| Program Number | Principal Investigator | Program Title |
|---|---|---|
| 13691 | Wendy L. Freedman, University of Chicago | CHP-II: The Carnegie Hubble Program to Measure Ho to 3% Using Population II |
| 13760 | Derck L. Massa, Space Science Institute | Filling the gap --near UV, optical and near IR extinction |
| 13765 | Bradley M Peterson, The Ohio State University | A Cepheid-Based Distance to the Benchmark AGN NGC 4151 |
| 13767 | Michele Trenti, University of Melbourne | Bright Galaxies at Hubble's Detection Frontier: The redshift z~9-10 BoRG pure-parallel survey |
| 13779 | Sangeeta Malhotra, Arizona State University | The Faint Infrared Grism Survey (FIGS) |
| 13801 | Varsha Kulkarni, University of South Carolina Research Foundation | Probing Structure in Cold Gas at z <~ 1 with Gravitationally Lensed Quasar Sightlines |
| 13845 | Adam Muzzin, University of Cambridge | Resolved H-alpha Maps of Star-forming Galaxies in Distant Clusters: Towards a Physical Model of Satellite Galaxy Quenching |
| 13941 | Eleonora Troja, University of Maryland | IDENTIFY THE SIGNATURE OF NEUTRON STAR MERGERS THROUGH RAPID CHANDRA/HUBBLE OBSERVATIONS OF A SHORT GRB |
| 14038 | Jennifer Lotz, Space Telescope Science Institute | HST Frontier Fields - Observations of Abell 370 |
| 14054 | Ehud Behar, Technion-Israel Institute of Technology | Tracking Down the Ionized Outflow of NGC 7469 |
| 14069 | Nate Bastian, Liverpool John Moores University | Searching For Multiple Populations in Massive Young and Intermediate Age Clusters |
| 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 |
| 14077 | Boris T. Gaensicke, The University of Warwick | The frequency and chemical composition of rocky planetary debris around young white dwarfs: Plugging the last gaps |
| 14088 | Eros Vanzella, INAF, Osservatorio Astronomico di Bologna | Unveiling the Lyman continuum morphology with HST |
| 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 |
| 14122 | Lise Christensen, University of Copenhagen, Niels Bohr Institute | Unveiling stellar populations in absorption-selected galaxies |
| 14127 | Michele Fumagalli, Durham Univ. | First Measurement of the Small Scale Structure of Circumgalactic Gas via Grism Spectra of Close Quasar Pairs |
| 14138 | Kohji Tsumura, FRIS, Tohoku University | Absolute Measurement of the Cosmic Near-Infrared Background Using Eclipsed Galilean Satellites as Occulters |
| 14140 | Jessica Werk, University of Washington | Using UV-bright Milky Way Halo Stars to Probe Star-Formation Driven Winds as a Function of Disk Scale Height |
| 14143 | Vincent Bourrier, Observatoire de Geneve | Probing the nature and evolution of the oldest known planetary system through Lyman-alpha observations |
| 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 |
| 14178 | Matthew A. Malkan, University of California - Los Angeles | WFC3 Infrared Spectroscopic Parallel Survey: The WISP Deep Fields |
| 14212 | Karl Stapelfeldt, NASA Goddard Space Flight Center | A Snapshot Imaging Survey of Spitzer-selected Young Stellar Objects in Nearby Star Formation Regions*.t23 |
| 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 |
| 14241 | Daniel Apai, University of Arizona | Cloud Atlas: Vertical Cloud Structure and Gravity in Exoplanet and Brown Dwarf Atmospheres |
| 14245 | Miriam Garcia, Centro de Astrobiologia (CSIC/INTA) Inst. Nac. de Tec. Aero. | The winds of the most Fe-poor massive stars of the Local Group: Sextans-A |
| 14257 | Dennis Bodewits, University of Maryland | Far UV spectroscopic measurements of the deuterium abundance of comets |
| 14327 | Saul Perlmutter, University of California - Berkeley | See Change: Testing time-varying dark energy with z>1 supernovae and their massive cluster hosts |
| 14340 | Alexandre Gallenne, Universidad de Concepcion | Accurate masses and distances of the binary Cepheids S Mus and SU Cyg |
| 14458 | David Jewitt, University of California - Los Angeles | Hubble Investigation of Active Asteroid 324P/La Sagra |
GO 13765: A Cepheid-Based Distance to the Benchmark AGN NGC 4151
Ground-based image of NGC 4151 |
