| Program Number | Principal Investigator | Program Title |
|---|---|---|
| 14607 | Eleonora Troja, University of Maryland | Identify the signature of neutron star mergers through rapid Hubble observations of a short GRB |
| 14624 | Hector G. Arce, Yale University | Taming the Flame: A Near-IR imaging study of the NGC 2024 (Flame Nebula) cluster |
| 14634 | Denis C Grodent, Universite de Liege | HST-Juno synergistic approach of Jupiter's magnetosphere and ultraviolet auroras |
| 14662 | Luigi R. Bedin, Osservatorio Astronomico di Padova | The end of the White Dwarf Cooling Sequences of Omega Centauri |
| 14697 | Bradley M Peterson, The Ohio State University | A Cepheid Distance to NGC 4051 |
| 14728 | John S. Gallagher, University of Wisconsin - Madison | Hearts of Darkness: Compact Obscured Nuclei in S0/a Galaxies |
| 14772 | Bart P. Wakker, University of Wisconsin - Madison | Observing gas in Cosmic Web filaments to constrain simulations of cosmic structure formation |
| 14840 | Andrea Bellini, Space Telescope Science Institute | Schedule Gap Pilot |
| 14849 | Eric S. Perlman, Florida Institute of Technology | The 3C111 Jet: X-ray Variability, Spectrum & Broadband SED |
| 15073 | Boris T. Gaensicke, The University of Warwick | Extreme evolved solar systems (EESS) |
| 15075 | Jay Christopher Howk, University of Notre Dame | The CGM of Massive Galaxies: Where Cold Gas Goes to Die? |
| 15077 | Tucker Jones, University of California - Davis | Accurate Emission Line Diagnostics at High Redshift |
| 15081 | Andrew Robinson, Rochester Institute of Technology | Revealing the circum-nuclear torus: HST imaging of active galaxies observed during a Spitzer reverberation mapping campaign |
| 15113 | Abhijit Saha, National Optical Astronomy Observatory, AURA | Extending the DA white dwarf spectrophotometric network to the Southern Hemisphere |
| 15115 | John David Silverman, University of Tokyo | Emergence of the supermassive black hole - galaxy mass relations at z > 1 |
| 15133 | Peter Erwin, Max-Planck-Institut fur extraterrestrische Physik | Solving the Mystery of Galaxy Bulges and Bulge Substructure |
| 15145 | Adam Riess, The Johns Hopkins University | The Hubble Constant to 1%: Physics beyond LambdaCDM |
| 15153 | Dan Watson, University of Rochester | The jets and shocks of NGC 1333: a large WFC3 mosaic of [Fe II] and H I line emission |
| 15162 | Peter Blanchard, Harvard University | Constraining the Late-Time Light Curve Behavior of Three Diverse Superluminous Supernovae |
| 15171 | Bryan Jason Holler, Space Telescope Science Institute | The rotation period, orbit, and mass of Eris' satellite Dysnomia |
| 15179 | Ruth C. Peterson, SETI Institute | Astrophysics Meets Atomic Physics: Fe I Line Identifications and Templates for Old Stellar Populations from Warm and Hot Stellar UV Spectra |
| 15181 | David J. V. Rosario, Durham Univ. | AGN Before and After: Towards a balanced view of the connection between circumnuclear gas and nuclear black hole activity |
| 15189 | David John Wilson, The University of Warwick | Post Common Envelope Binaries as probes of M dwarf stellar wind and habitable zone radiation environments |
| 15215 | Vardha N. Bennert, Cal Poly Corporation, Sponsored Programs Department | A Local Baseline of the Black Hole Mass - Host Galaxy Scaling Relations for Active Galaxies |
| 15229 | Emanuele Daddi, Commissariat a l'Energie Atomique (CEA) | Spectroscopic redshifts and age dating of a first statistical sample of passive galaxies at z~3 |
| 15238 | Adam L. Kraus, University of Texas at Austin | The IMF to Planetary Masses Across the Milky Way |
| 15241 | Kirsten L. Larson, California Institute of Technology | Clumpy Star Formation in Local LIRGS |
| 15242 | Lucia Marchetti, Open University | SNAPshot observations of the largest sample of lensed candidates in the Equatorial and Southern Sky identified with Herschel |
| 15265 | John Blakeslee, NRC Herzberg Institute of Astrophysics | MASSIVE+: The Growth Histories of MASSIVE Survey Galaxies from their Globular Cluster Colors |
| 15275 | Karoline Gilbert, Space Telescope Science Institute | Securing HST's UV Legacy in the Local Volume: Probing Star Formation and the Interstellar Medium in Low Mass Galaxies |
| 15303 | Chris D'Andrea, University of Pennsylvania | Revealing the Environmental Dependence in Superluminous Supernovae Diversity |
| 15328 | Jessica Agarwal, Max Planck Institute for Solar System Research | Orbital period and formation process of the exceptional binary asteroid system 288P |
| 15344 | David Jewitt, University of California - Los Angeles | Centaurs and Activity Beyond the Water Sublimation Zone |
| 15350 | Walter Peter Maksym, Smithsonian Institution Astrophysical Observatory | Resolved BPT Mapping of Nearby AGN |
| 15424 | William B. Sparks, Space Telescope Science Institute | An intensive ultraviolet imaging campaign for Europa's plumes |
| 15427 | James M. Schombert, University of Oregon | Exploring the Nature of Dark Matter Through Near-IR CMD's of LSB Galaxies |
GO 14662: The end of the White Dwarf Cooling Sequences of Omega Centauri
ACS imaging of the central regions of Omega Cen |
