| Program Number | Principal Investigator | Program Title |
|---|---|---|
| 13760 | Derck L. Massa, Space Science Institute | Filling the gap --near UV, optical and near IR extinction |
| 13776 | Michael D. Gregg, University of California - Davis | Completing The Next Generation Spectral Library |
| 14038 | Jennifer Lotz, Space Telescope Science Institute | HST Frontier Fields - Observations of Abell 370 |
| 14070 | Philip D. Bennett, Eureka Scientific Inc. | A Red Supergiant Mass Accurate to 1% |
| 14072 | Martha L. Boyer, Space Telescope Science Institute | The Evolution of Metal-rich Asymptotic Giant Branch Stars |
| 14074 | Roger Cohen, Universidad de Concepcion | Opening the Window on Galaxy Assembly: Ages and Structural Parameters of Globular Clusters Towards the Galactic Bulge |
| 14080 | Anne Jaskot, Smith College | LyC, Ly-alpha, and Low Ions in Green Peas: Diagnostics of Optical Depth, Geometry, and Outflows |
| 14086 | Jay Strader, Michigan State University | Dynamical Confirmation of a Stellar-mass Black Hole in the Globular Cluster M62 |
| 14096 | Dan Coe, Space Telescope Science Institute - ESA | RELICS: Reionization Lensing Cluster Survey |
| 14098 | Harald Ebeling, University of Hawaii | Beyond MACS: A Snapshot Survey of the Most Massive Clusters of Galaxies at z>0.5 |
| 14119 | Luciana C. Bianchi, The Johns Hopkins University | Understanding Stellar Evolution of Intermediate-Mass Stars from a New Sample of SiriusB-Like Binaries |
| 14163 | Mickael Rigault, Humboldt Universitat zu Berlin | Honing Type Ia Supernovae as Distance Indicators, Exploiting Environmental Bias for H0 and w. |
| 14172 | Brendan Bowler, University of Texas at Austin | Imaging Accreting Protoplanets in the Young Cluster IC 348 |
| 14181 | S Thomas Megeath, University of Toledo | A Snapshot WFC3 IR Survey of Spitzer/Hershel-Identified Protostars in Nearby Molecular Clouds |
| 14186 | Heddy Arab, Observatoire de Strasbourg | Mapping dust extinction properties across the IC 63 photodissociation region |
| 14209 | Brian Siana, University of California - Riverside | The Final UV Frontier: Legacy Near-UV Imaging of the Frontier Fields |
| 14212 | Karl Stapelfeldt, Jet Propulsion Laboratory | A Snapshot Imaging Survey of Spitzer-selected Young Stellar Objects in Nearby Star Formation Regions*.t23 |
| 14217 | Mark R. Showalter, SETI Institute | Neptune's Evolving Inner Moons and Ring-Arcs |
| 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 |
| 14237 | Nial Rahil Tanvir, University of Leicester | r-process kilonova emission accompanying short-duration GRBs |
| 14259 | Denija Crnojevic, Texas Tech University | Resolved halo substructures beyond the Local Group: the assembly histories of NGC 253 and NGC 5128 |
| 14260 | Drake Deming, University of Maryland | A Metallicity and Cloud Survey of Exoplanetary Atmospheres Prior to JWST |
| 14268 | Nicolas Lehner, University of Notre Dame | Project AMIGA: Mapping the Circumgalactic Medium of Andromeda |
| 14343 | Nitya Kallivayalil, The University of Virginia | Proper Motion and Internal Kinematics of the SMC: are the Magellanic Clouds bound to one another? |
| 14347 | John Sebastian Pineda, University of Colorado at Boulder | Joint VLA and HST Observations of Brown Dwarf Aurorae |
| 14790 | Jessica Agarwal, Max Planck Institute for Solar System Research | Investigating the binary nature of active asteroid 288P/300163 |
GO 14038: HST Frontier Fields - Observations of Abell 370
HST observations of the Frontier Fields cluster, Abell 370 |
