| Program Number | Principal Investigator | Program Title |
|---|---|---|
| 14072 | Martha L. Boyer, Space Telescope Science Institute | The Evolution of Metal-rich Asymptotic Giant Branch Stars |
| 14096 | Dan Coe, Space Telescope Science Institute - ESA | RELICS: Reionization Lensing Cluster Survey |
| 14158 | Eileen T Meyer, University of Maryland Baltimore County | Mapping the kpc-scale Velocity Structure of Jets with HST |
| 14160 | John M. O'Meara, Saint Michaels College | A 100 million-fold increase in the measured sizes of neutral gas reservoirs in the early Universe |
| 14163 | Mickael Rigault, Humboldt Universitat zu Berlin | Honing Type Ia Supernovae as Distance Indicators, Exploiting Environmental Bias for H0 and w. |
| 14481 | Jelle Kaastra, Space Research Organization Netherlands | Shining light on obscured AGN outflows |
| 14594 | Rich Bielby, Durham Univ. | QSAGE: QSO Sightline And Galaxy Evolution |
| 14606 | Brooke Devlin Simmons, University of California - San Diego | Secular Black Hole Growth and Feedback in Merger-Free Galaxies |
| 14618 | Michael Shara, American Museum of Natural History | Ultraviolet Flashers in M87: Rapidly Recurring Novae as SNIa Progenitors |
| 14634 | Denis C Grodent, Universite de Liege | HST-Juno synergistic approach of Jupiter's magnetosphere and ultraviolet auroras |
| 14649 | Katherine Anne Alatalo, Carnegie Institution of Washington | Opening a New Window into Galaxy Evolution Through the Lens of CO-detected Shocked Poststarburst Galaxies |
| 14651 | Matt James Darnley, Liverpool John Moores University | Recurrent Nova M31N 2008-12a: The surrounding 'Super-Remnant' - A signpost to Type Ia Supernova progenitors |
| 14652 | Benne Willem Holwerda, Sterrewacht Leiden | 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 |
| 14661 | Michael H. Wong, University of California - Berkeley | Wide Field Coverage for Juno (WFCJ): Jupiter's 2D Wind Field and Cloud Structure |
| 14667 | Hsiao-Wen Chen, University of Chicago | Differentiating Gas Infall and Outflows with Resolved Star Formation Morphology |
| 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 |
| 14685 | Wen-fai Fong, University of Arizona | Underlying Hosts or Highly-Kicked? Determining the Nature of Host-less Short Gamma-ray Bursts with HST |
| 14700 | Ben E. K. Sugerman, Goucher College | Light Echoes and the Environments of SNe 2014J and 2016adj |
| 14706 | Eilat Glikman, Middlebury College | Testing the Triggering Mechanism for Luminous, Radio-Quiet Red Quasars in the Clearing Phase: A Comparison to Radio-Loud Red Quasars |
| 14719 | Philip N. Best, Royal Observatory Edinburgh | The detailed properties of star-forming regions at high redshift: a matched-resolution HST-Halpha-ALMA study |
| 14727 | Pierre-Alain Duc, Commissariat a l'Energie Atomique (CEA) | Probing Super Star Cluster formation in the most favorable environments: the metal-enriched, gas-rich and turbulent collisional ring of NGC 5291 |
| 14734 | Nitya Kallivayalil, The University of Virginia | Milky Way Cosmology: Laying the Foundation for Full 6-D Dynamical Mapping of the Nearby Universe |
| 14759 | Thomas M. Brown, Space Telescope Science Institute | What Happens in the Atmospheres of Hot Horizontal Branch Stars Near 20, 000K? |
| 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 |
| 14770 | Sangmo Tony Sohn, Space Telescope Science Institute | Proper Motions of the Crater-Leo Group: Testing the Group Infall Scenario |
| 14779 | Melissa Lynn Graham, University of Washington | A NUV Imaging Survey for Circumstellar Material in Type Ia Supernovae |
| 14840 | Andrea Bellini, Space Telescope Science Institute | Schedule Gap Pilot |
| 14846 | Aaron Romanowsky, San Jose State University | Ultra-diffuse Galaxies in Clusters and the Field: Masses and Stellar Populations |
| 14884 | Jessica Agarwal, Max Planck Institute for Solar System Research | Characterising the dust ejection process in the first known active binary asteroid system 288P/300163. |
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 14163: Honing Type Ia Supernovae as Distance Indicators, Exploiting Environmental Bias for H0 and w.
