This week on HST

HST Programs: July 17 - July 23, 2017

Program Number Principal Investigator Program Title
14181 S Thomas Megeath, University of Toledo A Snapshot WFC3 IR Survey of Spitzer/Hershel-Identified Protostars in Nearby Molecular Clouds
14212 Karl Stapelfeldt, Jet Propulsion Laboratory A Snapshot Imaging Survey of Spitzer-selected Young Stellar Objects in Nearby Star Formation Regions*.t23
14597 Jay Farihi, University College London An Ultraviolet Spectral Legacy of Polluted White Dwarfs
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
14635 Yuri I. Izotov, Ukrainian National Academy of Sciences, MAO Lyman continuum leaking in luminous compact star-forming galaxies
14652 Benne Willem Holwerda, University of Louisville Research Foundation, Inc. Super-Eight: The brightest z~8 Galaxies
14654 Peter Milne, University of Arizona A Second Ladder: Testing for Bias in the Type Ia Distance Scale with SBF
14656 Ivana Orlitova, Astronomical Institute, Academy of Sciences of CR How does ionizing radiation escape from galaxies?
14672 Ruth C. Peterson, SETI Institute Tracing the Earliest Nucleosynthesis from Elements Just Past the Iron Peak in Extremely Metal-Poor Dwarfs
14681 Alessandra Aloisi, Space Telescope Science Institute Tracing Galactic Outflows to the Source: Spatially Resolved Feedback in M83 with COS
14702 Jeremy J. Drake, Smithsonian Institution Astrophysical Observatory The first mass and angular momentum loss measurements for a CV-like binary
14704 Charlie Conroy, Harvard University A Year in the Whirlpool
14707 Philip Louis Massey, Lowell Observatory Searching for the Most Massive Stars in M31 and M33
14710 Antonino Paolo Milone, Australian National University Multiple Stellar Populations in Young Magellanic Cloud Clusters
14720 Doron Chelouche, University of Haifa Photometric Mapping of the Galactic Outflow in NGC 7552
14737 Jiri Krticka, Masaryk University Unveiling the nature of the only main-sequence pulsar CU Vir
14742 Dieu D. Nguyen, University of Utah Improving Central Black Hole Mass Measurements in Low Mass Early Type Galaxies
14749 Mischa Schirmer, Gemini Observatory, Southern Operations Low redshift Lyman-alpha blobs
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
14772 Bart P. Wakker, University of Wisconsin - Madison Observing gas in Cosmic Web filaments to constrain simulations of cosmic structure formation
14774 Trent J. Dupuy, University of Texas at Austin Dynamical Masses for Free-Floating Planetary-Mass Binaries
14777 Nahum Arav, Virginia Polytechnic Institute and State University Deciphering Quasar Outflows and Measuring their Contribution to AGN Feedback
14779 Melissa Lynn Graham, University of Washington A NUV Imaging Survey for Circumstellar Material in Type Ia Supernovae
14784 Evgenya L. Shkolnik, Arizona State University HAZMAT: Habitable Zones and M dwarf Activity across Time
14840 Andrea Bellini, Space Telescope Science Institute Schedule Gap Pilot
15003 Joshua Kammer, Southwest Research Institute Stellar Occultation by 2014 MU69

Selected highlights

GO 14634: HST-Juno synergistic approach of Jupiter's magnetosphere and ultraviolet aurorae

Hubble ultraviolet image of auroral activity near Jupiter's north magnetic pole
Planetary aurorae are stimulated by the influx of charged particles from the Sun, which travel along magnetic field lines and funnel into the atmosphere near the magnetic poles. Aurorae therefore require that a planet has both a substantial atmosphere and a magnetic field. They are a common phenomenon on Earth, sometimes visible at magnetic latitudes more than 40 degrees from the pole, and have also been seen on Jupiter, Saturn, Uranus and Neptune. Jovian auroral activity is also affected by the Galilean satellites, which generate electric currents that can produce bright auroral spots (see figure), and, in some cases, have their own auroral storms. Hubble has monitored activity for more than two decades now, with a dedicated campaign during the International Heliosphysical Year (2007/2008) using the Advanced Camera for Surveys Solar Blind Channel. In 2011, NASA launched the JUpiter Near-polar Orbiter (JUNO) which will provide the first in situ measurements of Jupiter's magnetic field and polar magnetosphere since the Galileo satellite which actively monitored Jupiter from 1995 to 2003. Juno arrived at Jupiter on July 4th 2016 and entered a 53-day orbit. Hubble is obtaining a series of far-UV images using the Space Telescope Imaging Spectrograph (STIS). Those data complement the on-board instrumentation by providing global maps of auroral activity.

GO 14681: Tracing Galactic Outflows to the Source: Spatially Resolved Feedback in M83 with COS

WFC3 image of star forming regions in M83
M83 is a grand design barred spiral galaxy lying almost face-on at a distance of ~4.5 Mpc from the Milky Way. Lying in the southern constellation of Hydra, the galaxy was originally discovered by the French astronomer Nicolas Louis de LaCaille from observations at the Cape of Good Hope in 1752, before being catalogued by Messier in 1781. The galaxy lies towards the centre of one of the two sub-groups of the Centaurus A association, and has a total luminosity estimated as ~2 x 1010LSun, or comparable with that of the Milky Way. As a nearby galaxty, M83 has been well observed by both amateurs and professonal astronomers, and has been the site of six SNe over the last century (SN 1923A, 1945B, 1950B, 1957D, 1968L and 1983N). At least four of these supernovae are classed as Type II, indicating their origin as massive stars (SN45B has few observations and SN1983N was a peculiar type I) and testifying tot he extensive star formation currently under way within the galaxy. The present program aims to investigate the global star-formation characteristics through spatially-resolved ultraviolet spectroscopic observations of individual star clusters within the disk. The observations will be made with the Cosmic Origins Spectrograph using the G130M and G160M gratings, covering the wavelength range 1130 to 1800 Angstroms. Those data will be matched against simulations and used to constrain the overall star formation within the spiral galaxy.

GO 14779: A NUV Imaging Survey for Circumstellar Material in Type Ia Supernovae

A recent supernova in M100
Supernovae mark the (spectacular) evolutionary endpoint for a subset of stellar systems. The final stages of evolution (or, more accurately, disruption) see the system eject substgantial masses of material into the interstellar medium. In at least some systems, those ejecta interact with circumstellar material produced during the evolutionary phases immediately prior to the system becoming a supernova. Theoretical expectations are that around 20% of SNe should possess such materials, but the expected iteractions have only brrn observed rarely. This may be because the material lies at relatively large distances from the star leading to longer lead times (>1 year) before the interactions. The present program aims to test this hypothesis through NUV snapshot observations with the WFC3/UVIS camera, targetting the sites of supernovae that erupted from 1 to 3 years ago.

GO 15003: Stellar occultation by 2014 2MU69

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 is redirecting 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 diameter 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. Stellar occultations provide very precise measurements of the location of asteroids and KBOs relative to the Earth. Consequently, these encounters can be used to refine the orbital parameters for the prime target to optimize the New Horizon encounter. In addition, the detailed light curve can be used to search for rings or debris around the KBO. The present observations target an encounter with e 12th magnitude K giant.

Past weeks:
page by Neill Reid, updated 2 /1/2017
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