| Program Number | Principal Investigator | Program Title |
|---|---|---|
| 14071 | Sanchayeeta Borthakur, The Johns Hopkins University | How are HI Disks Fed? Probing Condensation at the Disk-Halo Interface |
| 14076 | Boris T. Gaensicke, The University of Warwick | An HST legacy ultraviolet spectroscopic survey of the 13pc white dwarf sample |
| 14078 | Jonathan Hargis, Space Telescope Science Institute | New Faint Galaxies at the Local Group's Edge: Antlia B and Five Candidate Ultra-Faint Dwarfs |
| 14106 | Lorenz Roth, Royal Institute of Technology | Probing Ceres' exosphere and water vapor outgassing |
| 14132 | Mark B. Peacock, Michigan State University | The spatial distribution of hot stellar populations in M31's globular clusters |
| 14170 | Eva Wuyts, Max-Planck-Institut fur extraterrestrische Physik | A Complete Census: Mapping the Lya Emission and Stellar Continuum in a Lensed Main-Sequence Galaxy at z=2.39 Hosting an AGN-driven Nuclear Outflow |
| 14199 | Patrick Kelly, University of California - Berkeley | Refsdal Redux: Precise Measurements of the Reappearance of the First Supernova with Multiple Resolved Images |
| 14206 | Adam Riess, The Johns Hopkins University | A New Threshold of Precision, 30 micro-arcsecond Parallaxes and Beyond |
| 14216 | Robert P. Kirshner, Harvard University | RAISIN2: Tracers of cosmic expansion with SN IA in the IR |
| 14219 | John P. Blakeslee, Dominion Astrophysical Observatory | Homogeneous Distances and Central Profiles for MASSIVE Survey Galaxies with Supermassive Black Holes |
| 14227 | Casey Papovich, Texas A & M University | The CANDELS Lyman-alpha Emission At Reionization (CLEAR) Experiment |
| 14243 | Deirdre Coffey, University College Dublin | True Jet Rotation Probed in NUV Jet Core |
| 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 |
| 14625 | Gilda E. Ballester, University of Arizona | Connecting the lower and upper atmospheres of a warm-Neptune. Implications for planetary evolution. |
| 14629 | Marc W. Buie, Southwest Research Institute | Astrometry of 2014MU69 for New Horizons encounter |
| 14638 | Knox S. Long, Eureka Scientific Inc. | What Makes Radio-detected and Optically-detected Supernova Remnants in NGC6946 Different? |
| 14649 | Katherine Anne Alatalo, Carnegie Institution of Washington | Opening a New Window into Galaxy Evolution Through the Lens of CO-detected Shocked Poststarburst Galaxies |
| 14668 | Alex V. Filippenko, University of California - Berkeley | Continuing a Snapshot Survey of the Sites of Recent, Nearby Supernovae: Cycle 24 |
| 14707 | Philip Louis Massey, Lowell Observatory | Searching for the Most Massive Stars in M31 and M33 |
| 14734 | Nitya Kallivayalil, The University of Virginia | Milky Way Cosmology: Laying the Foundation for Full 6-D Dynamical Mapping of the Nearby Universe |
| 14767 | David Kent Sing, University of Exeter | The Panchromatic Comparative Exoplanetary Treasury Program |
| 14786 | Benjamin F. Williams, University of Washington | Progenitor Masses for Every Nearby Historic Core-Collapse Supernova |
| 14797 | Ian Crossfield, University of California - Santa Cruz | Atmospheric Albedos, Alkalis, and Aerosols of Hot Jupiters |
| 14807 | Elena Sabbi, Space Telescope Science Institute | The primordial binary fraction in the young massive cluster Westerlund 2 |
| 14809 | Gabor Worseck, Max-Planck-Institut fur Astronomie, Heidelberg | An Accurate Measurement of the IGM HeII Lyman Alpha Forest toward a Newly Discovered UV-bright Quasar at z>3.5 |
| 14840 | Andrea Bellini, Space Telescope Science Institute | Schedule Gap Pilot |
| 14862 | Ariel Goobar, Stockholm University | Resolving the multiple images of the strongly lensed SNIa iPTF16geu |
| 14864 | Jessica Agarwal, Max Planck Institute for Solar System Research | Tracing rotational fission in the first known active binary asteroid system 288P/300163 |
GO 14078: New Faint Galaxies at the Local Group's Edge: Antlia B and Five Candidate Ultra-Faint Dwarfs
The Magellanic irregular, NGC 3109 |
