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Adamo, Angela (Stockholm Univ., Sweden) – Contributed Talk
Cluster formation and disruption, the role of the galactic host environment revealed by HST
Less than 30 years ago the launch of the HST established a new field of research focus on young star clusters (YSCs). Galactic and
extragalactic star-forming regions show that the vast majority of stars are formed in clustered environments, with gravitationally bound
YSCs sitting in the densest cores of giant molecular clouds (GMCs). Massive YSCs are commonly formed in local galaxies and could
possibly be linked to the globular clusters, remnants of the extreme star formation process occurred in a much younger and less evolved
Universe. After Servicing Mission 4, the study of YSCs has been revived. The access to sensitive UV detectors with a large field of view
has allowed to survey wider samples of cluster populations. The inclusion of the U-band is crucial for cluster analysis because it breaks
the degeneracy between age and extinction. In my contribution I will focus on the role of the galactic environment in determining the
fraction of stars forming and surviving as bound clusters. There is increasing evidence that the fraction of star formation happening in
bound YSCs (i.e. cluster formation efficiency, CFE) depends on the physical conditions of the galactic environment. If cluster formation
would only be dominated by size-of-sample effect, one would expect the CFE to be constant (the number of clusters increase as
function of increasing star formation rate, SFR, but overall the fraction of star formation happening in star clusters is the same). At the
same time, if clusters are disrupted in spite of their physical properties or the type of environment where they live, one would expect to
not see any trend in their disruption rate. I will present the results achieved with the study of the cluster populations in two grand-design
nearby spiral galaxies, M 83 and M 51. The CFE and cluster disruption has been derived for the whole systems as well as in different
regions of the same galaxy. Overall, these results suggest that the CFE increases as function of SFR densities. Similarly disruption seams
to decrease in the outer regions where the interstellar medium is less dens and shear less strong.
Barstow, M.A. (Univ. Leicester) , S. Preval, S.L. Casewell and J.K.Webb – Contributed Talk
White Dwarfs as probes of fundamental physics and astronomical processes
As the end products of more than 90% of all stars white dwarfs are important objects to study in their own right. However, they also
serve as important laboratories to study fundamental physical and astronomical processes. We present three examples of new results
from our own HST guest observer programmes and archival research:
Recently, we assembled a high spectral resolution and signal-to-noise spectrum of a hot white dwarf, from multiple STIS far-UV calibration exposures, and used it to demonstrate the feasibility of measuring the changes in the value of the fine structure constant in strong
gravity. The upper limit obtained was dominated by uncertainties in the laboratory wavelengths of the spectral lines. Subsequently, we
have obtained a similar data set for a much lower gravity object and use this to provide a set of reference wavelengths, significantly
improving the constraints on the possible fine structure constant variation.
Using STIS, we have obtained Balmer line spectra for a sample of white dwarfs in resolved binary systems from which we can measure
their effective temperature and gravity and an accurate radial velocity, yielding a measurement of the gravitational redshift. Together
these data provide accurate mass and radius determinations capable of testing the theoretical mass-radius relation and distinguishing
between possible structural models.
Surveys of a large sample of hot, H-rich DA white dwarfs show an unexpected diversity in the abundances of photospheric metals that
cannot be explained by differences in the stellar temperature and surface gravity. Measurement of the abundances of C and Si show
that in all cases C is depleted, indicative of a rocky origin for the material. A likely explanation is that the metals in hot DA atmospheres
are accreted from extra-solar planetary debris and then retained in the envelope by radiative forces.
Bean, Jacob (University of Chicago) - Contributed Talk
Exoplanets in HD
The first detection of an exoplanet atmosphere, which was obtained with HST using the technique of transit spectroscopy, is now more
than a decade old. There has been a lot of progress in this area in the intervening years, and detections of many different atoms and
molecules have been reported for a number of exoplanets using a wide variety of ground- and space-based telescopes. However, just
detecting the atmospheres of these planets is not enough anymore. Revealing the fundamental properties of exoplanet atmospheres
to investigate their natures and origins requires high precision spectroscopy. Although HST remains the premier facility for exoplanet
atmosphere observations, more intense observational campaigns are necessary to achieve this goal. I will present results from the first
intensive HST exoplanet atmosphere campaigns that aim to advance this new paradigm. I will begin by describing the unambiguous
conclusions from a Cycle 20 Large program focussed on the super-Earth archetype GJ1214b. I will then present the first outcomes
from an ongoing Cycle 21 Large Treasury program, including data from an attempt to perform phase-resolved spectroscopy of an
exoplanet by continuously observing complete planetary rotation periods. I will conclude with a look forward at how HST observations
can continue to revolutionize this field in the short-term, and how JWST will ultimately usher in a new era by enabling high-precision
measurements of smaller and cooler exoplanets, some of which may resemble Earth.
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Bellini, Andrea (STScI) – Poster # 8
Hubble Space Telescope proper motion (HSTPROMO) of Galactic globular clusters
The stable environment of space makes HST an excellent astrometric tool. Its diffraction-limited resolution allows it to distinguish and
measure positions and fluxes for stars all the way to the center of most globular clusters. Apart from small changes due to breathing, its
PSFs and geometric distortion have been extremely stable over its 20-year lifetime. There are now over 20 globular clusters for which
there exist two or more well-separated epochs in the archive, spanning up to 10 years or more. In addition, new properly designed
observations are being acquired for 47 clusters, 34 of which are currently without prior high-quality second-epoch observations (GO13297, PI: Piotto). Our photometric and astrometric techniques allow us to measure thousands of stars in the central few arcmins
from the clusters’ center, with typical proper-motion errors of ~0.2 mas/yr. These high-quality measurements are crucial in order to
detect the possible central intermediate-mass black hole and put constraints on its mass, in addition to provide direct a measurement
of the cluster anisotropy and equipartition, allow detailed studies of the clusters’ internal dynamics, their distance, their rotation and
many other scientific applications.
Blair, William (Johns Hopkins University) – Poster # 9
HST/WFC3 Observations of the Grand Design Spiral M83: Star Clusters, Supernova Remnants, and More
The face-on grand design spiral galaxy M83 (d=4.6 Mpc) is an actively star-forming galaxy, with spiral arms filled with giant H II
regions and an intense nuclear starburst. The galaxy itself is a veritable supernova factory, having generated six known SNe in less
than 100 years. Hence, one might expect of order 60 or more supernova remnants (SNRs) less than a thousand years old, as well
as many older SNRs dominated by ISM emission. Our cycle 19 program seeks to understand the entire stellar lifecycle on a galactic
scale, connecting clusters and star formation properties to the SNRs and X-ray properties of this fascinating galaxy. Many on our team
have also obtained deep Chandra data for this galaxy (729 ks), with widespread diffuse emission and over 440 point X-ray sources
identified to date. We have obtained HST/WFC3 UVIS and IR camera emission-line and broadband data for seven fields covering the
bulk of the bright optical disk of M83. We have identified over 3000 star clusters, from the youngest forming clusters to old globulars.
The emission-line data have yielded new information on the SNR population, in particular allowing the characterization the smallest
diameter objects not resolvable from the ground (1”=22 pc at M83). We are finding the use of [Fe II] 1.644 micron emission to be
an important new diagnostic for finding SNRs in addition to the usual criteria. In total, nearly 300 SNRs have now been identified, and
we are working to characterize the stellar populations near many of them, and in some cases constrain the properties of the precursor
stars. While we have identified ~65 optical SNR candidates with angular sizes below 0.5” (<11 pc), we are not finding the expected
population of ejecta-dominated young SNRs, with the singular exception of the very young remnant of SN1957D. Rather, most of
the young SNRs appear to have quickly evolved into the radiative phase. Gemini-S GMOS spectra of selected objects confirm the
lack of observed high velocities or obvious ejecta-enhancement of abundances. This unexpected result implies that the CSM/ISM
environments for most young remnants in M83 are very dense, perhaps due in part to enhanced mass loss from the precursor stars
due to the super-solar metal abundances in much of this galaxy. We will show representative data from all relevant data sets that lead
us to this conclusion. This work is supported in part by STScI grant HST-GO-12513.01-A and Chandra grant SAO-GO1-12115C to
Johns Hopkins University.
Brammer, Gabriel (STScI) – Poster # 27
Spectroscopic Constraints on z > 10 Galaxy Candidates with the WFC3/IR Grisms
Extremely deep imaging surveys with ACS and WFC3/IR have uncovered large samples of galaxies in the very early universe, including
a relatively small but exciting sample of galaxy candidates at z > 10. Spectroscopic confirmation of the redshifts of these objects (and
rejecting interlopers) is critical for robust characterization of the rapidly-evolving galaxy population less than ~500 Myr after the Big
Bang. Potential low-redshift contaminants of these high redshift samples are galaxies with extreme emission-line equivalent widths
that can mimic the far-UV Lyman break. With 17 orbits of WFC3 grism observations in the Hubble Ultra-Deep Field, indeed we marginally detect an emission line for the faint z~12 candidate UDFj-39546284 and argue that it is more likely an [OIII]-emitter at z~2.
However, for a surprisingly bright sample of recently-discovered z~10 candidates, grism exposures of just two orbits are sufficient to
place strong constraints against the low-redshift emission line hypothesis and favor the high-redshift interpretation of those galaxies.
Future deep HST/WFC3 grism integrations of ten orbits or more can actually detect the continuum Lyman break for unambiguous
redshift confirmation of bright z~10 candidates, paving the way for JWST in a regime currently utterly unaccessible from the ground.
