Updated Team Expertise.-300393381Assigned ID: 198
----- Attempting Submission 1 (Thu Mar 05 00:45:49 GMT 2020) -----
HST Phase I Proposal 198 successfully submitted.
Receipt: # 198-1
----- Attempting Submission 2 (Fri Mar 06 23:00:49 GMT 2020) -----Resubmitting Phase II because we need to do a repeat observation of target J01415 because the shutter was closed for one orbit's worth of observations. This new observation is labled as #54.-870122347----- Attempting Submission 1 (Wed Jun 17 19:31:53 GMT 2020) -----
----- Attempting Submission 2 (Mon Nov 23 22:13:29 GMT 2020) -----Exploring the origin of the M31-M33 filamentBetween M31 and M33 lies a debris field of HI clouds. These clouds may represent a tidal remnant from a past interaction between M31 and a satellite galaxy, a population of satellite galaxies, halo gas condensations, cooling gas along an intergalactic medium filament, or M31 stellar or weak AGN feedback. We request HST/COS UV absorption-line and coordinated GBT HI emission-line observations along 2 UV bright background QSO sightlines to conduct a detailed investigation of the chemical composition, dust depletion patterns, and kinematics of the M31-M33 clouds to constrain their origin. Using the requested observations, along with archival observations, we will further measure their ionization properties to determine the relative influence of the surrounding coronal gas and the incident radiation field has on them. Combined, this will enable us to assess where this gas came from, how much material it contains in neutral and ionized gas, and whether this stream could survive a journey to M31. This study will provide insight on how L* galaxies replenish their gas reservoirs by measuring the physical properties of material that is inflowing onto M31 in absorption- and emission-line spectroscopy out to 1/3 of a virial radius.This is a 12-orbit proposal to observe two background QSO targets that lie between M31-M33.
For all visits, we begin with an ACQ SEARCH followed by an ACQ IMAGE, which are then both followed by science observations. For all sceince observations, we use 2 FP-POS positions (positions 3 and 4) to dither the placing of the spectrum on the COS G130M grating with central wavelength set to 1291 AA.
V01 to V03 observes QSO (GALAX-J010328.6+354730, z=0.525) for a total of 10 orbits. We split these into 3 visits with V01 having 4 orbits and V01 and 2 both having 3 orbits.
V04 observes a QSO (GALAX-J010415.8+402243, z=0.193) for 2 orbits.
There are no scheduling constraints on any of the visits. All targets passed the instrument bright target checks such that they are below the COS brightness limits.PI Kat Barger has considerable spectroscopic expertise spanning multiple wavelength ranges, including radio (HI 21-cm), optical nebular lines, and UV with HST COS/STIS. She has led and is leading projects on numerous gas streams that are flowing onto the Milky Way, including the Magellanic Cloud, Leading Arm, Complex A, and the Smith Cloud. She is also leading the HST 15161 project entitled "The fate of infalling gas during its final approach onto the Milky Way disk." She will led the overall project efforts, especially on the UV spectroscopy front.
CoI Andrew Fox is an expert in UV absorption-line spectroscopy and have substantial amount experience investigating the gas cycle in the Milky Way, the Magellanic Clouds, and distant galaxies. Fox has also led numerous HST projects, including HST 12604 entitled "Ionization in the Magellanic Stream: A Case Study of Galactic Accretion" and HST 13840 entitled "The Smith Cloud: Galactic or Extragalactic?".
CoI Bart Wakker has an extensive background in studies of the interstellar and intergalactic medium, having published over 100 papers on these subjects. He has worked with published many paper using data from ground-based radio and optical telescopes, as well as many of the UV space instruments (IUE, FUSE, FOS, GHRS, STIS, COS), being PI on 11 HST observing and 4 HST archival projects, as well as Co-PI or Admin-PI on 7 others. After originally working on gas clouds near the Milky Way, he has moved to specializing in analyzing gas clouds in the local universe, both around galaxies and in the Cosmic Web. Wakker will assist with the data reduction (including night only observations) and UV spectroscopic analysis.
CoIs Felix J. Lockman, Daniel J. Pisano, Spencer Wolfe all have substantial experience studying the circumgalactic medium Local Group galaxies in HI with the Green Bank Telescope (GBT). This is the team that is leading the GBT mapped observations of the gas cloud population between M31 and M33, which resulted in a 2013 Nature article entitled "Discrete clouds of neutral gas between the galaxies M31 and M33" (Spencer et al. 2013). Further, Lockman was the GBT site director for 6 years. These CoIs will led the GBT HI efforts.
Elena D'Onghia has led numerous galaxy simulation projects, including hydrodynamical simulations to decipher past interacts between the Magellanic Clouds and between M31 and M33. These simulations explore numerous initial conditions to determine what parameters reproduce the observed systems. D'Onghia will led the galaxy simulation efforts, helping us to explore the physical properties of the gas clouds for different origin scenarios.Intergalactic Medium and the Circumgalactic Medium6falsefalsetruefalsefalsefalse3.9trueSUPPORTEDISMABSORPTION LINE SYSTEM - EXTRAGALACTICFILAMENTHIGH VELOCITY CLOUDIGMTIDAL TAILNOThis object was generated by the target selector and retrieved from the GALEX database.J2000J2000V=15.4 mag, FUV=18.83 mag, NUV=17.57 magISMABSORPTION LINE SYSTEM - EXTRAGALACTICFILAMENTHIGH VELOCITY CLOUDIGMTIDAL TAILNOThis object was generated by the targetselector and retrieved from the GALEX database.J2000J2000g=15.91 mag, FUV=16.79 mag, NUV=16.38 magCOS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.160646846300093.37(Tic-Visit
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