0Assigned ID: 191
----- Attempting Submission 1 (Thu Apr 04 14:43:02 GMT 2019) -----
HST Phase I Proposal 191 (chvc-c27.apt) successfully submitted.
Receipt: # 191-1
----- Attempting Submission 2 (Thu Apr 04 14:53:32 GMT 2019) -----
HST Phase I Proposal 191 (chvc-c27.apt) successfully submitted.
Receipt: # 191-2Comments on 10/12/20: Resubmitting with new Visit 59 (one orbit) to repeat failed final orbit of Visit 09 (see HOPR 91885).
Resubmitting with longer exposure times for ACQ/SEARCH exposures 03.001 and 04.001 following discussion with CS Bethan James. Now using 80s instead of 17s. Exposure times for science exposures 03.003 and 04.003 have been reduced accordingly to fit the orbits.-432450875----- Attempting Submission 1 (Tue Jul 23 13:48:02 GMT 2019) -----
----- Attempting Submission 2 (Wed Oct 02 16:41:34 GMT 2019) -----
----- Attempting Submission 3 (Mon Oct 12 20:05:23 GMT 2020) -----I have run the Visit Planner.The Nature and Origin of Compact High-Velocity CloudsGalaxy evolution is driven by the exchange of gas between disks and the surrounding circumgalactic medium. The physics governing this exchange depends on small-scale structure in the gas. This structure can be studied in detail in the Milky Way halo, which hosts a population of ~200 poorly understood compact high-velocity clouds (CHVCs) each spanning less than two degrees on the sky. Almost everything we know about CHVCs comes from 21 cm radio observations. To broaden our understanding and fully characterize their properties, we propose a UV absorption-line survey. We have selected a sample of 5 CHVCs from the Galactic All Sky Survey (GASS) and identified a UV-bright AGN that lies directly behind each cloud. Using HST/COS observations we will study the CHVCs in absorption in a wide range of UV metal lines, allowing us to probe their metallicity, ionization level, dust content, and kinematics. Together, these measurements will provide key new constraints on the origin of CHVCs, allowing us to discriminate between extragalactic origins (low metallicities and simple kinematics), Galactic origins (high metallicities and complex kinematics) and Magellanic origins (intermediate metallicity). Finally, this proposal will establish empirical constraints on MW halo gas at cloud scales that are just being reached by state-of-the-art hydrodynamical simulations of the circumgalactic medium.
We also request Green Bank Telescope 21 cm pointings in each AGN direction under the joint HST/NRAO category to obtain the reference H I column densities at high spatial resolution and sensitivity.This is a straightforward COS/FUV program to observe 5 AGN with the G130M/1222 and G160M/1533 settings, in order to study Milky Way halo clouds in absorption. Each target will be observed with an NUV ACQ/IMAGE (all with MIRRORB) followed by the TIME-TAG science exposures. We use all four FP-POS positions per cenwave and one grating per visit. The visits are between 2 and 4 orbits long. For Visits 03 and 04 (target UVQSJ011054-154540), a 2x2 ACQ/SEARCH is included before the ACQ/IMAGE since the coordinates are less well known than for the other four targets.All team members have considerable experience with the observation, analysis, and interpretation of UV datasets on gas in and around galaxies.
The PI Dr Andrew Fox is an expert in the reduction, analysis, and interpretation of HST/COS spectra of diffuse gas in the Universe. He has led four HST GO proposals in CGM-related science, all of which have led to refereed publications and NASA press releases, and has first-authored 11 ApJ papers using UV spectroscopy. He will oversee the analysis and manage the contributions of the Co-Is.
Dr 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 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. He will lead the data reduction and spectral co-addition.
Dr Jay Lockman has decades of experience of radio studies of gas in the ISM and CGM and is the Green Bank Telescope Principal Scientist. He will lead the GBT H I component of the proposal.
Dr Vanessa Moss has led the analysis of the CHVC catalog drawn from the Galactic All-Sky Survey (GASS) and is an expert on the H I properties of the HVCs, including their kinematics.
Dr Naomi Mc-Clure Griffiths is the PI of GASS, from which the CHVCs in our sample were drawn, and an expert on the properties of HI in the ISM.
Dr Trisha Ashley is an expert on the H I properties of dwarf galaxies, the interpretation of velocity fields, star formation, and blue compact dwarf galaxies.
Dr David French has just finished a PhD thesis based on data from COS, studying the Lyman alpha absorption lines associated with nearby galaxies.
Prof. Philipp Richter is also a highly experienced UV spectroscopist with decades of expertise on deriving chemical and physical conditions of interstellar and circumgalactic gas.
Dr Jason Tumlinson is a highly experienced UV user and global expert in galaxy formation and evolution, and is the PI of the COS-Halos and COS-Dwarfs programs on the CGM.
Dr Molly Peeples is an expert on the circumgalactic medium and the PI of the FOGGIE suite of high-resolution numerical simulations of galaxy formation. These models are predicting objects that look like Compact HVCs.Galaxies and the IGM6falsefalsetruefalsefalsefalse2.5trueSUPPORTEDISMABSORPTION LINE SYSTEM - GALACTICCORONAL GASHIGH VELOCITY CLOUDNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALEX FUV=16.88 NUV=16.59ISMABSORPTION LINE SYSTEM - GALACTICCORONAL GASHIGH VELOCITY CLOUDNOJ2000J2000GALEX FUV=17.94 NUV=17.38ISMABSORPTION LINE SYSTEM - GALACTICCORONAL GASHIGH VELOCITY CLOUDNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALEX FUV=17.14 NUV=16.76ISMABSORPTION LINE SYSTEM - GALACTICCORONAL GASHIGH VELOCITY CLOUDNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALEX FUV=17.27 NUV=17.19ISMABSORPTION LINE SYSTEM - GALACTICCORONAL GASHIGH VELOCITY CLOUDNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALEX FUV=17.81 NUV=17.66COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.1593198746000249.56674472712348(Tic-Visit
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