Cacciari, Carla (INAF, Osservatorio Astronomico Bologna) – Poster # 30
Gaia
The ESA mission Gaia, launched on 19 December 2013, will perform an all-sky survey to V=20 providing astrometric data of
unprecedented accuracy for about one billion sources, as well as spectro-photometry, and medium resolution spectroscopy (to V=17).
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This promises to provide a major breakthrough in the understanding of the many aspects related to the Galaxy structure, formation
and evolution, as well as on issues of cosmological importance. The general characteristics and expected performance of Gaia will be
described, and an update will be presented based on the available information from commissioning activities.
Calamida, Annalisa (STScI) – Contributed Talk
The white dwarf cooling sequence of the Galactic bulge
We present F606W,F814W (V,I)-band time-series data of ~1 million stars in the low-reddening Sagittarius window in the Galactic
bulge. Images were collected with the Advanced Camera far Surveys (ACS) and the Wide Field Camera 3 mounted on the Hubble
Space Telescope. The total field of view is ~ 17x18 arcminutes, which was observed approximately every two weeks for two consecutive years, with the principal aim to detect a hidden population of isolated black holes and neutron stars in the Galactic disk through
astrometric microlensing.
Here we present results based on the combined deep images of the four ACS fields. The final photometric catalog of ~ 1 million stars
reaches down to V ~ 31 mag. Proper motions were also measured, with an accuracy of better than ~ 0.15 mas/yr at V ~ 26 mag
in both coordinates. We were then able to separate disk and bulge stars and obtain a clean bulge color-magnitude diagram. Together
with several candidate extreme horizontal branch (EHB) stars we were able to identify for the first time a clearly defined white dwarf
(WD) cooling sequence in the bulge. The comparison between theory and observations shows that a substantial fraction of the WDs
is systematically redder than the canonical cooling tracks for CO-core WDs. This evidence would suggest the presence of He-core
WDs in the Galactic bulge, formed in close binaries, as has been found in the disk and in a few Galactic globular and open clusters.
The presence of close binaries in the EHB and WD bulge population is further supported by the finding of five cataclysmic variable
candidates, two EHB ellipsoidal variables, and a dwarf nova in outburst in one of the ACS fields.
Calvi, Valentina (STScI/Univ. Padova) – Poster #21
The Effects of Surface Brightness Dimming in the Selection of High-z Galaxies
Surface brightness (SB) dimming affects all cosmological sources in the form (1+z)4 . The strong dependence of SB dimming with
increasing redshift suggests the presence of a selection bias when searching for high-z galaxies, i.e. we tend to detect only those
galaxies with a high SB. We made use of the GOODS, HUDF, and XDF Hubble Space Telescope legacy data-sets to study the SB
dimming effect predicted by cosmology, including the effects of clumpiness within the high-z galaxies. We selected a sample of Lymanbreak galaxies at z~4 (i.e. B-band dropouts) detected in all of the data-sets and found no significant trend when comparing the total
magnitudes measured from images with different depth. The study of cosmological SB dimming is also important since it could affects
our prediction of what JWST can observe at higher redshifts, where younger galaxies may exhibit a larger fraction of clumpiness. Our
direct comparison shows that galaxies detected in GOODS do not become significantly brighter in the HUDF or XDF. This suggest that
most of their light is compact and hints to the fact that JWST will likely not find diffuse star forming components.
Carpenter, K.G (NASA/GSFC) and Ayres, T.R. (UCO), for the ASTRAL Science Team – Poster #4
Minting and Mining Stellar Spectra in the Hot and Cool Star HST Treasury “Advanced Spectral Library (ASTRAL)” Programs
Over the past three years, two of the largest-ever HST stellar spectroscopic Guest Observer programs have been undertaken. The
“Advanced Spectral Library (ASTRAL)” Project (PI = T. Ayres) consists of two Treasury Programs, the first in Cycle 18 on “Cool Stars”
(GO-12278) and the second in the current Cycle 21 on “Hot Stars” (GO-13346). These programs are designed to collect a definitive
set of representative, high-resolution (R~30,000-100,000), high signal/noise (S/N>100) spectra, with full UV coverage (~1200 3000 A) of prototypical stars across the HR diagram, utilizing the high-performance Space Telescope Imaging Spectrograph (STIS).
These data will enable investigations of a broad range of problems -- stellar, interstellar, and beyond -- for many years into the future.
ASTRAL/Cool Stars obtained spectra of eight F-M evolved late-type stars, including iconic objects like Betelgeuse and Procyon.
ASTRAL/Hot Stars is in the process of observing 21 early-type stars, which span a broad range of spectral types between early-O
and early-A, both main sequence and evolved stars, fast and slow rotators, as well as chemically peculiar and magnetic objects. The
targets include equally iconic Sirius, Vega, and the classical wind source Zeta Puppis. All of these extremely high-quality STIS UV echelle
spectra will be available from the HST archive and, in post-processed and merged form, at http://casa.colorado.edu/~ayres/ASTRAL/.
Here, we summarize the overall content and design of the observing programs and the spectra now available for community use;
and then present some detailed illustrative examples of datasets and the on-going scientific analyses. The examples will include: (1)
discussions of the very rich spectra of the two evolved M stars in the sample, the M3.4 giant Gamma Crucis (GaCrux) and the M2Iab
supergiant Alpha Orionis (Betelgeuse), and the ways in which they facilitate the study of the outer atmospheres and winds of cool, lowgravity stars; (2) and a “first look” at one of the earliest datasets to come out of the Hot Star program, a “high definition” UV spectrum
of the magnetic chemically peculiar “Ap” star HR 465; and (3) others targets and science as time permits.
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Casertano, Stefano (STScI), Riess, Adam (STScI/JHU), and the SHOES team
– Contributed Talk
High precision parallax measurements with the Perpendicular Spatial Scan mode of WFC3
We present preliminary results from a new observing method that takes advantage of the Perpendicular Spatial Scan capability of WFC3
to obtain high-precision parallax measurements for Galactic Cepheids. This mode allows much more accurate one-dimensional position
measurements for sufficiently bright targets than possible with either imagers or the FGS on HST. We estimate a final parallax accuracy
ranging from 20 to 40 micro-arcseconds, or a single-target distance accuracy of ~ 5% at 1-2.5 kpc for an optimally observed target,
using four or five orbits of HST time per target. When complete in early 2015, our program will obtain distance measurements for 18
long-period Galactic Cepheids, which will form the best available calibrator for the local value of the Hubble constant (expected error
~ 2%) until the completion of the GAIA mission.
Achieving the desired accuracy requires careful planning and a thorough understanding of the peculiarities of both WFC3 and of
guiding with HST.
We will describe the key elements for successful observations and analysis, including choices of filter and scan rate, consideration
of the number and density of reference stars, time- and filter-dependent changes in the geometric distortion, and correction for
micro-rotations in the HST reference frame. As the required precision of ~0.001 pixels exceeds what can be achieved with direct
observations, many of these elements require extensive analysis of available spatial scan calibration observations and/or self-calibration
from the data themselves.
We will also present a preliminary parallax value and a discussion of statistical and systematic accuracies for the first target, for which
observations have been completed in August 2013.
Cepollina, F. (NASA GSFC), & Pellegrino, J. (ATK Space Systems) – Contributed Talk
The Flagship Observatory for the Next Generation: 20-meter Telescope
Over the years NASA has used the majority of its space assets and resources to further the scientific discovery of the universe, and
appropriately so.
As we look forward to the future – past the achievements of Hubble and even beyond the anticipated success of James Webb – we
can envision a future in which very-large-diameter observatories will continue this legacy of great international space observatories.
In this paper, we propose a concept for implementing the design of a 20-meter telescope that leverages NASA’s current and anticipated
advancements in space transportation as well as astronaut on-orbit assembly and maintenance, augmented by robotically controlled
space-system elements. Such an architecture would draw on the development of Orion and the SLS heavy-lift vehicle and also the
experience gained through previous servicing and assembly missions, particularly those to the Hubble Space Telescope and the
International Space Station. Confidence in this approach is bolstered by recent technology advancements in autonomous navigation
and docking, robotics and on-board high speed computing, as well as demonstrations such as the Robotic Refueling Mission on the
International Space Station.
Christian, C. (STScI); Nota, A. (ESA/ STScI); Grice, N. (You Can Do Astronomy LLC);
Greenfield, P. (STScI); Shaheen, N. (National Federation of the Blind, Jernigan Institute);
Sabbi, E. (STScI) – Poster # 12
You Can Touch These! HST images come to life through 3D tactile models
For nearly 24 years, Hubble Space Telescope has dazzled the public and science community alike with spectacular imagery and
amazing discoveries. The mission also has a long history of providing exemplary education and outreach materials based on that
HST research thereby contributing to public understanding of astronomy and enthusiasm for science. We now extend the suite of
HST multimedia resources to the tactile world. In this presentation, we describe our new innovative process for transforming Hubble
images into tactile 3D models. This unique tool is designed especially to make astronomy accessible and understandable to visually
impaired individuals. Our initial process was developed using multicolor images of stellar clusters for which we transformed scientific
measurements of scale, intensity and distance for each aspect of a star formation region (gas, dust, filamentary structure, stars etc.)
into a format compatible with 3D printers. The data are sliced into layers that represent different distances and then fitted together, so
that the user can explore the structure of the astronomical object with their fingertips, slice-by-slice, analogous to a visual fly-through
from near to far. Students will be able to identify and spatially locate the different components of these complex astronomical objects,
namely gas, dust and stars, and will learn about the formation and composition of stellar clusters. The primary audiences for the 3D
models are middle school and high school blind students and, secondarily, blind adults. However, we believe that the final materials will
address a broad range of individuals with varied and multi-sensory learning styles, and will be interesting and visually appealing to the
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public at large. Our process is aimed at automation so that in the future, we can export HST data in 3d printer format so that anyone
can produce these tactile materials in their home or classroom.
