| Program Number | Principal Investigator | Program Title |
|---|---|---|
| 14096 | Dan Coe, Space Telescope Science Institute - ESA | RELICS: Reionization Lensing Cluster Survey |
| 14227 | Casey Papovich, Texas A & M University | The CANDELS Lyman-alpha Emission At Reionization (CLEAR) Experiment |
| 14269 | Nicolas Lehner, University of Notre Dame | Just the BASICs: Linking Gas Flows in the Circumgalactic Medium to Galaxies |
| 14594 | Rich Bielby, Durham Univ. | QSAGE: QSO Sightline And Galaxy Evolution |
| 14608 | Nadia L Zakamska, The Johns Hopkins University | Host galaxies of high-redshift quasars with extreme outflows |
| 14611 | Or Graur, Harvard University | Going gently into the night: constraining Type Ia supernova nucleosynthesis using late-time photometry |
| 14618 | Michael Shara, American Museum of Natural History | Ultraviolet Flashers in M87: Rapidly Recurring Novae as SNIa Progenitors |
| 14621 | Jason J. Wang, University of California - Berkeley | Probing the young circumplanetary environment of a directly-imaged exoplanet through a rare transit event |
| 14622 | Katherine E. Whitaker, University of Connecticut | A Chance Alignment: Resolving a Massive Compact Galaxy Actively Quenching at z=1.8 |
| 14626 | Mary Barsony, SETI Institute | DASH Mapping of IC348: The IMF from 2 to 80 Jupiter Masses |
| 14628 | Danielle Berg, University of Wisconsin - Milwaukee | The Evolution of C/O in Low Metallicity Dwarf Galaxies |
| 14636 | Igor Dmitrievich Karachentsev, Russian Academy of Sciences, Special Astrophysical Obs. | TRGB Distances to the Edge Between the Local Sheet and Virgo Infall: Last of the Low Hanging Fruit |
| 14641 | Edward M. Sion, Villanova University | Short Orbital Period Recurrent Novae as Supernovae Type Ia Progenitors |
| 14646 | Siyi Xu, European Southern Observatory - Germany | A White Dwarf with an Actively Disintegrating Asteroid |
| 14648 | Adam Riess, The Johns Hopkins University | A New Threshold of Precision, 30 micro-arcsecond Parallaxes and Beyond |
| 14649 | Katherine Anne Alatalo, Carnegie Institution of Washington | Opening a New Window into Galaxy Evolution Through the Lens of CO-detected Shocked Poststarburst Galaxies |
| 14652 | Benne Willem Holwerda, University of Louisville Research Foundation, Inc. | Super-Eight: The brightest z~8 Galaxies |
| 14653 | James Lowenthal, Smith College | The most luminous galaxies: strongly lensed SMGs at 1 |
| 14654 | Peter Milne, University of Arizona | A Second Ladder: Testing for Bias in the Type Ia Distance Scale with SBF |
| 14657 | Lida Oskinova, Universitat Potsdam | The wind variability in oscillating massive stars |
| 14668 | Alex V. Filippenko, University of California - Berkeley | Continuing a Snapshot Survey of the Sites of Recent, Nearby Supernovae: Cycle 24 |
| 14675 | Julia Christine Roman-Duval, Space Telescope Science Institute - ESA | Metal Evolution and TrAnsport in the Large Magellanic Cloud (METAL): Probing Dust Evolution in Star Forming Galaxies |
| 14704 | Charlie Conroy, Harvard University | A Year in the Whirlpool |
| 14734 | Nitya Kallivayalil, The University of Virginia | Milky Way Cosmology: Laying the Foundation for Full 6-D Dynamical Mapping of the Nearby Universe |
| 14762 | Justyn Robert Maund, University of Sheffield | A UV census of the sites of core-collapse supernovae |
| 14767 | David Kent Sing, University of Exeter | The Panchromatic Comparative Exoplanetary Treasury Program |
| 14768 | Nathan Smith, University of Arizona | UV Signatures of Shock Interaction in an Eta Carinae Analog |
| 14779 | Melissa Lynn Graham, University of Washington | A NUV Imaging Survey for Circumstellar Material in Type Ia Supernovae |
| 14798 | Michal Drahus, Uniwersytet Jagiellonski | Origin and Evolution of the First Known Ultra-Young Asteroid Family and its Doubly-Synchronous Binary Member |
| 14808 | Nao Suzuki, Institute for Physics and Mathematics of the Universe | SUbaru Supernovae with Hubble Infrared (SUSHI) |
| 14811 | Laurent Lamy, Observatoire de Paris - Section de Meudon | The Grand Finale : probing the origin of Saturn s aurorae with HST observations simultaneous to Cassini polar measurements |
| 14853 | Mirko Krumpe, Leibniz-Institut fur Astrophysik Potsdam (AIP) | Catching a Changing Look Quasar as it undergoes significant changes in accretion rate |
| 14877 | Vincent Bourrier, Observatoire de Geneve | Confirmation and characterization of an exosphere around the super Earth 55 Cnc e |
| 14903 | Lorenz Roth, Royal Institute of Technology | Detection methods for water vapor in Europa's plumes. |
GO 14227: The CANDELS Lyman-alpha Emission At Reionization (CLEAR) Experiment
Part of the GOODS/Chandra Deep Field South field, as imaged by HST |
