| Program Number | Principal Investigator | Program Title |
|---|---|---|
| 14096 | Dan Coe, Space Telescope Science Institute - ESA | RELICS: Reionization Lensing Cluster Survey |
| 14178 | Matthew A. Malkan, University of California - Los Angeles | WFC3 Infrared Spectroscopic Parallel Survey: The WISP Deep Fields |
| 14181 | S Thomas Megeath, University of Toledo | A Snapshot WFC3 IR Survey of Spitzer/Hershel-Identified Protostars in Nearby Molecular Clouds |
| 14277 | John Thomas Stocke, University of Colorado at Boulder | Probing Hot Gas in Spiral-Rich Galaxy Groups |
| 14495 | David Sobral, Lancaster University | The gas-metallicity and the ISM of the brightest Lyman-alpha emitter at z=6.6: metal-free? |
| 14596 | Xiaohui Fan, University of Arizona | Is Lyman Alpha Emitter CR7 Powered by a Direct Collapse Black Hole? |
| 14602 | Jay Christopher Howk, University of Notre Dame | The Perseus Project: Probing Metal Mixing, Dust Destruction, and Kinematics in the Vertical Extension of the Perseus Arm |
| 14606 | Brooke Devlin Simmons, University of California - San Diego | Secular Black Hole Growth and Feedback in Merger-Free Galaxies |
| 14609 | Tracy M Becker, Southwest Research Institute | Psyche's UV Reflectance Spectra: Exploring the origins of the largest exposed-core metallic asteroid |
| 14618 | Michael Shara, American Museum of Natural History | Ultraviolet Flashers in M87: Rapidly Recurring Novae as SNIa Progenitors |
| 14629 | Marc W. Buie, Southwest Research Institute | Astrometry of 2014MU69 for New Horizons encounter |
| 14630 | Thomas E. Collett, University of Portsmouth | A unique probe of the dark matter distribution in a halo at z=1: A strong lens with a bright central image |
| 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 |
| 14655 | Sowgat Muzahid, Universiteit Leiden | Probing Warm-Hot Gas in the Outskirts of Galaxy Clusters Using Quasar Absorption Lines |
| 14658 | Eric W. Peng, Peking University | Massive Star Clusters and the Origin of Ultra-Diffuse Galaxies |
| 14668 | Alex V. Filippenko, University of California - Berkeley | Continuing a Snapshot Survey of the Sites of Recent, Nearby Supernovae: Cycle 24 |
| 14672 | Ruth C. Peterson, SETI Institute | Tracing the Earliest Nucleosynthesis from Elements Just Past the Iron Peak in Extremely Metal-Poor Dwarfs |
| 14677 | Tim Schrabback, Universitat Bonn, Argelander Institute for Astronomy | Probing the most distant high-mass galaxy clusters from SPT with HST weak lensing observations |
| 14693 | Karen Marie Leighly, University of Oklahoma Norman Campus | Testing the Torus Origin of the Broad Absorption Line Outflow in WPVS 007 |
| 14700 | Ben E. K. Sugerman, Eureka Scientific Inc. | Light Echoes and the Environments of SNe 2014J and 2016adj |
| 14721 | Christopher J. Conselice, University of Nottingham | The Fundamental Plane of Ultra-Massive Galaxies at z~2 |
| 14729 | Rajib Ganguly, University of Michigan | A New Twist in the Quasar Radio Dichotomy: The Case of the Missing Outflows |
| 14734 | Nitya Kallivayalil, The University of Virginia | Milky Way Cosmology: Laying the Foundation for Full 6-D Dynamical Mapping of the Nearby Universe |
| 14754 | Crystal Linn Martin, University of California - Santa Barbara | Confronting the 3D Orientation of Galactic Disks in Space: Disk Structure vs. Circumgalactic Gas Flows |
| 14779 | Melissa Lynn Graham, University of Washington | A NUV Imaging Survey for Circumstellar Material in Type Ia Supernovae |
| 14783 | Kailash C. Sahu, Space Telescope Science Institute | Detecting Isolated Black Holes through Astrometric Microlensing |
| 14787 | Justin D. Linford, George Washington University | Imaging the Ejecta in Classical Novae |
| 14797 | Ian Crossfield, University of California - Santa Cruz | Atmospheric Albedos, Alkalis, and Aerosols of Hot Jupiters |
| 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 |
| 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 |
GO 14096: RELICS: Reionization Lensing Cluster Survey
Hubble image and mass map for the cluster ACT-CL J0102-4915, one of the clusters included in the RELICS program |
The overwhelming majority of galaxies in the universe are found in clusters. As such, those 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, and the Frontier Fields program, targeting six clusters for deep multi-colour imaging. RELICS is focused on using massive galaxy clusters as gravitational telescopes, searching for strongly lensed background galaxies drawn from the high redshift universe. Imaging 46 fields in 41 galaxy clusters, this program aims to identify galaxies with redshifts in the range 9 < z < 12. By targeting strongly-lensing clusters, standard models for galaxy evolution suggest that the program can deliver ~100 galaxies in that redshift range, together with more than 150 galaxies at z~8. A significant number of these galaxies should be brighter than H~25.5, and therefore accessible to more detailed follow-up observations. Conversely, the actual number of galaxies detected will set constraints on the galaxy number-redshift distribution, and the overall formation and assembly history. |
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 14633: A SNAP UV Spectroscopic Study of Star-Planet Interactions
SOHO image of an extremely strong solar flare |
Stellar activity, whether through flares and coronal mass ejections, has the potential to affect the ability of life to evolve and survive on otherwise habitable planets in stellar systems. High energy radiation can lead to significant mutations, and particle ejections can actually strip the atmospheres of unfortunate planets. Previous HST programs have focused on low mass M dwarfs, the most populous stars in the galaxy, and systems where the habitable zone lies close to the parent star, with a correspondingly higher vulnerability. Those observations suggest evidence for interactions between the stellar transition region and the planets, with a correlation between the presence of high temperature emission lines (N V, C IV, Si IV) and the planetary mass and orbit i.e. suggestive of planetary interactions driving conditions in the stellar corona. The present SNAP program expand obsevations to higher-mass K dwarfs and solar-type G dwarfs that are known to harbour exoplanets, searching for similar correlations. The Cosmic Origins Spectrograph will be used to obtain UV spectra (1150-1450 Angstroms), providing a broad sampling of the range of activity levels among these dwarfs. |
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. |