Cignoni, M. (STScI), Sabbi, E. (STScI), and the HTTP Collaboration – Poster # 14
Dissecting the starburst: spatially resolved star formation in the Tarantula Nebula
The aim of this work is to decipher the complex star formation history of the most active star forming region in the Local Group, the
Tarantula Nebula in the Large Magellanic Cloud, taking advantage of the unique multi-wavelength data set recently assembled within
the Hubble Tarantula Treasury Project (HTTP), an Hubble Space Telescope imaging survey designed to resolve stars down to the
sub-solar mass regime (< 0.5 Mo) for the entire Nebula. As part of the effort to exploit these data, we compare the observational
Color-Magnitude Diagrams with synthetic ones generated using isochrones from theoretical stellar libraries. Chief results of this analysis
involve: (i) Spatial patterns of star formation, (ii) Time scale of star formation, (iii) Role of massive stars in the star formation process,
(iv) reddening maps of the region.
Coe, Dan (STScI) – Contributed Talk
Gravitationally Lensed Hubble Images Measuring Cosmic Evolution from 400-600 Myr
The first galaxies are a frontier of extragalactic astronomy. How and when did they form, and how did they contribute to reionization?
Answers to these questions require both census taking and detailed studies of individual galaxies. Gravitationally lensed Hubble WFC3/
IR imaging has enabled efficient discovery of galaxies in the first 600 million years (z > 8.5). The Cluster Lensing And Supernova
survey with Hubble (CLASH) Multi-Cycle Treasury program revealed galaxies as distant as MACS0647-JD at z ~ 10.8 (420 Myr).
Upcoming HST WFC3/IR grism spectroscopy should help confirm this z ~ 11 discovery, and deep Spitzer imaging will constrain the
galaxy’s age, stellar mass, and rest-frame UV slope (beta). Searches for additional z ~ 10 candidates have so far revealed fewer than
expected. This z ~ 10 deficit suggests more rapid buildup in galaxy numbers and cosmic star formation rate density during the first
600 million years than at later times. Improved statistics to confirm or controvert this deficit are forthcoming from the Frontier Fields
program. By the time of this meeting, two strongly-lensed Hubble Frontier Fields images will be our deepest images of the universe to
date, probing nJy sources. To complement these deep 140-orbit images, a large new HST program should obtain shallow (few orbit)
WFC3/IR imaging of many (~100) strong lensing clusters to reveal z ~ 8.5 candidates as bright as 24th magnitude, enabling detailed
follow-up study with current facilities. Wide field surveys such as Euclid and WFIRST-AFTA will further complement these high-redshift
searches. Together, these programs will significantly advance our understanding of galaxy evolution at z > 8.5 while providing promising
targets for JWST.
Correnti, Matteo (STScI) – Poster # 11
What Causes Extended Main Sequence Turn-offs in Intermediate-Age star clusters?
Recently, extended main sequence turn-offs (eMSTOs) have been found in many intermediate-age (1-2 Gyr) star clusters in the
Magellanic Clouds. In addition to eMSTOs, some clusters were recently found to exhibit striking composite clumps of red giants,
which represent a strong argument in favor of the interpretation that eMSTOs are due to stars formed at different times within the
parent cluster, with age spreads of 150-500 Myr. In this context, I will present results obtained from the analysis of deep two-colour
HST WFC3 UVIS photometry (cycle 20 HST program GO-12908) for two Magellanic Clouds cluster, namely NGC 2209 and NGC
2249. These two clusters are an ideal benchmark to understand the actual physical conditions necessary for the onset of eMSTO
and multiple populations. In fact, from the photometric evidence available to date, two distinct scenarios have emerged to explain the
eMSTO phenomenon: eMSTO are only hosted by intermediate-age clusters with core radii larger than a certain large value (r_c >
3.7 pc) or eMSTO can only be hosted by clusters for which the escape velocity of the cluster was higher than the wind velocities of
the stars thought to provide material used to form the second generations at the time such stars were present in the cluster (at ages
of ~ 5-30 Myr for massive stars and ~ 50-200 Myr for IM-AGB stars). The results obtained from these two clusters, for which the
properties (core radii, escape velocity) are such that the two scenarios mentioned above give opposite predictions as to the presence
of an eMSTO, will be discussed together with the possible implications in our understanding of the physical conditions responsible for
the onset and retention of multiple populations in star clusters.
Crenshaw, D.M. (Georgia State University) – Poster # 22
AGN Winds and their Importance for Feedback
AGN provide feedback to their environments via mass outflows of ionized gas, which likely play a critical role in the formation of
large-scale structure in the early Universe, chemical enrichment of the intergalactic medium, and self-regulation of supermassive black
hole and galactic bulge growth. These winds are often detected via blueshifted UV absorption lines from the nucleus or from spatially
resolved optical emission lines in the narrow-line region on scales of hundreds of parsecs. We use HST observations of nearby AGN
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with STIS, COS, and WFC3 to constrain the geometry and physical conditions in the outflows and measure their mass outflow rates
and kinetic luminosities, in order to gauge their importance for providing significant AGN feedback. Near and mid-IR imaging and
spectroscopy with JWST will allow us to probe the kinematics of circumnuclear regions and entire objects with high dust extinctions,
to look for signatures of inflowing gas, as well as outflows, to derive a complete physical picture of the mechanisms of feeding and
feedback in AGN.
Dalessandro, Emanuele (Univ. Bologna) - Poster # 10
The WFPC2 UV survey: the Horizontal Branch morphology of Galactic globular clusters
We present accurate far-UV and optical photometry obtained with the WFPC2 and ACS/SBC cameras on board the HST for more than
40 Galactic globular clusters (GGCs). Far-UV color-magnitude diagrams (CMDs) are the most efficient tools to study hot populations in
old stellar systems and to perform meaningful and detailed comparisons with theoretical models. In particular, far-UV CMDs allow to
put severe constraints on the role played by Helium in shaping the Horizontal Branch (HB) morphology in GGCs and, more in general,
on the so called “HB second-parameter problem”. In this context we will show in detail two examples: the massive cluster NGC 2808
and the “historical second-parameter pair “ at intermediate metallicity, M3 and M13. In addition, taking advantage of the photometric
homogeneity of our data-set, we will present the effective temperature extent and distribution of HB stars in our GGC sample, as
inferred from far-UV CMDs. We will show the results of a multi-variate analysis connecting the HB effective temperature to other cluster
parameters.
Dalla Bonta’, Elena (Univ. Padova) – Poster # 18
The Fundamental Plane of Abell 1689
We carried out a photometric analysis of a sample of early-type galaxies in Abell 1689 at z=0.18, using Hubble Space Telescope
Advanced Camera for Surveys archive images in the rest-frame V-band. We performed a two-dimensional photometric decomposition
of each galaxy surface-brightness distribution using the GASP2D fitting algorithm. We adopted both a Sérsic and de Vaucouleurs law.
S0 galaxies were analyzed also taking into account a disc component described by an exponential law and bars of SB0 galaxies were
described by the profile of a Ferrers ellipsoid. The derived photometric parameters have been used to quantify how the Fundamental
Plane of Abell 1689 is affected by the use of different photometric laws.
Danhoni Neves, Marcos Cesar (State University of Maringa) – Poster # 1
The cigoli-galilei codex: an heliocentric madonna in lodovico cardi´s radical anamorphosis
Relationships between Art and Science hailing from the friendship between Lodovico Cardi (Cigoli) and Galileo Galilei are investigated,
especially by analyzing the books Sidereus Nuncius and Istoria e Dimostrazione sulle macchie Solari e loro accidenti and the painting
The Assumption of the Virgin. The codex that the artist and the scientist covertly inscribed in the painting The Assumption of the Virgin
to strengthen the Copernican theory and the new science therein derived is studied. Keywords: Cigoli, Galileo, Codex, Copernicanism,
heliocentrism. ,
De Marchi, Guido (ESA/ESTEC) – Poster # 13
The extinction law inside the 30 Doradus nebula
We have studied the interstellar extinction in a field of ~ 3' × 3' at the core of the 30 Doradus nebula, including the central R 136
cluster, in the Large Magellanic Cloud (LMC). Observations at optical and near-infrared (NIR) wavelengths, obtained with the WFC3
camera on board the Hubble Space Telescope, show that the stars belonging to the red giant clump are spread across the colour–
magnitude diagram because of the considerable and uneven levels of extinction in this region. Since these stars share very similar
physical properties and are all at the same distance, they allow us to derive the absolute extinction towards about 150 objects and the
extinction law in the range 0.3 − 1.6 μm. At optical wavelengths, the extinction curve is almost parallel to that of the diffuse Galactic
interstellar medium, but the value of Rv = 4.5 ± 0.2 that we measure indicates that there is a grey component with a larger fractions
of large grains. At wavelengths longer than ~ 1 μm, the contribution of the grey component tapers off as ^{−1.5}, like in the Milky
Way, suggesting that the nature of the grains is otherwise similar to those in our Galaxy. This extinction law leaves no doubt that in these
regions large grains are more important than in the diffuse Galactic ISM, suggesting that in star-forming regions grains are generally
larger, large grains are more frequent, or both. We are now extending these studies to a large portion of the Tarantula nebula using
existing HST observations at ultraviolet, optical and near infrared wavelengths.