Supernova in M101 |
Supernovae have long attracted the attention of both amateur and professional astronomers as a means of studying the violent eruption and death of massive stars and degenerates. However, in the last decade they have also acquired considerable importance as distance indicators, tracing the expansion of the universe to redshifts well beyond the reach of more conventional yardsticks, such as cepheids, and providing a key underpinning for the hypothesised existence of dark energy. Understanding the supernovae themselves, and, in particular, their progenitors, is key to accurately interpreting their luminosities and distances. Recent observations have suggested that there may be a correlation between the brightnesses of Type Ia supernovae and some characteristics of their local environment; specifically, supernovae found in close proximity to star formation appear to be sub-luminous. The present SNAP program uses the UVIS camera on WFC3 to image the locations of supernovae that have been used to map the Hubble flow, and will use the UV-to-optical flux ratio to characterise the local environment, potentially offering a means of tightening the distribution in the Hubble diagram. |
GO 14770: Proper Motions of the Crater-Leo Group: Testing the Group Infall Scenario
The low-mass dwarf galaxy, Leo II |
The Milky Way, M31 and M33 are the three largest galaxies in the Local Group, and their gravitational potential dominates the motions of the more than 25 other members, the majority of which are 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. Cosmological models of formation scenarios suggest that these individual systems may actually consist of a smaller number of groups, which collectively fell into the potential well defined by the larger systems. One such group of Mily Way satellites includes the 5 systems Crater 1, Crater 2, Leo II, Leo IV and Leo V. Understanding the full 3-D space motions of these systems can help constrain formation scenarios. Even though those galaxies, and their brightest stellar constituents, are faint, measuring radial velocity is a relatively straightforward procedure. Deriving tangential motions is not, since the typical proper motions of these systems are a few mas/year at best. The present program aims to capitalise on the exceptional resolution and high stability of HST to address this issue. Wide Field Camera 3 and the Advanced Camera for Surveys will be used to obtain first epoch observations of Crater 2 and Leo V; second epoch observations in later cycles will be used to determine absolute motions for those 2 systems and for the globular cluster, Crater 1. |
GO 14884:Characterising the dust ejection process in the first known active binary asteroid system 288P/300163.
The multiple nuclei of the main belt comet P/2013 R3 as imaged by Hubble in late 2013 and 2014 |
The classical picture evoked by the noun 'asteroid" is of a large, unchanging space rock, silently orbiting the Sun within the main belt, between Mars and Jupiter. Over the last decade, however, observations have shown that this classical picture is, like many, not entirely accurate. A number of asteroids have been discovered that show clear signs of some type of surface activity. Some have been dubbed "main belt comets", including the asteroid Scheila (d ~ 110 km), which was observed to have acquired a halo in October-December 2010; the asteroid 1979 OW7/1996 N2, which exhibited similar behaviour in 1996 and again in 2002; MBC-2013-P5, which has exhibited a spectacular set of dusty tails; and MBC P/2013 R3 (pictured here), which has multiple "nuclei" that are gradually drifting apart at speeds of less than 1 metre/second. The origin of the activity is unclear, and may reflect either the present of volatiles or residual effects from fragmentation. The present observations centre on the asteroid 288P/300163 (also known as 2006 VW139).This system was detected in outburstin 2010/2011, and has been resolved as a binary. The present observations aim to monitor the dust activity as the system crosses the ecliptic mid-Plane and makes a close approach to Earth. The goal is to determine the rotational properties, and constrain whether the dust activity might be related to the systems fragmentation for form a binary. The system will be imaged at optical wavelengths with Wide Field Camera 3. |