-wavelength analysis of three associations in Shan, HY. The CFHT/MegaCam Stripe-82 Survey, 160 the context of the full sample, 169 Shapiro, I. L. Schmidt, E. Spectral Properties of Narrow Line Seyfert cosmological solutions in the Modified Starobinsky 1 galaxies, 433 inflation, 461 Schmieder, B. Recurrent solar coronal jets induced by Sheen, Yun-Kyeong magnetic emergence, 78 Schneider, D. P. Properties of type Ia supernovae 139 Sicardy, B. Schneiter, M. On the sensitivity of extrasolar mass–loss Sicardy, B. MagAl: A new tool to analise galaxies Stellar Occultations by Transneptunian and Centaurs Objects: results from more than 10 photometric data, 402 Scholz, A. Precise stellar occultation predictions for 39 selected TNOs/Centaurs, 33 rate ranges: HD 209458b a case study, 316 Schoenell, W. Herschel-ATLAS and ALMA: I. A z=1.027 Einstein Ring of Molecular Gas and Dust, inside rich galaxy clusters, 470 Schoenell, W. Gravitational waves and stability of observed events, 29 Sicardy, B. Stellar occultation by the trans-Neptunian The GalileoMobile Project, 189 The SONYC survey: Towards a complete object 2002 KX14, 195 Sicardy, B. census of brown dwarfs in star forming regions, 86 Schreiber, M. R. Imaging polarimetry of the potentially Stellar occultations by trans-Neptunian objects, 224 Sicardy, B. planet-forming circumstellar disk HD 142527. The NaCo view, 30 Study of Pluto’s atmosphere from stellar occultation, 200 Schreiber, M. R. The evolution of protoplanetary disk, Siffert, B. B. 14 The Type Ia Supernova Pipeline for the Javalambre Physics of the Accelerating Universe Schreiber, M. R. White dwarf-main sequence binaries Astrophysical Survey (J-PAS), 466 Sigismondi, C. from SDSS DR8: unveiling the cool white dwarf population, 318 Schroeder, K-P. Effects of enhanced neutrino emission Silva, A. L. Brazilian Participations in the International Astronomical Search Collaboration, 186 on the evolution of low-mass stars, 240 Schulze, S. Silva, A. R. The UV GRB host galaxy luminosity function, 132 Schuster, W. Solar astrometry and the heliometer of Rio de Janeiro, 181 ALS 2883: Analysis of spectroscopic features, 314 Silva, C. Q. A. A photometric study of M67: anchoring Identification and extraction of photo- measurements for the determination of astrophysical metric redshifts of quasars with narrow-band filters, parameters of bright stars, 63 467 Schwartz, M. Silva, G. G. Brazilian Participations in the International Transit Timing Variations analysis in exoplanet host stars, 230 Secco, L. F. Astronomical Search Collaboration, 186 Silva, J. R. P. An observational overview of the rotation 2-Pt. Correlation Function for Luminous Red Galaxies, 464 Seriacopi, D. B. in binary systems, 290 Silva, J. R. P. Envelopes of Evolved Stars: Galactic and Magellanic Clouds B[e] Supergiants, 276 Serio, A. rotations of field evolved stars, 280 Silva, J. R. P. GeMS/GSAOI: from commissioning to operations and science results, 180 Time-dependent nonextensivity arising from the rotational evolution of solar-type stars, 277 Setia Gunawan, D. Y. A. Mass loss from massive stars, Silva, J. S. The IMPACTON project: rotational proper- 291 Sfair, R. Theoretical distribution function for ties of NEAs, 222 Silva, K. M. G. Dust production of the small satellites immersed in the arcs/ring of Saturn, 205 MLS110213:022733+130617: A new eclipsing polar above the period gap, 46 Silva, K. M. G. Probing accretion on the high-magnetized polar RX J1007.5-2017, 312 551 Silva, L. C. P. Sobral, D. Star formation at the edge of the Universe, “Planetário e Teatro Digital Johannes Kepler” and its Institutional Pedagogical Project, 185 Silva, M. P. 336 Sochting, I. K. Huge-LQG- the largest structure in the Theoretical distribution function for rotations of field evolved stars, 280 universe, 157 Silva, P. B. The GalileoMobile Project, 189 Silva, T. da Sodré Jr., L. Evaluation of Learning of Synchronous Sodré Jr., L. Rotation of the Moon Mediated By Computational Resource, 501 Silveira, C. R. Sodré Jr., L. Abundâncias de Zinco em estrelas do Sodré Jr., L. Zone to the Galactic Habitabl

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