Diaz, Rosa (STScI) – Poster # 36
JWST Science Operations Design Reference Mission: one year into JWST observations
The James Webb Space Telescope (JWST) will enable scientific breakthroughs, much like HST. As we approach our scheduled 2018
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launch, HST users should look closely to the scientific goals of JWST and identify science opportunities and those areas yet not explored
by HST that will enhance JWST science and that will greatly impact many of the themes we research today. The Science Operations
Reference Mission (SODRM) is a suite of realistic JWST science programs that cover the main scientific themes of the observatory.
STScI is using the SODRM to guide development of the JWST ground system, but the contents of the SODRM also highlight science
observations well suited to the capabilities of JWST. We summarize the contents of the SODRM, both scientifically and in terms of
instrument capabilities. We provide a more detailed look at specific SODRM programs to illustrate the typical planning and observing
sequence for JWST.
Disney, Mike (Univ. of Cardiff) – Poster # 28
Reionisation and the tolman universe
Before launch it was confidently expected that HST would see few if any galaxies beyond redshift 2 because of Surface –Brightness
[SB] dimming by a factor of , the ‘Tolman Effect’, which amounts to 9 magnitudes at z = 7. A Milky Way should fall completely beneath
the sky at z =1.2. Yet deep fields reveal high-z galaxies aplenty. What can be gong on? It cannot be the consequence of dramatic
Evolution because stellar population studies in nearby galaxies show that their star-formation has been steady, not falling dramatically.
We suggest that the high z (> 1) Universe is indeed dominated by Tolman dimming which hides the great majority of galaxies from
sight. What we do see are completely different populations from different redshifts, intrinsically higher SB but smaller populations farther
back in the past. Such a very different ‘Tolman Universe’ explains many puzzles: why the observed SBs of galxies are independent of
redshift; why high-z galaxies are physically small; ‘Downsizing’ i.e. lower luminosity galaxies apparently forming later; inexplicable numbers
of QSOALs at high redshift; ‘Infant Mortality’ i.e. less young galaxies than galaxies born; Red Nuggets; but above all ‘The Reionisation
Problem’. In a Tolman Universe only a small fraction of the galaxies at any redshift will be detectable individually, the rest being hidden
below the sky, where their diffused light could none-the-less re-ionise the Universe. Because of Surface Brightness selection-effects
deep fields only provide microtone slices of the total galaxy population, different at each redshift.
Paul D. Feldman(1), Harold A. Weaver(2), Michael F. A’Hearn(3), Michael R. Combi(4), and
Neil Dello Russo(2) – Contributed Talk
(1) Department of Physics and Astronomy, The Johns Hopkins University,
3400 N. Charles Street, Baltimore, Maryland 21218, USA
e-mail: [email protected] (2) Space Department, Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 207236099, USA
(3) Astronomy Department, University of Maryland, College Park, MD
20742, USA (4) Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, Ann Arbor, MI 48109, USA
Far-ultraviolet Spectroscopy of Comets C/2009 P1 (Garradd) and 103P/Hartley 2 with the Cosmic Origins Spectrograph on the Hubble Space Telescope
We report on sensitive far-ultraviolet spectroscopy at 1 A spectral resolution of two recent comets with the Cosmic Origins Spectrograph
(COS) on HST. Comet 103P/Hartley 2 was observed on three dates surrounding the time of the EPOXI spacecraft fly-by on 2010
November 4. Comet C/2009 P1 (Garradd) was observed on 2012 January 18. For both comets, the principal objective was to
determine the relative CO abundance from measurements of the CO Fourth Positive system in the spectral range of 1400 to 1700
A. Nineteen bands of this system were clearly identified in C/2009 P1. The comet’s water production rate was derived from nearly
simultaneous STIS observations of the OH (0,0) band at 3085 A, and the derived CO/H2O production rate ratio of ~20% makes
this an extremely CO-rich comet. In contrast, the CO bands were extremely weak in 103P/Hartley 2, a highly evolved Jupiter-family
comet, and the CO/H2O ratio was found to be of the order of 0.3% (Weaver et al, ApJ 734, L5, 2011). In both comets strong partially
resolved emission features due to multiplets of S I, centered at 1429 and 1479 A, and multiplets of C I at 1561 and 1657 A, were
observed. In addition, the S I intercombination multiplet, also at 1479 A, is clearly resolved from the neighboring allowed transition,
although its excitation mechanism remains unclear.
Ferraro, F.R. (Univ. di Bologna) – Contributed Talk
An empirical clock to measure the dynamical age of stellar systems
The definition of reliable clocks able to measure the age of cosmic structures is a crucial task in Astrophysics, but only a few chronometers are currently known in the Universe. The most famous is the luminosity of the main sequence turn-off point, to measure the
chronological age of stellar aggregates. However, this quantity alone is unable to fully characterize the global evolution of a system:
indeed, stellar clusters with the same chronological age can have experienced quite different levels of dynamical evolution.
By using the radial distribution of Blue Straggler Stars in a sample of ~20 Galactic globular clusters, we recently defined the first
empirical clock able to measure the dynamical age of stellar aggregates from pure observational properties (Ferraro et al. 2012,
Nature, 492, 393). A crucial role in the derivation of these results has been played by the HST: high-resolution imaging, especially
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in the near-ultraviolet, has been crucial to properly obtain complete samples of Blue Straggler stars in the central regions of even the
most concentrated globular clusters. We present the state of the art results about Blue Straggler stars in Galactic globular clusters and
their crucial role in clarifying the internal dynamical processes occurring in these highly collisional stellar systems
Fischer, Travis (Dept. of Physics & Astronomy, Georgia State University) – Poster #23
Determining AGN Inclinations via Narrow-Line Region Kinematics
Active Galactic Nuclei (AGN) are axisymmetric systems to first order; their observed properties are likely strong functions of inclination
with respect to our line of sight. However, except for a few special cases, the specific inclinations of individual AGN are unknown. We
have developed a promising technique for determining the inclinations of nearby AGN by mapping the kinematics of their narrow-line
regions (NLRs), which are often easily resolved with Hubble Space Telescope (HST) [O III] imaging and long-slit spectra from the Space
Telescope Imaging Spectrograph (STIS). Our studies indicate that NLR kinematics dominated by radial outflow can be fit with simple
biconical outflow models that can be used to determine the inclination of the bicone axis, and hence the obscuring torus, with respect
to our line of sight. We present NLR analysis of 53 Seyfert galaxies, resultant inclinations from models of 17 individual AGN with clear
signatures of biconical outflow, and strong correlations discovered between inclination and neutral hydrogen column density, infrared
color, and H Beta full-width at half maximum (FWHM). These correlations provide evidence that the orientation of AGN with respect
to our line of sight affects how we perceive them.
Biconical outflow may still exist in a portion of the remaining targets if the required kinematic components for our models are not
visible because they are too compact, obscured, or convolved with other components like rotation. Employing infrared Integral Field
Unit (IFU) observations, available via ground-based observatories and the forthcoming Near-Infrared Spectrograph (NIRSpec) aboard
the James Webb Space Telescope (JWST), would allow us to analyze the kinematics of [S III] 0.9533 &#956;m emitting gas, which
originates in the same gas that emits [O III] observable in HST long-slit optical spectra, avoiding extinction problems present at optical
wavelengths and allowing us to observe the full extent of biconical outflows. In addition, mapping the kinematics of NLRs prove to be
more efficient with IFUs as a single observation would require multiple HST/STIS long-slit observations to replicate the resultant spectral
map of the NLR and surrounding areas.
Fontana, Adriano, A Grazian, et al. (INAF Roma) – Contributed Talk
The assembly of massive galaxies from HDF to CANDELS
Reconstructing the process of stellar mass assembly in galaxies is one of the major challenges of modern astrophysics. The extragalactic
deep surveys executed with the Hubble Space Telescope have been a major tool not only to detect galaxies at the highest redshift
but also - crucially - to estimate their stellar mass and other rest-frame properties.
After briefly reviewing the previous achievements of HST in this context, I will present the latest results obtained in the framework of the
CANDELS survey. Thanks to its exquisite combination of spatial resolution, image depth and near--IR spectral coverage, the CANDELS
data allows us to constrain with unprecedented accuracy a number of observables that are crucial to reconstruct the evolution of
galaxies in the first Gyrs: the galaxy stellar mass function at z>4; the number of low mass galaxies at z~2; the number density and
nature of quiescent galaxies at z>2; the star-formation properties and star-formation histories of LBG and other sources at z>3. I will
finally show why the combination of these results depict a scenario that challenges the most recent predictions of theoretical models
of galaxy evolution.
Grillo, Claudio (Niels Bohr Inst., Denmark) – Contributed Talk
The successful synergy between HST and VLT: accurate strong lensing modeling in the CLASH and Frontier Fields cluster MACS
J0416-2403
I will present a detailed mass model of the CLASH and Frontier Fields galaxy cluster MACS J0416-2403 that can predict the observed
positions of 30 multiple images, belonging to 10 spectroscopically confirmed lensing systems, with an unprecedented accuracy. By
taking advantage of the observations in the 16 HST/ACS and WFC3 bands of the CLASH program, we have been able to identify
the most important strong lensing systems present in this cluster. Our large spectroscopic follow-up program with the VLT/VIMOS has
allowed us to measure the redshifts of these systems over a range between 1.9 and 3.2. We have combined the multi-band HST
photometry with the VLT spectroscopic observations to select and model the mass distribution of ~500 candidate cluster members
residing in the inner regions of the cluster. This refinement in the cluster mass modeling is the origin of the extraordinary multiple image
reconstruction. I will show the new results on the model-predicted central mass profile and magnification maps of the cluster. These
are the essential elements to push forward the exploration of the distant Universe within the current Frontier Fields initiative and before
the advent of JWST.
