EVOLUTION OF THE QUASAR POPULATION AT HIGH REDSHIFT
... First I would like to thank my advisor Xiaohui Fan for his guidance, encouragement, and his friendship. He always inspires me to develop independent thinking and research skills, and to collaborate with others in different fields. Without his support, I could not have done my doctoral work. I am gra ...
... First I would like to thank my advisor Xiaohui Fan for his guidance, encouragement, and his friendship. He always inspires me to develop independent thinking and research skills, and to collaborate with others in different fields. Without his support, I could not have done my doctoral work. I am gra ...
The Observer`s Guide to the Gamma-Ray Burst
... The luminosity, energetics and shape of the γ-ray pulse of a given GRB can reveal clues to the origin of its high-energy emission, and thus its emission process. Of particular importance is whether the γ-rays emitted by llGRBs arise from the same mechanism as high-luminosity GRBs (i.e. from a jet), ...
... The luminosity, energetics and shape of the γ-ray pulse of a given GRB can reveal clues to the origin of its high-energy emission, and thus its emission process. Of particular importance is whether the γ-rays emitted by llGRBs arise from the same mechanism as high-luminosity GRBs (i.e. from a jet), ...
Lyman-alpha imaging of starburst galaxies in the local universe and beyond Matthew Hayes
... review can be found in Kennicutt (1998a). For standard initial mass function (IMF; the mass distribution of stars at zero age)1 , the relative abundance of massive stars is small. Since these stars have very short lifetimes (less than the proto-stellar collapse timescale) ongoing star formation is r ...
... review can be found in Kennicutt (1998a). For standard initial mass function (IMF; the mass distribution of stars at zero age)1 , the relative abundance of massive stars is small. Since these stars have very short lifetimes (less than the proto-stellar collapse timescale) ongoing star formation is r ...
the mass distribution and lifetime of prestellar cores in perseus
... Ophiuchus. In a companion paper to this work (M. L. Enoch et al. 2008, in preparation), we use the comparison of 1.1 mm and Spitzer data to study the properties of embedded protostars. In particular, we examine the bolometric temperatures and luminosities of Class 0 and Class I protostars in Perseus ...
... Ophiuchus. In a companion paper to this work (M. L. Enoch et al. 2008, in preparation), we use the comparison of 1.1 mm and Spitzer data to study the properties of embedded protostars. In particular, we examine the bolometric temperatures and luminosities of Class 0 and Class I protostars in Perseus ...
Galaxy And Mass Assembly (GAMA): Gas Fuelling of Spiral Galaxies
... We quantify the effect of the galaxy group environment (for group masses of 1012.5 to 1014.0 M ) on the current star formation rate (SFR) of a pure, morphologically-selected, sample of disk-dominated (i.e. late-type spiral) galaxies with redshift ≤ 0.13. The sample embraces a full representation of ...
... We quantify the effect of the galaxy group environment (for group masses of 1012.5 to 1014.0 M ) on the current star formation rate (SFR) of a pure, morphologically-selected, sample of disk-dominated (i.e. late-type spiral) galaxies with redshift ≤ 0.13. The sample embraces a full representation of ...
Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H2O
... the comparison indicates that both sources are at far-IR wavelengths point-sources compared with the PACS 9 × 9 spatial resolution (∼1.3 × 1.3 kpc2 for NGC 4418 and ∼3.1 × 3.1 kpc2 for Arp 220). The continua of both sources are shown in Fig. 1, including the Spitzer IRS spectra (Spoon et al. 200 ...
... the comparison indicates that both sources are at far-IR wavelengths point-sources compared with the PACS 9 × 9 spatial resolution (∼1.3 × 1.3 kpc2 for NGC 4418 and ∼3.1 × 3.1 kpc2 for Arp 220). The continua of both sources are shown in Fig. 1, including the Spitzer IRS spectra (Spoon et al. 200 ...
β Relation for Local Galaxies
... a much lower ratio of the b-parameter compared to starburst galaxies. However, the results of Boquien et al. (2009, 2012), and Siebert et al. (2005) do not support the birthrate parameter result; instead, they suggest that the offset may merely be a result of the difference in dust geometry between ...
... a much lower ratio of the b-parameter compared to starburst galaxies. However, the results of Boquien et al. (2009, 2012), and Siebert et al. (2005) do not support the birthrate parameter result; instead, they suggest that the offset may merely be a result of the difference in dust geometry between ...
Watson et al. 2007a - Department of Physics and Astronomy
... Solar- and later-type young stars, and test the standard models of dust processing which result in the conversion of originally amorphous dust into minerals. We find strong evidence of evolution of the dust crystalline mass fraction in parallel with that of the structure of the disks, in the sense t ...
... Solar- and later-type young stars, and test the standard models of dust processing which result in the conversion of originally amorphous dust into minerals. We find strong evidence of evolution of the dust crystalline mass fraction in parallel with that of the structure of the disks, in the sense t ...
Galaxy Formation and Evolution.
