| Program Number | Principal Investigator | Program Title |
|---|---|---|
| 13646 | Ryan Foley, University of Illinois at Urbana - Champaign | Understanding the Progenitor Systems, Explosion Mechanisms, and Cosmological Utility of Type Ia Supernovae |
| 13702 | Sally Oey, University of Michigan | Mapping the LyC-Emitting Regions of Local Galaxies |
| 13740 | Daniel Stern, Jet Propulsion Laboratory | Clusters Around Radio-Loud AGN: Spectroscopy of Infrared-Selected Galaxy Clusters at z>1.4 |
| 13757 | Saurabh W. Jha, Rutgers the State University of New Jersey | The Progenitor System of a Peculiar Thermonuclear White-Dwarf Supernova |
| 13760 | Derck L. Massa, Space Science Institute | Filling the gap --near UV, optical and near IR extinction |
| 13763 | S. Thomas Megeath, University of Toledo | WFC3 Spectroscopy of Faint Young Companions to Orion Young Stellar Objects |
| 13765 | Bradley M Peterson, The Ohio State University | A Cepheid-Based Distance to the Benchmark AGN NGC 4151 |
| 13783 | George G. Pavlov, The Pennsylvania State University | Thermal evolution of old neutron stars |
| 13856 | Denija Crnojevic, Texas Tech University | Resolving the faint end of the satellite luminosity function for the nearest elliptical Centaurus A |
| 14038 | Jennifer Lotz, Space Telescope Science Institute | HST Frontier Fields - Observations of Abell 370 |
| 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 |
| 14084 | Seth Redfield, Wesleyan University | Connecting Earth with its Galactic Environment: Probing Our Interstellar Past Along the Historical Solar Trajectory |
| 14089 | Paul A. Wilson, CNRS, Institut d'Astrophysique de Paris | Far-UV observations of H, C, N and O in exocomets of Beta Pic |
| 14098 | Harald Ebeling, University of Hawaii | Beyond MACS: A Snapshot Survey of the Most Massive Clusters of Galaxies at z>0.5 |
| 14102 | Claus Leitherer, Space Telescope Science Institute | The II Zw 40 Supernebula: 30 Doradus on Steroids |
| 14110 | David Kent Sing, University of Exeter | Charaterizing the atmosphere of the enlarged Neptune-mass planet HAT-P-26b |
| 14118 | Luigi R. Bedin, Osservatorio Astronomico di Padova | The end of the White Dwarf Cooling Sequences of Omega Centauri |
| 14134 | Swara Ravindranath, Space Telescope Science Institute | Spectral Diagnostics for the Reionization Era: Exploring the Semi-Forbidden CIII] Emission in Low Metallicity Green Pea Galaxies |
| 14141 | Guy Worthey, Washington State University | NGSL Extension 1. Hot Stars and Evolved Stars |
| 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 |
| 14189 | Adam S. Bolton, University of Utah | Quantifying Cold Dark Matter Substructure with a Qualitatively New Gravitational Lens Sample |
| 14193 | Catherine Espaillat, Boston University | Footprints of the Magnetosphere: the Star- Disk Connection in T Tauri Stars |
| 14206 | Adam Riess, The Johns Hopkins University | A New Threshold of Precision, 30 micro-arcsecond Parallaxes and Beyond |
| 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 |
| 14227 | Casey Papovich, Texas A & M University | The CANDELS Lyman-alpha Emission At Reionization (CLEAR) Experiment |
| 14234 | Joshua D. Simon, Carnegie Institution of Washington | The Lowest Luminosity Star-Forming Galaxy |
| 14241 | Daniel Apai, University of Arizona | Cloud Atlas: Vertical Cloud Structure and Gravity in Exoplanet and Brown Dwarf Atmospheres |
| 14251 | Amy E. Reines, National Optical Astronomy Observatory, AURA | The Structures of Dwarf Galaxies Hosting Massive Black Holes |
| 14259 | Denija Crnojevic, Texas Tech University | Resolved halo substructures beyond the Local Group: the assembly histories of NGC 253 and NGC 5128 |
| 14262 | Knud Jahnke, Max-Planck-Institut fur Astronomie, Heidelberg | Are the fastest growing black holes at z=2 caused by major galaxy mergers? |
| 14327 | Saul Perlmutter, University of California - Berkeley | See Change: Testing time-varying dark energy with z>1 supernovae and their massive cluster hosts |
| 14465 | Jonathan Charles Tan, University of Florida | Peering to the Heart of Massive Star Birth |
| 14474 | David Jewitt, University of California - Los Angeles | Comet P/2010 V1 fragmentation event |
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 14084: Connecting Earth with its Galactic Environment: Probing Our Interstellar Past Along the Historical Solar Trajectory
The Sun's path through the local interstellar medium |
The Sun's motion around the Galaxy takes it through a range of environments within the interstellar medium.At the present time the Sun lies on the edge of the "Local Bubble", a region of very low gas density. Its recent motions took it through a cloud of interstellar material that is moving radially outward within the disk. It is not clear how, or indeed whether, the local ISM has a significant effect on solar heliosphere and the individual bodies in the Solar System, including Earth. The present program aims to explore that issue through high resolution ultraviolet spectroscopy of eight stars that lie in the direcion of the Sun's past motion. These stars serve as backlights to the local ISM, whose component elements manifest themselves by absorbing the stellar light. The observations will use the Cosmic origins Spectrograph to search for characteristics features due to ionised Fe II and Mg II. |
GO 14212: A Snapshot Imaging Survey of Spitzer-selected Young Stellar Objects in Nearby Star Formation Regions
HST image of the face-on debris disk in the G2 dwarf, HD 107146 |
Planet formation occurs in circumstellar disks around young stars. Most of the gaseous content of those disks dissipates in less than 10 million years, leaving dusty debris disks that are detectable through reflect light at near-infrared and, to a lesser extent, optical wavelengths. The structure of those disks is affected by massive bodies (i.e. planets and asteroids), which, through dynamical interactions and resonances, can produce rings and asymmetries. Analysis of the rangle of morphological structure in these systems provides insight into the distribution of properties of planetary systems. HST currently provides almost the only means of achieving the high-contrast required for the detection of scattered light from these disks in the presence of the bright parent stars. While many such systems have been observed, only a relatively small number of disks have been imaged successfully at visual or near-infrared wavelengths. The present SNAPSHOT program aims to expand the sample by targetting sources within nearby star-forming regions that have past Spitzer observations that indicate a significant infra-red excess, suggesting the presence of a circumstellar disk.The Advanced Camera for Surveys will be used to obtain images in the V and I-bands (F606W and F814W filter), providing high resolution data that can be analysed for direct evidence of disks or companions. |
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. |