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Grogin, Norman.A. (STScI) and the STScI ACS Team – Poster # 35
Twelve Years with the Advanced Camera for Surveys : Looking Back and Looking Forward
Installed during Servicing Mission 3B in 2002 and repaired during Servicing Mission 4 in 2009, the Advanced Camera for Surveys
(ACS) remains a crucial workhorse imager for HST after twelve years on orbit. The ACS Team at STScI continues to labor intensively
to provide the HST community with the highest level of data from the ACS instruments. We review ACS developments since the prior
status report at the HST3 Conference in 2010, with particular focus on innovative measures to mitigate the steadily degrading charge
transfer efficiency of the Wide Field Channel. These include post-readout pixel-based correction in our calibration software, and prereadout implementation of LED flash. We also summarize some of the recent science highlights with ACS, as well as planned/ongoing
large programs relying on ACS, such as the HST Frontier Fields.
Henry, Alaina (GSFC) – Contributed Talk
Low Masses and High Redshifts: The Evolution of the Mass-Metallicity Relation
The mass-metallicity relation in galaxies is sensitive to the exchange of gas between galaxies and the intergalactic medium. As such,
observations of this correlation constrain the feedback processes that regulate the growth of galaxies. While early studies focusing on
relatively massive (M>10^9.5 Msun) high-redshift galaxies have found lower metallicities than are seen locally, constraints on the low
mass evolution have been slower to develop. Yet it is at low masses that the effects of star formation feedback are the strongest, and
observations have the most leverage to test theoretical models. HST WFC3 grism observations, with their unprecedented sensitivity
to faint, high-redshift star-forming galaxies, offer the ideal solution to this challenge. Combining UDF and WISP data, I will present new
measurements of the z~1.8 mass-metallicity relation, reaching stellar masses 30 times lower than previous robust measurements.
With these data, we make new tests for evolution of the mass-metallicity-SFR plane at high redshifts and low masses. Finally, I will
show how these observations can be used to test theoretical models where gas inflow, outflow, and star formation form an equilibrium.
Kirshner, Robert P. and the RAISIN Team* (Harvard University)- Contributed Talk
RAISIN: SN IA in the IR-- the best route to knowledge of cosmic expansion
In Cycle 20, the RAISIN Team has observed 24 Type Ia supernovae in the restframe infrared using the infrared channel of the Wide
Field Camera on HST. These supernovae were discovered with Pan-STARRS, verified with MMT, Magellan, Keck, or Gemini, and
then placed into the HST schedule as non-disruptive targets of opportunity. A series of observations with the infrared channel of WFC
established the infrared light curve for each of our targets. Ground-based observations of nearby supernovae in the NIR, carried out
by the Carnegie Supernova Project and by the CfA Supernova Program have established that SN Ia are more nearly standard candles
in the y, J, and H bands. What’s more, the vexing problems introduced by conflating dust absorption and intrinsic color variations in SN
Ia are reduced in the infrared. The result is more precise and more accurate distance determination to each event, leading to more
reliable knowledge of the cosmic expansion history and of the inferred properties of dark energy. The RAISIN program shows that a
more comprehensive program of NIR observations could lead to the world’s best determination of dark energy properties. JWST will
be a superb tool for exploring the near-IR of more distant supernovae and providing a thorough test of the physical ideas that have
been advanced to explain why SN IA are such good standard candles in the NIR.
The Co-investigators of RAISIN include:
Robert Kirshner, Peter Challis, Ryan Chornock, Ryan Foley, Wendy Freedman, Andrew Friedman, Joshua Frieman, Peter Garnavich, Eric Hsiao, Mark Huber,
David Jones, Kaisey Mandel, Howie Marion, Gautham Narayan, Bob Nichol, Mark Phillips, Armin Rest, Adam Riess, Steven Rodney, Masao Sako, Chris Stubbs,
John Tonry, and Michael Wood-Vasey,
Kubo, Mariko (Astronomical Institute Tohoku University), Poster # 19
Formation of massive early-type galaxies in the protocluster at z=3.1
We have studied the protocluster at z=3.09 in the SSA22 field by using the deep and wide near-infrared (NIR) imaging and spectroscopic data obtained with Subaru MOIRCS. We first selected the candidate protocluster galaxies by using the photometric redshifts
based on the spectral energy distribution (SED) and found significant density excess of the galaxies at z_phot~2.6-3.6. We also
conducted the NIR spectroscopic observations. A large fraction of the candidates are certainly the protocluster members at z=3.043.12. We also confirmed massive quiescent galaxies and plausible multiple mergers in the SSA22 protocluster. First, we found that
the reddest five galaxies (J-K_AB>2.4) confirmed as the protocluster members have the SEDs dominated by old stellar populations
(Burst like star-formation, Age>1.4 Gyr, specific SFR <0.2 and stellar mass ~10^11 M_sun). This may be for the first time to show
the association of the massive quiescent galaxies, which may be the progenitors of massive early-types, with the protocluster at z>3.
Four out of five of them are detected in X-ray (Lx~10^43-43.5 erg/s, moderately luminous), suggesting the roles of AGNs in their
formation. Second, we confirmed the objects with multiple counterparts. From the photometric analysis, we found that many Lyman
Alpha Blobs at z=3.09 and sub-mm sources in the SSA22 field host multiple stellar components. From the spectroscopic follow-ups,
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we may for the first time, found that some of them are actually group galaxies clustered within 200 kpc. They would be hierarchical
multiple mergers at the early-phase of formation history of massive early-type galaxies. These multiple merging systems at high-z will
be very important targets at the era of JWST.
Lamy, Laurent (LESIA, Observatoire de Paris, CNRS, France) – Poster # 2
Accessing HST auroral observations through the APIS database
Remote UV measurement of the outer planets are a wealth of informations on rings, moons, planetary atmospheres and magnetospheres.
Auroral emissions in particular provide highly valuable constraints on the auroral processes at work and the underlying coupling between
the solar wind, the magnetosphere, the ionosphere and the moons. Key observables provided by high resolution spectro-imaging
include the spatial topology and the dynamics of active magnetic field lines, the radiated and the precipitated powers or the energy of
precipitating particles.
The Hubble Space Telescope (HST) acquired thousands of Far-UV spectra and images of the aurorae of Jupiter, Saturn and Uranus
since 1993, feeding in numerus magnetospheric studies. But their use remains generally limited, owing to the difficulty to access and
use raw and value-added data.
APIS, the egyptian god of fertilization, is also the acronym of a new database (Auroral Planetary Imaging and Spectroscopy), aimed
at facilitating the use of HST planetary auroral observations. APIS is based at the Virtual Observatory (VO) of Paris and provides a free
and interactive access to a variety of high level data through a simple research interface and standard VO tools. We will present the
capabilities of APIS and illustrate them with several examples.
Lee, Myung Gyoon (Soul National University), Poster # 5
Calibration of the Luminosity of Type Ia Supernovae with the Tip of the Red Giant Branch
Type Ia supernovae (SNe Ia) are known to be a powerful standard candle so that they play an important role in cosmic distance scale
research. Since the discovery of cosmic acceleration, a need for more accurate calibration of SNe Ia luminosity is increasing. So far,
the luminosity calibrations of SNe Ia have been done mainly using the Population I distance indicator, Cepehid variables. However,
recent calibrations of SNe Ia luminosity in the literature show a sizable scatter. Taking advantage of the high resolution of the Hubble
Space Telescope, we have been trying to improve the luminosity calibration of SNe Ia using the Population II distance indicator, the tip
of the red giant branch (TRGB). We present recent progress of our work for nearby SN Ia host galaxies based on the data in the HST
archive. We discuss the implication of our results in relation with the calibration of optical and near-infrared maximum magnitudes of
SNe Ia and the Hubble constant.
MacKenty, John W. (STScI) – Poster # 32
Current Performance and Future Potential of Wide Field Camera 3
This talk describes the current scientific performance of HST’s Wide Field Camera 3. Since its deployment in 2009, WFC3 has supported
over half of HST’s science programs. It provides observers with significantly enhanced capabilities in the UV and IR combined with excellent astrometric and photometric stability, a rich selection of filter elements, and a highly capable slit-less infrared spectroscopic mode.
Ongoing efforts at STScI to fully characterize and calibrate this instrument make possible steadily improved observations and enhance
the value of the HST archive. The primary long-term degradation in WFC3 is the unavoidable accumulation of radiation damage to its
CCD detectors in the ultraviolet/visible channel. Major progress in the mitigation of the consequences of this damage via the addition
of small amounts of background illumination and the utilization of increasingly sophisticated post-observation restoration methods has
been achieved of the past two years. While WFC3 has fully reached its pre-launch performance expectations, the re-implementation
of the observatory level spatial scan mode makes possible a set of observations not expected during the design of the instrument.
Specifically, the available dynamic range has been expanded to include very bright sources in the infrared (including a direct measurement of Vega), high signal to noise ratio spectra of exo-planet transits with sensitivity to spectral feature variations of a few tens of
parts per million have be accomplished, and the angular separations of stars have been measured to less than 30 micro-arc seconds
enabling the accurate measurement of stellar parallax out to 3-4 kpc. Plans for future improvements for both observing strategies
and data processing software will be presented. For example, ongoing studies of the backgrounds present in both visible and infrared
observations and the causes of their variations suggest options for improved planning of observations. When combined with improved
data reduction software for the extraction of infrared spectra, these should enable spectroscopic measurements of extremely faint
sources. Furthermore, advances in the characterization of persistence in the infrared detector has resulted in the routine production of
predictive persistence images -- a development of immediate value for WFC3 observers and potentially useful for JWST.