... F R A N K VA N D E N B O S C H is Assistant Professor at Yale University, and is known for his studies of the formation, dynamics, and clustering of galaxies. S I M O N W H I T E is Director at the Max Planck Institute for Astrophysics in Garching. He is one of the originators of the modern theory o ...
... F R A N K VA N D E N B O S C H is Assistant Professor at Yale University, and is known for his studies of the formation, dynamics, and clustering of galaxies. S I M O N W H I T E is Director at the Max Planck Institute for Astrophysics in Garching. He is one of the originators of the modern theory o ...
Direct Evidence for Termination of Obscured Star Formation by
... local to the SMBH can (3) heat gas in the ISM, and/or (4) drive gas out of the galaxy via kinetic pressure. Most discussions of AGN feedback condense the four feedback mechanisms described above into two simplified paradigms; ‘quasar’ mode feedback and ‘radio’ mode feedback. Quasar mode feedback ass ...
... local to the SMBH can (3) heat gas in the ISM, and/or (4) drive gas out of the galaxy via kinetic pressure. Most discussions of AGN feedback condense the four feedback mechanisms described above into two simplified paradigms; ‘quasar’ mode feedback and ‘radio’ mode feedback. Quasar mode feedback ass ...
submillimeter observations of giant molecular clouds in the large
... regions N158C, N159, and N160 with a few prominent CO clouds in the J ¼ 2Y1 and J ¼ 3Y2 transitions of CO. They find that the kinetic temperatures are 10Y80 K and the highest temperature is toward 30 Dor. The smallest beam size and grid spacing are 1500 and 1100 , respectively, in the J ¼ 3Y2 emissi ...
... regions N158C, N159, and N160 with a few prominent CO clouds in the J ¼ 2Y1 and J ¼ 3Y2 transitions of CO. They find that the kinetic temperatures are 10Y80 K and the highest temperature is toward 30 Dor. The smallest beam size and grid spacing are 1500 and 1100 , respectively, in the J ¼ 3Y2 emissi ...
University of Groningen Late-type spiral galaxies Ganda, Katia
... 2005) mainly refers to the emission-line properties, to the characteristics of the HII regions or to the nature of the innermost component. In particular, no study has addressed yet in a systematic way the stellar populations of late-type spiral galaxies with a two-dimensional coverage. Existing stu ...
... 2005) mainly refers to the emission-line properties, to the characteristics of the HII regions or to the nature of the innermost component. In particular, no study has addressed yet in a systematic way the stellar populations of late-type spiral galaxies with a two-dimensional coverage. Existing stu ...
http://arxiv.org/pdf/1401.1510v1.pdf
... The flux-limited sub-mm selection ensures a relatively homogenous sample of the most intensely starforming dust obscured galaxies at z & 3: Due to the negative kcorrection, the sub-mm flux detection limit corresponds roughly to a cut in SFR over the considered redshift range. Note that while a fract ...
... The flux-limited sub-mm selection ensures a relatively homogenous sample of the most intensely starforming dust obscured galaxies at z & 3: Due to the negative kcorrection, the sub-mm flux detection limit corresponds roughly to a cut in SFR over the considered redshift range. Note that while a fract ...
Modeling Spatially and Spectrally Resolved Observations to
... This thesis owes much to the support of my officemate, Zach Berta, for five years of advice on life, computers, and astronomy. I thank Diego Muñoz, Robert Harris, Ragnhild Lunnan, and Sarah Rugheimer for countless snack and coffee breaks; Wen-fai Fong and Nick Stone for leading camping trips and t ...
... This thesis owes much to the support of my officemate, Zach Berta, for five years of advice on life, computers, and astronomy. I thank Diego Muñoz, Robert Harris, Ragnhild Lunnan, and Sarah Rugheimer for countless snack and coffee breaks; Wen-fai Fong and Nick Stone for leading camping trips and t ...
Constraints on the physical properties and chemical evolution of star
... constrain the physical properties and chemical enrichment of the gas in galaxies at all cosmic epochs. This is important, because galaxies are being detected at always higher redshift and upcoming observations with large telescopes, such as the James Webb Space Telescope, will gather high-quality sp ...
... constrain the physical properties and chemical enrichment of the gas in galaxies at all cosmic epochs. This is important, because galaxies are being detected at always higher redshift and upcoming observations with large telescopes, such as the James Webb Space Telescope, will gather high-quality sp ...
The 3-D shaping of NGC 6741: A massive, fast
... surrounded by a sharp low-excitation skin (the ionization front), and embedded in a spherical (radius 0.080 pc), almostneutral, high-density (n(H I) 7 × 103 atoms cm−3 ) halo containing a large fraction of the nebular mass (Mhalo ≥ 0.20 M ). The kinematics, physical conditions and ionic structu ...
... surrounded by a sharp low-excitation skin (the ionization front), and embedded in a spherical (radius 0.080 pc), almostneutral, high-density (n(H I) 7 × 103 atoms cm−3 ) halo containing a large fraction of the nebular mass (Mhalo ≥ 0.20 M ). The kinematics, physical conditions and ionic structu ...