Hubble has made significant contributions in many science areas, but galaxy formation, assembly and evolution is a topic that has been transformed by the series of deep fields obtained over the past 20 years. CANDELS, one of three Multi-Cycle Treasury Program executed in cycles 18 through 20, is one of the more recent additions to this genre.Building on past investment of both space- and ground-based observational resources, it covers five five fields including both the Great Observatory Origins Deep Survey (GOODS), centred on the northern Hubble Deep Field (HDF) in Ursa Major and the Chandra Deep Field-South in Fornax. In addition to deep HST data at optical and near-infrared wavelengths, the fields have been covered at X-ray wavelengths by Chandra (obviously) and XMM-Newton; at mid-infrared wavelengths with Spitzer; and ground-based imaging and spectroscopy using numerous telescopes, including the Kecks, Surbaru and the ESO VLT. This represents an accumulation of almost 1,000 orbits of HST time, and comparable scale allocations on Chandra, Spitzer and ground-based facilities. CANDELS added new optical and near-infrared observations with WFC3 and ACS (see this link for more details). Those data have been processed and analysed by both the CANDELS team and by other groups within the community. The present program builds on this foundation by adding 16 pointings within the CANDELS fields with the WFC3 G102 grism. The goal is to probe reionisation by measuring the strength of Lyman-alpha absorption in galaxies at redshifts between z=6.5 and z=8.2. The expectation is that the ovall absorption strength should decrease with decreasing redshift as the intergalactic medium is ionised, and the proportion of neutral gas decreases. |
GO 14594: QSAGE: QSO Sightline And Galaxy Evolution
An HST GHRS spectrum of the bright quasar, HE 2347-4342 |
Star formation is the key astrophysical process in determining the overall evolution of galactic systems, the generation of heavy elements, and the overall enrichment of interstellar and intergalactic material. Tracing the overall evolution through a wide redshift range is crucial to understanding how gas and stars evolved to form the galaxies that we see around us now. In particular, the star formation rate appears to have declined significantly between redshifts z~2 and z~1. The present program aims to compile observations that measure the star formation rate in a large sample of galaxies at z~1. This goal will be achieved by using the G141 grism on Wide Field Camera 3 to target fields centred on quasars where spectroscopy indicates the presence of gaseous absorbers (ie galactic halos) at the appropriate redshift. |
GO 14704: A Year in the Whirlpool
The Whirlpool galaxy, M51 |
NGC 5194, the Whirlpool galaxy, is a grand design spiral galaxy with an interacting lower-mass companion, NGC 5195, lying at a distaince of ~7 Mpc from the Milky Way. Originally catalogued as the 51st obect in Charles Messier's list of non-comets, its spiral nature was first discerned by visual observations using the Earl of Rosse's Leviathan of Parsontown. With its clearly deefined spiral structure, M 51 is a prime target for star formation investigations. The present program aims to probe the star formation history by mapping the number and distribution of asymptotic giant branch long period variable (AGB LPV) stars. or miras. These LPV have periods ranging from ~150 days to more than 500 days, and there are well determined correlations between the periodicity and the mass (and hence age) of the individual stars. with such long periods, obervations need to be spaced over a correspondingly long time frame, and the present program schedules observations at 34 epochs over a full year. |
GO 14811: The Grand Finale : probing the origin of Saturn's aurorae with HST observations simultaneous to Cassini polar measurements
|
Planetary aurorae are stimulated by the influx of charged particles
from the Sun, which travel along magnetic field lines and funnel into the atmosphere near
the magnetic poles. Aurorae therefore require that a planet has both a substantial atmosphere and
a magnetic field. They are a common phenomenon on Earth, sometimes visible at magnetic latitudes
more than 40 degrees from the pole, and have also been seen on Jupiter, Saturn, Uranus
and Neptune. Saturn passed through its equinox in August 2009, and in the succeeding years the north pole has tilted
more and more towards the Sun. As a consequence, we now have an excellent view of the polar regions. Moreover,
the Cassini probe has moved into a polar orbit, that takes it regularly across the auroral regiosn.
The present program is using STIS to obtain time-tagged FUV images during those passages,
enabling a direct comparison of the large-scale structure with
|