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Marston, Anthony (ESA/ESAC) – Poster # 15
Herschel Shows Earliest Star Forming Stages: A JWST Project in Waiting
Several large-scale galactic plane far-infrared and sub-millimetre imaging projects have been undertaken with the Herschel Space
Observatory. These have included complete surveys of the Gould Belt of clouds that encircle the position of the solar system within
the Milky Way, as well as sites of star formation and induced star formation, e.g. in the HOBYS program which covers such well known
objects as M16 (“Eagle nebula”), M17 and Vela C. We present some of the results from the M16 region imaged at 70-500 m in the
HOBYS Key Project. Hundreds of very young stellar object candidates have been discovered that cover some of the earliest phases of star
formation over a wide range in masses. Not all are formed in the main dust/gas filaments in the region. The spatial resolution of Herschel
is poor (3” at best for the shortest wavelength images) and begs for follow-up with JWST at near- and mid-infrared wavelengths, both
with imaging and spectroscopy. This will allow many of the physical parameters of young star forming objects to be determined. In this
poster, we outline some of the areas of detailed JWST follow-up of Herschel YSO candidates that can lead to improved understanding
of the early stages of evolution of massive stars. These include, but are not limited to multiplicity and clustering, size, orientation and in
some cases structure of surrounding disks, as well as evolution of ices, water and carbon dioxide in regions local to the YSOs.
Massari, Davide (Univ. Bologna) – Poster # 20
HST absolute proper motions of NGC6681 and the Sagittarius Dwarf Spheroidal Galaxy
We present one of the latest results of the HSTPROMO collaboration, regarding the measurement of accurate proper motions in
crowded stellar fields like Galactic globular clusters. The case of NGC 6681 (M70) is particularly interesting since we were able to
measure the absolute proper motions for the three populations intercepted in the direction of the cluster: the cluster itself, the Sagittarius
Dwarf Spheroidal galaxy and the Galactic field. For this we used Hubble Space Telescope ACS/WFC and WFC3/UVIS optical imaging
separated by a temporal baseline of 5.5 years. Five background galaxies were used to determine the zero point of the absolute-motion
reference frame. We also used background Sagittarius Dwarf Spheroidal stars to determine the rotation of the globular cluster in the
plane of the sky, finding that NGC 6681 is not rotating significantly.
Matawari, Ken (Tohuko Univ.) - Poster # 24
HST view of red K-[3.6] galaxies
We identified and studied the 38 objects with red K-[3.6] color in the Spitzer SEDS survey UDS field (Mawatari et al. in prep). From
the SED fitting analysis with large set of model templates, we found that there are four kinds of galaxies among our red galaxy sample:
(1)quiescent galaxies at z>5, (2)dusty star-forming galaxies in a wider redshift range (3)emission line galaxies at z>4, (4)AGNs. SEDS
fields are also covered by HST CANDELS survey and CANDELS imaging yields significant constraints to their SEDs and morphological
information. Finally we conclude that red K-[3.6] galaxies with relatively blue [3.6]-[4.5] color and no MIPS/24um counterpart in the
CANDELS field have high possibility of being quiescent (i.e. post star-burst phase with log(Ms)~11 and age>0.3Gyr) galaxies at z>5.
It is surprising result and they are interesting targets for future JWST spectroscopy.
Momcheva, Iva (Yale Univ.) – Contributed Talk
The 3D-HST Survey: Overview and Early Science Results
3D-HST is a near-infrared spectroscopic survey with the Hubble Space Telescope designed to study the physical processes that shape
galaxies in the distant Universe. This Treasury program was allocated 248 orbits of HST time during Cycles 18 and 19. 3D-HST has
surveyed ~600 square arc minutes of well-studied extragalactic survey fields (AEGIS, COSMOS, GOODS-S, UKIDSS-UDS) with two
orbits of primary WFC3/G141 grism coverage and two to four orbits with ACS/G800L coverage. Providing the critical third dimension - redshift - via slitless optical and near-IR grism spectra, 3D-HST opens new possibilities for science and discovery in the deep
extragalactic fields. In this talk I will briefly outline the goals and observations of the survey, review its current status and describe the
unique final dataset which includes over 2000 orbits of HST time. I will also highlight several of the early science results from the survey.
Finally, I will explore the limits of current deep HST grism observations in light of the expected capabilities of JWST.
Neuhaeuser, Ralph (U Jena, Germany) , Fred M. Walter (Stony Brook University, USA),
Valeri V. Hambaryan (U Jena, Germany), Nina Tetzlaff (U Jena, Germany) – Poster # 3
Kinematics and Equation-of-State of nearby Neutron Stars
After our discovery of RXJ1856 as a nearby, optically faint (V=26), X-ray bright neutron star with HST (Walter, Wolk, Neuhaeuser 1996)
and its confirmation (Walter & Matthew 1997), we analyzed eight more HST images to measure its large parallax (123 +/- few pc)
and large proper motion (1/3 arc sec per year, Walter et al. 2010). Distance and proper motion point back to the Sco OB association,
the likely birth place of this neutron star in a supernova.
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The travel time gives its kinematic age (0.5 Myr, e.g. Tetzlaff et al. 2011), which is smaller and, hence, consistent with the characteristic
age upper limit from X-ray period and its derivative (few Myr). From X-ray temperature, optical brightness, and distance, we could also
obtain a radius constraint: 17 +/- 3 km (Walter et al. 2010). RXJ 1856 is the prototype of the class of Magnificent Seven neutron
stars, isolated systems which are not accreting and whose emission is thermal. With additional XMM observations and X-ray phaseresolved spectroscopy, we can in principle also determine its compactness (M/R); together with the known radius R, we can then obtain
its mass M (work in progress). As this is the nearest known isolated thermal neutron star, determination of its radius and mass will
place strong constraints on the neutron star Equation-of-State. We present our past and ongoing work and discuss future application
of space telescopes to neutron stars.
O’Meara, John (Saint Michael’s College) – Poster # 29
Measuring the Mean Free Path of Ionizing Photons Over Cosmic History
From the time of its launch with GHRS and FOS to the present day with STIS and COS, HST has built a rich legacy of spectroscopic
observations of Lyman limit systems (LLS), those quasar absorption line with enough neutral hydrogen to be optically thick at the Lyman
limit. I will review the history of Lyman limit system observations with HST, and present new results from COS and WFC3 observations
of LLS, along with a discussion of our new understandings of how LLS are linked to galaxies and their environments.
Oesch, Pascale (Yale Univ.) – Contributed Talk
HST’s Discovery of Luminous Galaxy Candidates at z~9-10
Thanks to ultra-deep observations with the WFC3/IR camera on HST the frontier of galaxies has now been pushed out to z~9-12,
only ~450 Myr from the Big Bang. However, until recently only a small number of intrinsically very faint galaxies could be identified
at these redshifts based on extremely deep WFC3/IR data in and around the GOODS-South field in addition to the CLASH cluster
survey. This changed with our recent analysis of the completed CANDELS survey data over GOODS-North, from which we identified
four surprisingly bright Lyman break galaxy candidates at z~9-10. These sources are a factor ~10-20x brighter than any previous
candidate at these redshifts. Their high number suggests that star-formation was highly stochastic in the very early universe resulting
in large field-to-field variance. Additionally, Spitzer/IRAC observations of these sources resulted in the first individual rest-frame optical
detection of galaxies at z>8, revealing that these sources already had a typical stellar mass of 10^9 Msol at a cosmic time of only
500 Myr. While the star-formation rate density of galaxies with SFR>0.7 Msol/yr is found to decrease rapidly from z~8 to z~10, the
discovery of these luminous sources has very promising implications for the detection of even earlier galaxies with JWST.
Oliveira, Cristina; Tumlinson, Jason; Sembach, Ken; O’Meara, John & Chris Thom (STScI) –
Poster # 21
The First Detection of Deuterated Molecular Hydrogen at z < 1.7 Beyond the Milky Way Galaxy
We report on the first detection of deuterated molecular hydrogen, HD, at a redshift < 1.7 beyond the Milky Way galaxy. HD and H2
are detected in HST/COS data of a low metallicity (Z ~ 0.07Z_sun) damped Ly system at z = 0.18562 toward QSO B0120-28,
with log N(H I) = 20.50 +/- 0.10. Four absorption components are clearly resolved in H2 while two components are resolved in
HD; the bulk of the molecular hydrogen is associated with the components traced by HD. We find total column densities log N(HD) =
14.82 +/- 0.15 and log N(H2) = 20.00 +/- 0.10. This system has a high molecular fraction, f(H2) = 0.39 +/- 0.10 and a low HD
to H2 ratio, log (HD/2xH2) = -5.5 +/- 0.2 dex. The excitation temperature, T01 = 65 +/- 2 K, in the component containing the bulk
of the molecular gas is lower than in other DLAs. These properties are unlike those in other DLA systems but are consistent with what
is observed in dense clouds in the Milky Way.
Oliveira, Cristina (STScI) – Poster # 33
Maintaining the Scientific Capabilities of HST/COS in the Far Ultraviolet
The Cosmic Origins Spectrograph (COS), onboard the Hubble Space Telescope (HST), provides the unique capability of moderate to
high resolution in the Far Ultraviolet (FUV), down to 900 A.
Unlike other types of detectors, such as CCDs, that age whether they are used or not, the performance of the COS/FUV detector
decreases significantly with usage, due to a process commonly referred to as gain sag.
Here, we discuss the ongoing efforts to overcome gain sag effects, with the goal of preserving the scientific capabilities of the COS/
FUV instrument as close as possible to those at launch, particularly the spectral resolution.
