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.
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.0Assigned ID: 5050
----- Attempting Submission 1 (Fri Mar 22 16:55:08 GMT 2024) -----
HST Phase I Proposal 5050 successfully submitted.
Receipt: # 5050-1
----- Attempting Submission 2 (Tue Mar 26 13:35:52 GMT 2024) -----
HST Phase I Proposal 5050 successfully submitted.
Receipt: # 5050-2I am aware of the COS G160M requirements at LP6 and have accounted for them in my overheads.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
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
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
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.
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.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
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.
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.
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.
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.
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.
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 OVERRUNResubmitting with two new visits following HOPR 93522 (approved on 4/3/26).
The new observations are Visit 24 (2 orbits; a repeat of Visit 14) and Visit 26 (1 orbit; a repeat of orbit #1 from Visit 16). The exposure times have been reduced by ~30s to avoid orbital visibility over-runs.-630757484----- Attempting Submission 1 (Fri Aug 02 13:22:30 GMT 2024) -----
----- Attempting Submission 2 (Fri Mar 21 12:30:14 GMT 2025) -----
----- Attempting Submission 3 (Wed Apr 09 12:49:55 GMT 2025) -----
----- Attempting Submission 4 (Mon Apr 06 13:26:33 GMT 2026) -----I am resubmitting a version with 2 new visits following HOPR 93522.
This is creating warnings for orbital visibility overruns and FP-POS issues from visits that have already executed. So this should not be a problem.Locating Clouds in the Milky Way's Nuclear OutflowRecent HST/COS observations have discovered outflowing cool gas clouds in the Milky Way's nuclear wind. While their chemical compostion, covering fraction, and kinematics have been characterized, their distance is largely unconstrained, so we do not know where along each line of sight the cool gas clouds are located. Without the distance to the clouds, we cannot definitively associate them with the Fermi or eROSITA Bubbles (the giant gamma-ray and X-ray structures created by a nuclear outburst) or reconstruct the history of the nuclear outflow. We have designed a novel experiment to determine the distance to the cool clouds using HST/COS observations of a sample of six blue horizontal branch (BHB) stars projected onto the Fermi and eROSITA Bubbles. The targets are chosen to lie at a range of distances from 4.7 to 9.5 kpc, with two targets inside the Bubbles and four in the foreground. By bracketing the location of high-velocity clouds (HVCs) seen in UV metal absorption lines (Si II, Si IV, C IV, Fe II) in the BHB spectra, we will determine whether the clouds arise inside or in front of the Bubbles. A detection of HVCs in both the foreground and background sightlines would place the clouds in front of the Bubbles. A detection in the background but not the foreground sightlines would place the clouds within the Bubbles or at their boundaries. We also request deep H I 21 cm spectra of each direction from the Green Bank Telescope to constrain the velocities and locations of the neutral gas in the HVCs, which directly aids our science goals. This experiment provides a method for mapping the spatial distribution of high-velocity gas in the Galactic halo.This is a COS FUV program to observe six blue horizontal branch (BHB) stars toward the Galactic Center, with the science goal of detecting foregound gas in absorption in several UV metal lines (particularly Si IV 1393, 1402 and C IV 1548, 1550).
Each target will be acquired with a NUV ACQ/IMAGE with the PSA and MIRRORB, followed by science observations with the G160M/1577 setting. For each target, the four FP-POS positions will be obtained either in one visit or spread across two visits. All visits are either 2 or 3 orbits in length, following the guidance from the PC.The PI Dr Andrew Fox is an expert in the analysis and interpretation of HST/COS 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 Rongmon Bordoloi is an expert on the Fermi Bubbles, Galactic winds, and the circumgalactic medium, and has first-authored several ApJ papers on these subjects.
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 Alex Fullerton has decades of experience analyzing UV spectra of massive stars from IUE, FUSE, and HST with expertise in in separating stellar and interstellar absorption lines.
Dr Ed Jenkins is an expert on UV spectroscopy and its use to characterize the physical and chemical properties of the interstellar and intergalactic media.
Dr Tanveer Karim is an expert on observational studues of the Fermi Bubble HVCs having published a first-author paper on this subject.
Dr Jay Lockman has decades of experience of radio studies of gas in the ISM and CGM and is an expert on the Fermi Bubbles and the nuclear wind.
Dr Jessica Werk is an expert on COS FUV spectroscopy of BHB stars and the separation of stellar and interstellar features in their spectra and an acknowledged expert on the CGM.
Dr Sara Cazzoli is an expert on observations of galactic winds, particularly AGN-driven winds and their physical and chemical properties.Intergalactic Medium and the Circumgalactic MediumStellar Populations and the Interstellar Medium6falsetruefalsefalsefalsefalsefalsetruePRIMARY3.25trueSUPPORTEDISMABSORPTION LINE SYSTEM - GALACTICHIGH VELOCITY CLOUDINTERMEDIATE VELOCITY CLOUDNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=17.74 NUV=16.77ISMABSORPTION LINE SYSTEM - GALACTICHIGH VELOCITY CLOUDINTERMEDIATE VELOCITY CLOUDNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=17.17 NUV=16.79ISMABSORPTION LINE SYSTEM - GALACTICHIGH VELOCITY CLOUDINTERMEDIATE VELOCITY CLOUDNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=18.08 NUV=17.43ISMABSORPTION LINE SYSTEM - GALACTICHIGH VELOCITY CLOUDINTERMEDIATE VELOCITY CLOUDNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=18.19 NUV=17.72ISMABSORPTION LINE SYSTEM - GALACTICHIGH VELOCITY CLOUDINTERMEDIATE VELOCITY CLOUDNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=17.80 NUV=16.93ISMABSORPTION LINE SYSTEM - GALACTICHIGH VELOCITY CLOUDINTERMEDIATE VELOCITY CLOUDNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=17.54 NUV=16.97COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode./private/var/folders/tk/3gx7p0k112l_9pg4glzb8hhh00015x/T/OPVisit15131141531115551460.xml1742581834000266.6895940611938(Tic-Visit
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