NGC 4151 is an intermediate-type spiral lying at a distance of approximately 19 Mpc from the Milky Way. Originally catalogued by Sir John Heschel, spectrscopic observations in the early 20th century revealed the presence of strong emission lines associated with the nucleus. With NGC 1068, NGC 4151 became a prototype for the class of galaxies catalogued by Carl Seyfehrt. We now know that' these features are associated with the accretion of hot gas onto a central supermassive black hole. As one of the nearest such galaxies, NGC 4151 has been subject to intense observations over the last 50 years, including analyses of the mass of the central black hole through modeling gas and stellar dynamics, and through reverberation mapping. These two measurments should be compatible, but the former relies on having a good distaince estimate. At present, NGC 4151's distance is based on purely statistical correlation, such as the Tully-Fisher relation, and therefore known to an accuracy of only 20% at best. The present program aims to redress this situation by searching for long-period Cepheid variables. These variables have their highest amplitued variation at blue wavelengths, so the WFC3 UVIS camera is being sued to search for candidates. Follow-up observations are being obtained with the WFC3-IR camera, since the Cepheid period-luminosity relation is tighter at IR wavelengths, and observations less sensitive to foreground absorption by dust. |
GO 13046: RAISIN2: Tracers of cosmic expansion with SN IA in the IR
The first supernova discovered by the Pan-STARRs survey |
Supernovae are the most spectacular form of stellar obituary. In recent years, these celestial explosions have acquired even more significance through the use of Type Ia supernovae as distance indicators in mapping the `dark energy' acceleration term of cosmic expansion. However, while there are well-established models for the two main types of supernovae (runaway fusion on the surface of a white dwarf in a binary system for Type Ia, or detonation of the core in Type II), some uncertainties remain as to the uniformity of the events. Moreover, as the sample of known supernova has grown, so has the range of photometric systems and the methods used to fit the light curve and account for the ever-present uncertainites inroduced by dust absorption. Consequently, the potential remains for systematic bias in distance estimates due both to intrinsic differences and to measurement errors. The present program builds on a Cycle 21 program, and aims to minimise these systematics by compiling standard sequences of observations, primarily in the Y, J, and H filters, of supernovae at redshifts between z~0.3 and 0.5. Focusing on those wavelengths minises the effects, and hence the uncertainties, due to dust absorption. The supernovae themselves are drawn from the Pan-STARRS survey, with the WFC3-IR camera on HST employed to obtain the photometry. |
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 14340: Accurate masses and distances of the binary Cepheids S Mus and SU Cyg
The radial velocity curve (left) and pulsational velocity curve (middle) of the primary component of the binary Cepheid, V1334 Cyg (Gallene et al, A&A, 552, A21) |
SU Cygni and S Muscae are short-period (P = 3.8 days, 9.66 days) classical Cepheid variables lying at a distance of a few hundred parsecs from the Sun. Both are known binary systems, with SU Cyg harbouring a ~4 solar mass, B6 companion and S Muscae matched with a 3-5 solar mass, B3-B5 companion. At optical wavelengths, the combined flux is dominated by the cooler Cepheid in these systems, but hot companion is detectable at ultraviolet wavelengths. The present program aims to use STIS to obtain ultraviolet spectra that will enable measurement of the radial velocity curve for the hot companions in these systems. Those observations will be combined with existing ground-based measurements of the Cepheid radial velocities, therefore determing velocity curves for both stars. Combining those data with high-precision astrometric measurements from ground-based interferometry will allow a direct measurement of mass and distance for both systems. |