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. Moreover, as intense concentrations of mass, galaxy clusters provide 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 builds on the highly successful CLASH program,which used 17-colour ACS/WFC3 images to map 25 galaxy clusters, tracing the mas profile and the dark matter distribution. in addition, the observations identified several lensed galaxies at redshifts that enter the JWST domaine, with the most distant object lying at a redshift z~11, within a few hundred million years of the Big Bang. The Frontier Fields program is a large-scale Director's Discretionary program that capitalises on the latter characteristic by targeting 4-6 strong-lensing galaxy clusters for very deep optical and near-infrared imaging. WFC3 and ACS will be used to observe the clusters, with simultaneous imaging obtained in parallel of a nearby "blank" field. Since the observations need to made at a specific orientation, they are being taken in two sets, ~6 months apart, alternating between detectors. Abell 370 at z=0.375 is the sixth and final target. The present observations will provide the second epoch data, with WFC3-IR covering the cluster and ACS centred on the parallel field. These observations will close out the 3-year Frontier Fields program. |
GO 14080: LyC, Ly-alpha, and Low Ions in Green Peas: Diagnostics of Optical Depth, Geometry, and Outflows
 A montage of green pea galaxies discovered by the Galaxy Zoo project |
Understanding the galaxy formation and galaxy evolution has been a strong focus of astronomical research since thne 1970s and remains a key issue for 21st century astrophysics. Since we cannot follow an individual galaxy through time, tackling these questions requires a statistical approach, and, as a result, large-scale surveys have played a crucial role in the field. In particular, the Sloan Digital Sky Survey, conducted from Apache point Observatory from the 1990s through the early years of this century, has provided a treasure trove of information of galaxies at low and moderate redshifts. One of the interesting discoveries that originated from SDSS was the discovery of so-called "green pea" galaxies - compact objects whose combined images have a greenish hue, originally uncovered by citizen scientists as part of the Galaxy Zoo project. Closer inspection shows that these are gas-rich galaxies lying at relatively low redshifts, 0.1 < z < 0.36, with the green-tinged hue partly stemming from the presence of strong oxygen ([O III]) emission. These characteristics indicate that the galaxies are undergoing strong star-forming episodes. The present program aims to take advantage of HST's unparalleled resolution and extraordinary sensitivity at ultraviolet wavelengths, and will use the Cosmic Origins Spectrograph to obtain spectra are far-UV wavelengths. Those observations will probe optical depth, the geometry of neutral gas and radiative transfer within these systems, revealing the physical structure of the underlying star forming regions and potentially offering insight into the nature of high redshift lyman-alpha emitters. |
GO 14217: Neptune's evolving Inner moons and Ring-Arcs
Voyager images of Neptune's rings |
> | The Saturnian ring system is the most prominent in the Solar System, visible in Galileo's refractor and first clearly identified by Huyghens in 1679. However, all of the gas/ice giants in the Solar System have ring systems. Neptune's rings are much less substantial, and were first detected through stellar occultations and then resolved as "ring-arcs" in ground-based observations made from ESO's La Silla observatory. They were subsequently imaged in more detail, and revealed as full rings, by Voyager 2 during its 1989 fly-by. There are at least 5 rings, named after the astronomers Galle, Le Verrier, Lasalle, Arago and Adams, all of whom contributed to Neptune's discovery. The rings are relatively tenuous and faint, more comparable with Jupiter's rings than Saturn's. Higher density arcs are evidenct in the outermost ring (Adams), and it is likely that their structure is maintained through orbital resonance with one of Neptune's inner moons, Galatea. The present program aims to probe those questions. In particular, it aims to recover Netune's 14th moon, S/2004 N 1, which is only ~9 km in diameter and was discovered through HST images in 2013. The present observations will enable a better determination of the orbital parameters. The observations will also be used to search for Naiad, whose orbit is also poorly defined. Finally, the WFC3 UVIS obervations will also be used to monitor changes in the ring-arc structure. |