The Milky Way, M31 and M33 are the three largest galaxies in the Local Group. The system, however, includes more than 25 other members, with the majority being dwarf spheroidal galaxies that are satellites of either M31 or the Milky Way. Those galaxies have old, evolved stellar populations, and even the most prominent have masses that are less than a few x 107 MSun, or 10-4 that of the Milky Way. Antlia B is the most recent discovery, a low-mass irregular system lying aproximately 1.3 Mpc from the Milky Way and ~72 kpc from the NGC 3109 dwarf. The discovery was made from ground-based CCD imaging taken by the Dark Energy Survey camera on the Cerro Tololo 4-metre Blanco telescope. The ground-based data show evidence for an old (~10 Gyr) population together with some relatively recent star formation (200-400 Myrs). That survey has also resulted in the identification of five extremely faint objects that may be ultra-faint dwarfs, with luminosities less than 104 LSun and mass-to-light ratios exceeding 100. Those systems also may well be satellites of NGC 3109. The present program aims to use Hubble to obtain deep V- and I-band (F606W and F814W) imaging with the Advanced Camera for Surveys, probing the stellar populations at significantly fainter magnitudes. |
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 14629: Astrometric Follow-up of 2014MU69U for the New Horizons Mission
Hubble Space Telescope images of the Pluto system, including the recently discovered moons, P4 and P5 |
The Kuiper Belt lies beyond the orbit of Neptune, extending from ~30 AU to ~50 AU from the Sun, and includes at least 70,000 objects with diameters exceeding 100 km. Setting aside Pluto, the first trans-Neptunian objects were discovered in the early 1990s. Most are relatively modest in size, with diameters of a few hundred km and photometric properties that suggest an icy composition, similar to Pluto and its main satellite, Charon. In recent years, a handful of substantially larger bodies have been discovered, with diameters of more than 1000 km; indeed, one object, Eris (2003 UB13), is slightly larger than Pluto (2320 km) and 25% more massive. We know the mass for Eris because it has a much lower mass companion, Dysnomia, which orbits Eris with a period of 16 days (see this recent press release ). Pluto itself has at least 5 companions: Charon, which is about 1/7th the mass of Pluto, and the much smaller bodies, Hydra, Nix, P4 and P5 discovered through HST observations within the last few years. The New Horizons Mission was launched on January 19th 2006 with the prime purpose of providing the first detailed examination of Pluto. Following the Pluto fly-by on Bastille day 2015, the program aims to redirect the probe towards one or more smaller members of the Kuiper Belt, with the goal of providing a closer look at these icy bodies. Based on Hubble imaging, a suitable prime target has been identified: 2014 MU69, a ~30 km KBO lying ~44 AU from the Sun. In addition, New Horizons is expected to take longer-range, monochromatic images of up to 10 other KBOs. The present observations aim to refine the orbital parameters for the prime target to optimize the New Horizon encounter. |
GO 14668: Continuing a Snapshot Survey of the Sites of Recent, Nearby Supernovae - Cycle 24
A recent supernova in M100 |
Supernovae mark the (spectacular) evolutionary endpoint for a subset of stellar systems. Standard models predict that they originate from massive stars and (probably) close binaries with a compact (WD, neutron star) component, but there are still some questions remaining over whether we fully understand the range of possible progenitors. The last decade has seen the development of a number of large-scale programs, usually using moderate-sized telescopes, that are dedicated to monitoring (relatively nearby galaxies, searching for new supernovae. This program builds on observations taken in several previous cycles, and aims to obtain follow-up multi-waveband images of nearby galaxies, focusing on the sites of recent supernovae. The program concentrates on systems within 20 Mpc of the Milky Way. The observations are taken well after maximum, with the aim of using the unparalleled angular resolution of WFC3 to identify the fading remnant, search for evidence for light echoes,characterise the local stellar population and perhaps determine the nature of the likely progenitor. |