| Program Number | Principal Investigator | Program Title |
|---|---|---|
| 14079 | Matthew James Hayes, Stockholm University | Unveiling the Dark Baryons II: the First Sample of OVI Emission Imaging |
| 14096 | Dan Coe, Space Telescope Science Institute - ESA | RELICS: Reionization Lensing Cluster Survey |
| 14114 | Pieter van Dokkum, Yale University | A Wide-Field WFC3 Imaging Survey in the COSMOS Field |
| 14164 | Ata Sarajedini, Florida Atlantic University | Exploring the nature and synchronicity of early cluster formation in the Local Group |
| 14182 | Thomas H. Puzia, Pontificia Universidad Catolica de Chile | The Coma Cluster Core Project |
| 14251 | Amy E. Reines, National Optical Astronomy Observatory, AURA | The Structures of Dwarf Galaxies Hosting Massive Black Holes |
| 14594 | Rich Bielby, Durham Univ. | QSAGE: QSO Sightline And Galaxy Evolution |
| 14597 | Jay Farihi, University College London | An Ultraviolet Spectral Legacy of Polluted White Dwarfs |
| 14606 | Brooke Devlin Simmons, University of California - San Diego | Secular Black Hole Growth and Feedback in Merger-Free Galaxies |
| 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 |
| 14633 | Kevin France, University of Colorado at Boulder | A SNAP UV Spectroscopic Study of Star-Planet Interactions |
| 14634 | Denis C Grodent, Universite de Liege | HST-Juno synergistic approach of Jupiter's magnetosphere and ultraviolet auroras |
| 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 |
| 14643 | Pieter van Dokkum, Yale University | Imaging of three Ultra Diffuse Galaxies with measured stellar kinematics |
| 14649 | Katherine Anne Alatalo, Carnegie Institution of Washington | Opening a New Window into Galaxy Evolution Through the Lens of CO-detected Shocked Poststarburst Galaxies |
| 14658 | Eric W. Peng, Peking University | Massive Star Clusters and the Origin of Ultra-Diffuse Galaxies |
| 14677 | Tim Schrabback, Universitat Bonn, Argelander Institute for Astronomy | Probing the most distant high-mass galaxy clusters from SPT with HST weak lensing observations |
| 14683 | Jean-Claude Bouret, CNRS, Laboratoire d'Astrophysique de Marseille | Before the Burst: The Properties of Rapidly Rotating, Massive Supergiants |
| 14699 | David Sobral, Lancaster University | The hosts of the early ionized bubbles: the nature and diversity of the most luminous Lyman-alpha emitters at z~6-7 |
| 14704 | Charlie Conroy, Harvard University | A Year in the Whirlpool |
| 14729 | Rajib Ganguly, University of Michigan | A New Twist in the Quasar Radio Dichotomy: The Case of the Missing Outflows |
| 14746 | Thomas Rauch, Eberhard Karls Universitat, Tubingen | Stellar Laboratories: High-precision Atomic Physics with STIS |
| 14758 | Zach K. Berta-Thompson, University of Colorado at Boulder | The Hydrogen Content of a Rocky Earth-Size Exoplanet |
| 14762 | Justyn Robert Maund, University of Sheffield | A UV census of the sites of core-collapse supernovae |
| 14772 | Bart P. Wakker, University of Wisconsin - Madison | Observing gas in Cosmic Web filaments to constrain simulations of cosmic structure formation |
| 14779 | Melissa Lynn Graham, University of Washington | A NUV Imaging Survey for Circumstellar Material in Type Ia Supernovae |
| 14797 | Ian Crossfield, University of California - Santa Cruz | Atmospheric Albedos, Alkalis, and Aerosols of Hot Jupiters |
| 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 |
| 14840 | Andrea Bellini, Space Telescope Science Institute | Schedule Gap Pilot |
| 14848 | Thomas R. Ayres, University of Colorado at Boulder | Cracking the Conundrum of F Supergiant Coronae |
| 14891 | William B. Sparks, Space Telescope Science Institute | Confirming the ice plumes of Europa |
| 14894 | Paul A. Wilson, CNRS, Institut d'Astrophysique de Paris | Observing the Beta Pic Hill sphere transit in the far-UV |
GO 14182: The Coma Cluster Core Project
Hubble image covering part of the central regions of the Coma cluster |
The Coma cluster is the nearest rich galaxy cluster, lying at a distance of
~100 Mpc from the Milky Way. The cluster includes well over 1000 major galaxies, centred on two giant