This is especially significant in the context of extending the lifetime of the Hubble Space Telescope and given that no mission with
similar scientific capabilities is planned for the near future.
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Östlin, Göran (Department of Astronomy, Oskar Klein Centre, Stockholm University) Contributed Talk
LARS’ - The Lyman Alpha Reference Samples
The Lyman alpha (Lya) line is widely used to find and identify galaxies in the distant universe, close to the epoch when the first galaxies
formed and when the universe was reionized. However the fact that Lya is a resonant line makes it optically thick even at moderate
neutral hydrogen column densities meaning that the radiative transport of Lya photons through galaxies is a complex problem where
the structure, kinematics and dust content of the ISM are the most important parameters. In order to effectively use Lya as a quantitative
probe of the distant universe, a better understanding of what effectively regulates the escape fraction of Lya is needed. Detailed studies
of local objects is here a vital ingredient, but the rest wavelength of Lya in the far UV then means that this can only be done with HST.
I will describe LARS, the Lyman Alpha Reference Sample - a multiwavelength imaging study with the HST from the far UV to the i-band,
including the Lya, H-alpha and H-beta lines, of 14 starburst galaxies at z=0.028-0.18. The products are resolved and photometrically
calibrated Lya images as well as maps of physical quantities like the dust content and age of the stellar population. Our initial results
reveal that when a lot of Lya manages to escape it does so in the form of diffuse scattering halos. The full sample is also now complete
with COS spectroscopy probing the Lya line shape and ISM absorption lines. LARS is now about to be extended, in cycle 21, with
28 more galaxies also including less violently star forming galaxies on the so called star formation main sequence. With no clear
successor in the near future that can take on HSTs role as a UV telescope, the LARS and eLARS samples will form the backbone of
Lya astrophysics for the foreseeable future.
Paolillo, Maurizio (Univ. Napoli Federico II) – Poster # 16
Wide-Field Hubble Space Telescope Observations of the Globular Cluster System in NGC1399
We present a high spatial-resolution imaging study of globular clusters (GCs) in NGC1399, conducted with the Advanced Camera
for Surveys (ACS). Using a novel technique to construct drizzled PSF libraries for HST/ACS data, we accurately determine the fidelity
of GC structural parameter measurements from detailed artificial star cluster experiments. The NGC1399 GC system reveals a trend
of increasing half light radius r_h versus galactocentric distance, Rgal, out to about 10 kpc and a flat relation beyond. This trend is
very similar for blue and red GCs out to 40 kpc. This suggests that the size difference between blue and red GCs is due to internal
mechanisms related to the evolution of their stellar populations. Modeling the mass density profile of NGC1399 shows that additional
external dynamical mechanisms are required to limit the GC size in the galaxy halo regions to r_h ≈2 pc, such as an exotic GC
orbit distribution function, an extended dark matter halo, and/or tidal stress induced by the increased stochasticity in the dwarf halo
substructure. Furthermore in NGC1399 compact GCs show a significantly smaller line-of-sight velocity dispersion than their extended
counterparts. Considering the weaker statistical correlation in the GC r_h-color and the GC r_h-Rgal relations, the more significant
GC size-dynamics relation appears to be astrophysically more relevant and hints at the dominant influence of the GC orbit distribution
function on the evolution of GC structural parameters.
Paresce, Francesco (INAF, Italy) – Poster # 17
Panchromatic Observations of the Cluster and Giant HII Region NGC 3603
We observed the giant HII region NGC 3603, site of one of the most compact and luminous massive star clusters in the Milky Way with
the WFC3 in various bands covering the spectral range from the UV to the near IR complemented by Herschel’s 5 broad wavelength
bands covering the range 70 to 500 microns. The main objective of the observations is to study at high spatial resolution and over
the widest possible spectral range the distribution and main physical characteristics of both the stars and the cold dust from which
they originated. This wide panchromatic and deep global view of the region allows us to better understand the details of the past and
ongoing star formation processes in the cluster that has often been used as a possible galactic starburst template. We present here
the first results of the combined observations showing the dust density and temperature distributions in the region and the physical
characteristics of the associated stars and point-like sources. All of these data show unequivocally that the region is still undergoing
intense star formation activity affecting its future evolution towards either eventual dissolution or the formation of a small globular cluster.
Pirzkal, N., G. Brammer and the WFC3 team (STScI) – Poster #34
The IR background as seen by WFC3
We present a new and improved characterization of the sky background light as seen by WFC3 in the near-infrared. We determine an
empirical model of the zodiacal background from thousands of images obtained using WFC3 since its installation on board of HST. While
the structure of the background, as parametrized as a function of sun angle and ecliptic latitude, is similar to the model contained in the
WFC3 ETC, this new model extends the model to smaller values of sun angle with an accuracy of ~0.1 e-/s/pix for F098M, F105W,
F125W, F140W, and F160W. We also present a characterization of the Earth-glow background as a function of the HST pointing
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orientation with respect to the Earth limb. Interestingly, we identify a strong emission line component of the background from He I at
1083 nm in the upper atmosphere that can significantly increase the background in both IR grisms and in broad-band filters sensitive
to this wavelength, even well above (> 40 deg) the bright Earth limb. Accounting for these effects will be important for optimizing the
efficiency of potential future deep integrations with the WFC3/IR grisms and bluer broad-band filters.
Pirzkal, N. B. (STScI), Rothberg and the PEARS team – Poster #25
We present a full analysis of the Probing Evolution And Reionization Spectroscopically (PEARS) slitess grism spectroscopic data obtained
with the Advanced Camera for Surveys on board Hubble Space Telescope. PEARS covers fields within both the Great Observatories
Origins Deep Survey (GOODS) North and South fields, making it ideal as a random survey of galaxies, as well as the availability of a
wide variety of ancillary observations complemented by the spectroscopic results. Using the PEARS data, we are able to identify starforming galaxies (SFGs) within the redshift volume 0 < z < 1.5. Star-forming regions in the PEARS survey are pinpointed independently
of the host galaxy. This method allows us to detect the presence of multiple emission-line regions (ELRs) within a single galaxy. We
identified a total of 1162 H , [O III], and/or [O II] emission lines in the PEARS sample of 906 galaxies to a limiting flux of ~10-18 erg
s-1 cm-2. The ELRs have also been compared to the properties of the host galaxy, including morphology, luminosity, and mass. From
this analysis, we find three key results: (1) the computed line luminosities show evidence of a flattening in the luminosity function with
increasing redshift; (2) the star-forming systems show evidence of complex morphologies with star formation occurring predominantly
within one effective (half-light) radius. However, the morphologies show no correlation with host stellar mass. (3) Also, the number
density of SFGs with M * >= 109 M ⊙ decreases by an order of magnitude at z <= 0.5 relative to the number at 0.5 < z < 0.9,
supporting the argument of galaxy downsizing.
Rejkuba, Marina (ESO), Bill Harris, Gretchen Harris, Laura Greggio – Contributed Talk
HST probes the outer stellar halo of an early type galaxy
We have used ACS and WFC3 cameras on board HST to resolve stars in the halo of the nearest giant E galaxy NGC 5128 out to 140
kpc (25 effective radii, Reff) along the major axis and 70 kpc (13 Reff) along the minor axis. This dataset provides an unprecedented
radial coverage of stellar halo properties in any galaxy.
Color-magnitude diagrams clearly reveal the presence of the red giant branch stars belonging to the halo of NGC 5128 even in the
most distant fields. The V-I colors of the red giants enable us to measure the metallicity distribution in each field and so map the
metallicity gradient out to ~90kpc (~17 Reff) distance from the galaxy centre. We observe a smooth transition from metal-rich inner
halo to metal-poor
outer halo. We also trace the stellar density gradient for metal-poor and metal-rich populations.
Rydberg, Claes-Erik (Stockholm Univ.) – Poster # 26
CLASH: lensed population III galaxy candidates discovered
The first metals in the universe are expected to be formed in population III stars. These are pristine stars consisting of almost exclusively hydrogen and helium. However, these stars have so far remained elusive. Simulations indicate galaxies consisting exclusively,
or almost exclusively, of population III stars form at z>6. By fitting Yggdrasil model spectra to multiband photometry data, we have
identified six population III galaxy candidates in the survey Cluster Lensing and Supernova survey with Hubble (CLASH). We rule out
alternative mundane galaxies and low redshift interlopers through similar fits to catalogs of spectra from more mundane objects. If
confirmed through spectroscopy, this would constitute the first detection of the “missing link” between the early pristine universe and
the metal-enriched universe.
Saha, Abhijit and Gautham Narayan (NOAO, Tucson) – Poster # 6
Establishing a Network of Faint DA White Dwarf Spectrophotometric Standards using WFC3 photometry and ground based
spectroscopy
Systematic uncertainties in photometric calibration are the dominant source of total error in dark energy studies using Type Ia Supernovae,
as well as other forefront cosmology efforts, e.g. photo-redshift determinations for weak lensing mass tomography. Current and nextgeneration ground-based all-sky surveys require a network of calibration stars with 1) known SEDs to properly and unambiguously take
into account passband differences, and 2) that are on a common photometric zeropoint scale. HST affords us the ability to establish
this essential network of faint primary photometric standards, exploiting the well-understood spectral energy distributions of DA white
dwarf stars, without the complications of observing through the time-variable Earth’s atmosphere. We have selected $9$ equatorial DA
targets that will have SNR approx$200$ in Pan-STARRS, Dark Energy Survey and LSST images, while avoiding saturation. We have
obtained Gemini spectra to constrain temperature and $log(g)$ and determine the SED, and we are using broadband HST photometry
to set the overall flux scale for each source, and determine any applicable reddening. Together with the bright HST CALSPEC standards,
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our network of faint stars can be used as fundamental spectrophotometric standards at wavelengths beyond the range of HST, and
in any arbitrary passband. By placing primary photometric standards directly into the multi-epoch, all-sky databases, we will enable
exquisitely precise measurements of variation in the total system sensitivity. This extends the precision photometric heritage from HST
to benefit essentially all existing and upcoming survey projects, and directly and specifically addresses one of the current barriers to
understanding the nature of dark energy.
