0Assigned ID: 953
----- Attempting Submission 1 (Fri Apr 07 21:51:45 GMT 2017) -----For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
INEFFICIENT ORDERING OF FP-POS POSITIONS
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
INEFFICIENT ORDERING OF FP-POS POSITIONS
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.Created Visits 29 and 30 to replace failed portions of VIsit 17 and 25.
As approved by Andy Fox.-314104940----- Attempting Submission 1 (Sat Jul 15 01:47:38 GMT 2017) -----
HST Phase II Proposal 15180 (elg_phaseII.apt) successfully submitted.
Receipt: # 15180-1
----- Attempting Submission 2 (Tue Jul 18 16:44:59 GMT 2017) -----
----- Attempting Submission 3 (Wed Jul 11 20:33:12 GMT 2018) -----
HST Phase II Proposal 15180 (ELG_c25_11july2018.apt) successfully submitted.
Receipt: # 15180-3
----- Attempting Submission 4 (Fri Jul 13 14:27:35 GMT 2018) -----
----- Attempting Submission 5 (Mon Sep 10 15:06:28 GMT 2018) -----
----- Attempting Submission 6 (Wed Dec 05 21:15:54 GMT 2018) -----
HST Phase II Proposal 15180 (ELG_c25_05dec2018.apt) successfully submitted.
Receipt: # 15180-6
----- Attempting Submission 7 (Mon Jun 17 18:27:55 GMT 2019) -----Warnings are now limited to FP-POS on NUV exposures.
These are deemed acceptible.ELGs in Absorption: Tracing the Cosmic Baryon Cycle from Noon til DuskFar beyond the visible star formation in galaxies, the circumgalactic medium (CGM) regulates the gaseous inflows and outflows that compete continuously over billions of years to drive galaxy formation and evolution. Successful programs carried out with the Cosmic Origins Spectrograph on HST have resolved the bulk baryonic content, spatial distribution, and chemical enrichment of the CGM surrounding z~0 galaxies with a diverse range of stellar masses and star formation histories. Complimentary studies with optical spectrometers on the ground have probed the CGM of star-forming galaxies and the massive galaxies hosting quasars at z~2. With this proposal, we will examine evolution (or lack thereof) in the CGM of star-forming z~1 galaxies (ELGs or emission-line galaxies) -- the central focus of several major, upcoming cosmological experiments (e.g. DESI, Euclid). We have identified 25 ELGs in the foreground of 24 z~1, bright quasars that will sample the CGM of star-forming galaxies at the peak epoch of galaxy evolution, when average star formation rates were higher than today and when z ~ 0 passive galaxies were likely undergoing their quenching. With this study, we will characterize the ionization state, gas kinematics, and covering fraction of the enriched gas that will ultimately go on to form the bulk of today's visible stars. Our sample will combine with a Cycle 24 sample of Large Red Galaxies to form a systematic study of the CGM in star forming and passive galaxies and establish a 4-6 Gyr timeline in CGM/galaxy interactions.As described in our Phase I proposal, we wish to obtain spectra for each of our
quasars from the rest-frame Lyman limit of the target galaxies (~1370A observed)
to approximately 1330A rest (or ~2450A observed).
This wavelength coverage is to be achieved by observing with (i) the G160M grating
with CENWAVE=1577A, (ii) the G230L grating with CENWAVE=3000A and
(iii) the G230L grating with CENWAVE=3360A. We then estimated exposure times
to achieve S/N=10 per R=2500 resolution element at 1500A, 1880A, and
2250A respectively. For the G160M grating, this implies binning up the spectra;
we chose this grating for its higher effective area.
For acquisitions, we adopted the GALEX NUV magnitudes
reported for each QSO and assumed a flat continuum. We
recover very similar results if we adopt a QSO spectrum at z=1.
The ETC for each is given and our brightest ~5 sources required
MIRROR-B to avoid WARNINGs.
For the spectra, we ran the ETC for our brightest source to
check for WARNINGs and the minimum buffer time. In all cases,
we use BUF times that are considerably larger than these minima.
Here are the ETCs for the spectra (also given in the Visits):
G160M
http://etc.stsci.edu/etc/results/COS.sp.1009367/
G230L_3000
http://etc.stsci.edu/etc/results/COS.sp.1009365/
G230L_3360
http://etc.stsci.edu/etc/results/COS.sp.1009366/
All G160M data were taken with all FP-POS.
With only a few exceptions, the G230L data were
taken with 2 or more FP-POS (mainly 2 orbit targets
where the extra overhead was deemed not worth it).
We found overheads were minimized by taking NUV spectra
after the AQC images (i.e. Orbit 1) and by starting the G160M
spectra at the start of Orbit 2 (or 3).Galaxies and the IGM6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYQSONOELGQSO01J2000J2000Magnitude is NUVGALAXYQSONOELGQSO2J2000J2000Magnitude is NUVGALAXYQSONOELGQSO3J2000J2000Magnitude is NUVGALAXYQSONOELGQSO4J2000J2000Magnitude is NUVGALAXYQSONOELGQSO5J2000J2000Magnitude is NUVGALAXYQSONOELGQSO6J2000J2000Magnitude is NUVGALAXYQSONOELGQSO07J2000J2000Magnitude is NUVGALAXYQSONOELGQSO8J2000J2000Magnitude is NUVGALAXYQSONOELGQSO9J2000J2000Magnitude is NUVGALAXYQSONOELGQSO10J2000J2000Magnitude is NUVGALAXYQSONOELGQSO11J2000J2000Magnitude is NUVGALAXYQSONOELGQSO12J2000J2000Magnitude is NUVGALAXYQSONOELGQSO14J2000J2000Magnitude is NUVGALAXYQSONOELGQSO15J2000J2000Magnitude is NUVGALAXYQSONOELGQSO16J2000J2000Magnitude is NUVGALAXYQSONOELGQSO17J2000J2000Magnitude is NUVGALAXYQSONOELGQSO18J2000J2000Magnitude is NUVGALAXYQSONOELGQSO19J2000J2000Magnitude is NUVGALAXYQSONOELGQSO20J2000J2000Magnitude is NUVGALAXYQSONOELGQSO21J2000J2000Magnitude is NUVGALAXYQSONOELGQSO22J2000J2000Magnitude is NUVGALAXYQSONOELGQSO23J2000J2000Magnitude is NUVGALAXYQSONOELGQSO24J2000J2000Magnitude is NUVCOS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360The scheduling data was generated by CASM 26.0.CASM was run in Phase II mode.154098973400065.6721370702553(Tic-Visit
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