ellipticals, NGC 4874 and NGC 4889. Chandra observations show that the
galaxies are embedded in very hot intracluster gas
(see |
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 14677: Probing the most distant high-mass galaxy clusters from SPT with HST weak lensing observations
The South Pole Telescope at the Amundsen-Scott South Pole Station |
The overwhelming majority of galaxies in the universe are found in clusters. As such, these systems offer an important means of tracing the development of large-scale structure through the history of the universe. Galaxy clusters can be identified at moderate redshifts by searching for signatures of the Sunyaev-Zeldovich effect: high energy electrons in the hot intercluster medium interact with radiation from the cosmic microwave background to distort the microwave spectrum. The South Pole Telescope is a 10-metre microwave/millimetre telescope located at Amundsen-Scott South Pole Station on the Antarctiva high plateau, close to the geographic South Pole. That telescope has been used to search for galaxy clusters. As intense mass concentrations, these systems are highly efficient gravitational lenses, capable of concentrating and magnifying light from background high redshift galaxies to allow detailed spectropic investigations of star formation in the early universe. Hubble imaging has already revealed lensed arcs and detailed sub-structure within a handful of rich clusters. At the same time, the lensing characteristics provide information on the mass distribution within the lensing cluster. The present program targets nine high-mass galaxy clusters that represent the strinbgest SZ detections. The Wide Field Camera on the Advanced Camera for Surveys and the Wide Field Camera 3 near-IR camera will be used to image those systems to measure the shapes of background galaxies. Those observations will be combined with Chandra X-ray data and Spitzer infrared data with the goal using weak lensing to characterise the cluster mass distributions. |
GO 14894: Observing the Beta Pic Hill sphere transit in the far-UV
Gemini Planet Imager observations of Beta Pic b; the linked image shows the extended disk |
It is now well established that planet formation occurs within circumstellar disks. The past decade has seen the identification of many examples of such phenomena around young stars, notably through infrared observations by the Spitzer space telescope and ground-based data from millimetre-wave interferometers.One of the most prominent is the edge-on debris disk disk around beta Pictoris, an A star at a distance of ~ 19 parsecs and an estimated age of ~10-20 million years. Originally discovered in the early 1980s, the system has been since targeted extensively from both the ground and space, including coronagraphic observations with STIS and direct imaging with WFPC2, ACS and WFC3 on HST. High angular-resolution ground-based imaging in late 2008 with the NACO instrument on the ESO Very Large Telescope resulted in the detection of a planet in that system. The planet's orbit lies close to the star, inside the inner edge of the debris disk with a semi-major axis of ~9 AU and slightly inclined to the plane of the disk. Spectroscopic observations indicate that the exoplanet is a gas giant, with a radius approximately 1.65 times that of Jupiter and a mass ~sevenfold greater. The orbital period is only 21.6 years, and since its discovery Beta Pic b has circled behind the parent star and been recovered by high-resolution imagers such as Sphere and the Gemini Planet Finder. The planet will shortly start its pasage across the face of the parent star. It remains unclear whether the planet itself will transit, but there is a strong expectation that the Hill sphere - the spatial volume where the planet's gravity dominates, and where residual material from its formation may be trapped - will transit. The present program aims to test this hypothesis by using the Cosmic Origins Spectrograph to search for variable absorption features in the specrtum of the parent star. |