Smith, Linda (ESA/STScI) – Poster # 18
An HST and near-IR Study of a Triplet of Superstar Clusters in the Starburst Core of M82
We present a study of the triplet of super star clusters in the core (region A) of the M82 starburst designated M82-A1, A2 and A3,
based on HST/STIS optical spectroscopy, archival HST imaging, and Gemini/NIFS near-IR IFU spectroscopy. We find the ages of the
three clusters to lie between 4.5 - 6.5 Myr from modelling of the STIS spectra and the presence or absence of CO bands in the NIR
data. Their photometric masses and sizes are measured to be 4–7 × 10^5 M⊙, and ∼2.8, 1.8, 1.0 pc for A1,2,3 respectively. From
the STIS spectra, we measure heliocentric radial velocities of 320 ± 2, 330 ± 6, and 336 ± 5 km s−1 for A1,2,3, placing them all
at the eastern end of the x2 orbits of the well-known bar. The clusters are located in a high density (800–1800 cm^−3) environment
and have compact H II regions, implying that a significant proportion of the cluster input mechanical energies has been radiatively lost
inside the clusters. We find that the cluster winds must have stalled due to the high ambient pressure of the ISM in this region of the
starburst. We discuss the possible formation scenarios of the three clusters, and propose that they were formed in-situ on the outer x2
orbits in regions of dense molecular gas. The subsequent negative radiative feedback from the central starburst region has then acted
to modify the gas on these orbits to the predominantly ionized state that we see today. This is consistent with the dynamically active
environment in the central starburst, where the state of the gas on the various orbits is likely to change on short timescales. The similar
radial velocities of the three clusters and their small projected separation of ∼ 25 pc suggest that they may merge in the near future.
Tacchella, Sandro (ETH Zurich, Institute for Astronomy) – Contributed Talk
Bulge formation and disk quenching at z~2: An HST perspective on the emergence and evolution of the most massive galaxies.
I will present the comparison, for our SINS-zSINF sample of massive galaxies on the star forming Main Sequence at z~2, of their
kpc-scale-resolved maps of on-going star formation (from Adaptive-Optics-assisted VLT/SINFONI Halpha spectra) and their underlying
stellar mass distributions (from HST/WFC3 data).
I will discuss how this comparison can explain, within a single self-consistent hierarchical picture, two main outstanding issues in galaxy
evolution: (1) the growth of stellar mass, separately in bulge and disk components, in Main Sequence galaxies at these high redshifts,
and (2) the evolution of the number density and structural properties of the quenched galaxy population, including the origin of the
puzzling growth of its average size with cosmic time.
Tailo, Marco (Univ. Roma) – Poster # 7
HST and stellar evolution: understanding the blue hook stars in Globular Clusters
We present new computation of the phase of Late Helium Flash which is responsible of the “blue hook” population in Globular Clusters.
The new models are fully evolutionary, as they are the outcome of computation from the main sequence to the Horizontal Branch
phase of models taking into account the presence of multiple populations in clusters where this phase appears to be populated. We
also compare our synthetic models with the observed HBs of the clusters Centauri and NGC2419. We deal in particular with the
analysis of the UV HST data for the cluster NGC 2419. We re-examine the peculiar “vertical” shape in the F435 vs. F435-F625 plane
of the blue hook in Centauri, in the ACS/WFC data described by Anderson & van der Marel (2009). This latter peculiar morphology
is shown to be easily reproduced in its whole extend by the evolution of a single mass evolving from the helium rich population present
in the cluster, undergoing the late He-flash. We are able to also interpret the presence of very hot HB stars that do not suffer the late
flash. Our models include computation of elemental diffusion, and can deal with the interpretation of the helium abundances measured
in the extended HB of Centauri.
Trenti, Michele (Univ. Cambridge) – Contributed Talk
Random sights with Hubble: the Brightest of Reionizing Galaxies survey
I will present the latest results of our Large HST/WFC3 Brightest of Reionizing Galaxies (BoRG) survey, which include the best determination of the galaxy luminosity function at redshift z~8, the constraints on the redshift evolution of the neutral hydrogen fraction from
Keck and VLT spectroscopic follow-up observations, and inference on the connection between galaxies and their dark-matter halos
from clustering analysis. Our data and their modeling point toward a scenario where there is a late reionization which is completed by
z~7-8, and where the evolution of the galaxy luminosity function is driven by evolution of the underlying halo mass function rather than
by a change in the efficiency of star formation. Our BoRG survey also offers a first glimpse of the rare and clustered galaxies that future
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large-area near-IR space missions such as EUCLID and WFIRST will see at z~8-10 and that will be prime targets for JWST follow-ups
to study the internal properties of galaxies in the epoch of Reionization.
Van der Wel, Arjenn (Max Planck Institute for Astronomy) – Contributed Talk
The path from compact z~2 galaxy to giant elliptical
Based on HST imaging from CANDELS and HST spectroscopy from 3D-HST we can now show that massive early-type galaxies
initially appear at early times (z~2-3) as compact, disk-like systems and subsequently grow in size and mass through merging,
gradually destroying their pre-existing disks. Two novel observational results provide the evidence for this narrative: 1) strong evolution
in the intrinsic thickness of the stellar body -- reconstructed from the projected axis ratio distribution -- as a function of redshift, and
2) a non-evolving slope and intrinsic scatter of the size-stellar mass relation. This new insight, as well as our general view on galaxy
evolution since z~2, is underpinned by the direct mass measurement of an early-type galaxy enabled by our recent discovery of the
most distant gravitational lens so far.
Whitmore, B. C. (STScI) – Poster # 37
The Unlimited Potential of the Hubble Archives
Since the beginning of the mission, the Hubble archives has revolutionized the way astronomers do their science. Twenty five years
ago an astronomer would have to go to the telescope themselves. With the advent of the Hubble archive, suddenly astronomers had
access to all Hubble data (after the 1 year proprietary time), the data was already calibrated (greatly reducing redundant work and
uniformity), and the data was shipped to them at their home institution.
But that was just the beginning. With the advent of the internet, a whole new set of capabilities and opportunities became possible. This
talk will highlight three examples, the:
Hubble Legacy Archive - (http://hla.stsci.edu), the Hubble Source Catalog - (http://archive.stsci.edu/hst/hsc) and the MAST Discovery
Portal - (http://mast.stsci.edu/explore).
Using these facilities, we are only now beginning to realize the true potential of the Hubble archives, both for the present, and for
decades into the future.
Rogier A. Windhorst, S. H. Cohen, R. A. Jansen (ASU), S. P. Driver, A. Robotham, M.
Alpaslan, R. Lange (ICRAR, U-WA), A. M. Hopkins, M. Cluver, I. Konstantopoulos (AAO,
Sydney), J. Stuart B. Wyithe, and Robert L. Barone-Nugent (U. Melbourne) – Poster # 31
Strategies to observe JWST First Light objects at z=10--20 based on recent results from the Hubble Wide Field Camera 3
UltraDeep Field.
We reflect on the best observing strategies to see an optimum number of First Light objects at z~10-20 with the James Webb Space
Telescope (JWST), based on recent results from the Hubble Wide Field Camera 3 UltraDeep Field.
First, we summarize the best available data to redshifts z<8 on how the Schechter UV Luminosity Function (LF) evolves in its faint-end
slope [alpha(z)], its characteristic luminosity [M*(z)] and corresponding space density [phi*(z)], and use hierarchical models to explore
how alpha(z) and phi*(z) may evolve for z>8. We use the strongly declining number of z=9-11 candidates in the HUDF-XDF compared
to the large number of z=7-8 objects, to constrain the plausible range in evolution of M*(z) for z>~9. While hierarchical models suggest
that alpha(z>8) converges to ~-2 and phi*(z>8) to ~< 10^-3/Mpc^3, the one plausible z~10-12 candidate seen in the HUDF-XDF
suggests that M*(z) may drop to fainter than M=-17.5 mag at z>10 in WMAP-yr9/ Planck13 cosmology.
If so, this may have a significant impact on the optimal observing strategies of z>10 objects with JWST. If M*(z) and/or phi*(z) continue
to decline significantly for z>9, only deep 200+ hr JWST surveys that reach to AB>31 mag will see a significant number of z>10
objects. Shallow or medium deep JWST surveys that reach to AB<30 mag may not see very many unlensed z>10 objects, since
they will generally sample brighter than M* at z>10. Hence, in order to sample the brighter-end of the LF at z>10 -- and to average
over the expected
significant cosmic variance at z>10 -- JWST will either need to observe a larger number (>5) of deep JWST fields, and/or it will need
to do a much larger number (>10-20) of medium-deep surveys on gravitational lensing foreground targets.
The 6 Hubble Frontier Fields that started in 2013 are excellent lensing targets for JWST. We suggest that additional lensing foreground
clusters or groups be identified all over the sky before JWST flies to optimize its surveys for objects at z>10. We present a subset of
2400 galaxy groups from the GAMA spectroscopic survey to z=0.4 that have M>10^15 M_o and are sufficiently compact to also
be excellent lensing targets for JWST medium-deep surveys of First Light objects at z>10.