Globular clusters are members of the Galactic halo population, which formed during the first extensive period of star formation in the Milky Way. As such, the properties of the 106 to 107 stellar constituents can provide crucial insight into the earliest stages of galaxy formation. Hubble has conducted a significant number of observing programs targeting these systems, with the majority designed to obtain moderately deep, multicolour imaging data of a range of clusters. Those programs probe evolved stars, on the red giant and horizontal branch, and generally extend only a few magnitudes below the main-sequence turnoff. Noetheless, the exqusite photometric precision offered by HST's camera has revealed that the majority of these systems have multiple stellar populations, rather than conforming to traditional single-burst formation models. A few clusters have been studied in detail - specifically, the two nearest clusters, NGC 6397, an extremely metal-poor cluster, and M4, a moderately metal-rich systems; Omega Centauri, one of the most massive clusters, perhaps even the remnant core of a dwarf galaxy; and 47 Tucanae, one of the higher metallicity systems, lying in the foreground of the Small Magellanic Cloud. Deep imaging of all four clusters has succeeded in clear detecion of the white dwarf cooling sequence in those clusters, and those data have been used to derive age estimates. The present program builds on past observations in aiming to probe the multiple white dwarf cooling sequences in Omega Cen. The WFC3/UVIS and ACS/WFC cameras will be used to obtain multi-colour imaging of the cluster. Those observations should enable measurement over the full extent of the white dwarf cooling sequences, offering the potential of resolving the nature and origin(s) of the distinct stellar populations. |
GO 15171: The rotation period, orbit, and mass of Eris' satellite Dysnomia
Hubble Space Telescope images of Eris and Dysnomia |
As is now well known, on 2006 the IAU changed pluto's status from the outermost planet in the solar system to a dwarf planet, and the largest currently-known member of the Kuiper. One of the main factors in adopting that revised classification was the discovery of several other large KBOs, at least comparable in size with Pluto. Those systems included Eris, discovered in 2005 by Mike Brown using the Palomar Schmidt telescope. Eris is probably slightly smaller than Pluto, with a diameter of ~2300 miles. Deep imaging with the Keck adaptive optics revealed that Eris has a companion, the moon Dysnomia. The system has since been imaged with Hubble, and the initial orbital measurements suggest that Eris is more massive (i.e. denser) than Pluto. The present program will use the Wide Fields camera 3 UVIS channel to monitor the system, providing both an improved determination of the relative orbits of the pair and potential measurment of the rotational period of Dysnomia through tracking photometric variations. |
GO 15275: Securing HST's UV Legacy in the Local Volume: Probing Star Formation and the Interstellar Medium in Low Mass Galaxies
Subaru image of the Leo A dwarf galaxy, one of the galaxies targeted in this program |
The Milky Way Galaxy is a member of a relatively sparse set of galaxies known as the Local Group. Fifty-four members are currently catalogued within ~1.5 Mpc., with the overwhelming majority being dwarf systems. The Milky Way and M31 are the two dominant members, with M33 the only other spiral system. Most of the dwarf galaxies are satellites of the three major systems, typically dwarf spheroidal systems that have exhausted most of their gaseous content and exhibit little or no current star formation. However, there are also a number of irregular dwarfs that are gas rich and exhibit ongoing star formation. Hubble is ideally suited to probing the characteristics of those systems, providing both unparalleled angular resolution to resolve the stellar populations and UV sensitivity to highlight actvie star formation regions. The present program is using Wide Field Camera 3 to obtain ultraviolet imaging of 22 low-mass, nearby (<3.5 Mpc) galaxies towards the edge of the Local Group. Combined with previous optical and near-IR imaging, the data will probe the star formation history in these systems, measure the UV flux, and map the dust distributions and composition. |
GO 15242: SNAPshot observations of the largest sample of lensed candidates in the Equatorial and Southern Sky identified with Herschel
An ALMA/HST composite image of the lensed galaxy, SDP 81 |
Gravitational lensing is a consequence the theory of general relativity. Its importance as an astrophysical tool first became apparent with the realisation (in 1979) that the quasar pair Q0957+561 actually comprised two lensed images of the same background quasar. In the succeeding years, lensing has been used primarily to probe the mass distribution of galaxy clusters, using theoretical models to analyse the arcs and arclets that are produced by strong lensing of background galaxies, and the large-scale mass distribution, through analysis of weak lensing effects on galaxy morphologies. Gravitational lensing can also be used to investigate the mass distribution of individual galaxies. Until recently, the most common background sources that were being detected and investigates were quasars. Galaxy-galaxy lenses, however, offer a distinct advantage, since the background source is extended, and therefore imposes a stronger constraints on the mass distribution of the lensing galaxy than a point-source QSO. HST has carried out a number of programs following up candidate lenses identified from the Sloan Digital Sky Survey and based on sub-mm observation by the Herschel satellite. The rpesent program aims to build on the latter sample by using Hubble Snapshot imaging with the F110W filter in the WFC3-IR camera to verify the nature of up to 200 lensing candidates from the major herschel extragalactic surveys. |