For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.Third Version.
Observations in G160M LP6 are ok since they all are >1 orbits.295351773Assigned ID: 5190
----- Attempting Submission 1 (Mon Mar 25 16:00:59 GMT 2024) -----
HST Phase I Proposal 5190 successfully submitted.
Receipt: # 5190-1
----- Attempting Submission 2 (Tue Mar 26 01:40:23 GMT 2024) -----
HST Phase I Proposal 5190 successfully submitted.
Receipt: # 5190-2
----- Attempting Submission 3 (Tue Mar 26 17:20:44 GMT 2024) -----
HST Phase I Proposal 5190 successfully submitted.
Receipt: # 5190-3G160M observations confirmed to be ok on LP6.For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.HOPR for Visit 02 and Visit 03-1783455364----- Attempting Submission 1 (Wed Aug 14 20:19:59 GMT 2024) -----
----- Attempting Submission 2 (Wed Jan 14 16:04:06 GMT 2026) -----
HST Phase II Proposal 17757 successfully submitted.
Receipt: # 17757-2
----- Attempting Submission 3 (Wed Jan 14 16:05:23 GMT 2026) -----SMProbing the front-side of the Circumgalactic Medium of the Large Magellanic CloudRecent simulations and observations have provided evidence for a warm-hot phase of the Large Magellanic Cloud (LMC)'s circumgalactic medium (CGM), known as the Magellanic Corona. This Corona shields the LMC from the effects of ram pressure stripping by the Milky Way (MW), but to date, all observations of the Corona have been on the back-side of the LMC CGM. Here we propose 29 orbits of HST/COS G130M/G160M spectroscopic observations of 5 recently-discovered low-latitude (|b|<30 degrees) UV-bright quasars to observe the front-side of the LMC CGM. Aiming to explore both warm-hot and cool phases of the LMC CGM through high and low ion UV metal absorption lines, our goals are to: (1) Detect and characterize the LMC CGM on the uncharted front-side. (2) Compare the LMC CGM between its backand front-sides, providing novel insights into the dynamics of interacting galaxies. (3) Combine these observations with hydrodynamical simulations to constrain the properties of MW CGM, Megellanic CGM, and bow shock region. This research promises to advance our understanding on the ongoing evolution of the interacting galaxies within the Local Group.This is a COS FUV program to observe five QSO targets behind the LMC using G130M and G160M. The science goal is detecting the LMC halo in absorption in a range of UV metal lines.
Each target will be acquired with a NUV ACQ/IMAGE with the PSA and MIRRORB, followed by science observations with the G130M/1291 and G160M/1577 settings. For the G160M observations, the four FP-POS positions will be obtained either in one visit or spread across two visits. All visits are up to 3 orbits in length, following the guidance from the PC.Dr Frances Cashman is an expert on the ISM and IGM and on Cloudy simulations of interstellar absorbers, and the properties of interstellar gas near the Galactic Center.
Dr Elena D'Onghia is an expert on galaxy evolution and on the dynamical evolution of the Magellanic System. She led a 2016 Annual Reviews article on the Magellanic Stream.
Dr Andrew Fox is an expert in the gaseous halos of galaxies and the analysis of UV spectra. He has led seven HST GO and two AR proposals, and has first-authored over 20 refereeed journal papers in related fields. He will coordinate and oversee the analysis and manage the Co-I contributions.
Dr David French is an expert in UV data reduction, analysis, and interpretation, with particular emphasis on the local CGM. He has led two HST archival proposals on CGM related science, resulting in 3 referred publications. He has extensive experience with UV space instruments including HST/COS, HST/STIS, and FUSE.
Dr Dhanesh Krishnarao is an expert with modeling the Magellanic CGM. He is leading the analysis of the high ions in the Magellanic Corona from HST archival program 16363.
Dr Scott Lucchini is an expert on simulations of the Magellanic System. He has published two papers on this subject (one in Nature and one in ApJL). He will lead the ram pressure simulations in this program.
The PI Dr Sapna Mishra is an expert in UV and optical quasar absorption line spectroscopy, with a focus on studying the LMC, IGM, CGM, galaxy cluster outskirts and quasar outflows. She is leading the analysis on the cool CGM of the LMC from HST archival program 17053.
Dr Jessica Werk is an expert in COS observations, COS data reduction, COS spectral analysis, and inferring column densities and physical properties from COS and other spectroscopic absorption line data.
CoIs Dr Chris Howk and Dr Nicolas Lehner have extensive experience leading large-scale studies of the IGM and CGM at both low and high redshifts, as well as investigations of the ISM in nearby galaxies, and the high-velocity population in the Milky Way halo. They will use their expertise to help infer the origin of the observed absorption features in the low latitude quasar spectra. Many of these projects have resulted in the release of valuable data products to the community through the igmspec database (http://github.com/specdb), CDS/Vizier, and the NASA Keck Observatory Archive (KOA).Intergalactic Medium and the Circumgalactic MediumGalaxies6falsetruefalsefalsefalsefalseSUPPORTEDISMABSORPTION LINE SYSTEMABSORPTION LINE SYSTEM - EXTRAGALACTICABSORPTION LINE SYSTEM - GALACTICCORONACORONAL GASNOThis object was generated by the targetselector and retrieved from the GALEX database.
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