0Assigned ID: 1003
----- Attempting Submission 1 (Fri Apr 05 23:53:38 GMT 2019) -----
HST Phase I Proposal 1003 (apt_qpgovi_v01.apt) successfully submitted.
Receipt: # 1003-1
----- Attempting Submission 2 (Fri Apr 05 23:54:56 GMT 2019) -----
HST Phase I Proposal 1003 (apt_qpgovi_v01.apt) successfully submitted.
Receipt: # 1003-2
----- Attempting Submission 3 (Sat Apr 06 00:01:00 GMT 2019) -----
HST Phase I Proposal 1003 (apt_qpgovi_v01.apt) successfully submitted.
Receipt: # 1003-3
----- Attempting Submission 4 (Sat Apr 06 00:11:26 GMT 2019) -----
HST Phase I Proposal 1003 (apt_qpgovi_v01.apt) successfully submitted.
Receipt: # 1003-4
----- Attempting Submission 5 (Sat Apr 06 00:26:45 GMT 2019) -----
HST Phase I Proposal 1003 (apt_qpgovi_v01.apt) successfully submitted.
Receipt: # 1003-5
----- Attempting Submission 6 (Sat Apr 06 00:32:54 GMT 2019) -----0----- Attempting Submission 1 (Fri Jul 19 16:01:47 GMT 2019) -----
----- Attempting Submission 2 (Thu Nov 21 21:40:43 GMT 2019) -----
----- Attempting Submission 3 (Tue Nov 26 20:17:56 GMT 2019) -----
----- Attempting Submission 4 (Thu Jul 23 18:37:02 GMT 2020) -----I have already rerun the visit planner, and there are green check marks next to both visits 54 and 59.
But somehow the APT kept saying the visit planner has to be run, even after I have done so.
Compared to the failed visits 04 and 09, I increase the ACQ/IMAGING exposure time 51.9 sec (and update the ETC calculation).
I also added the "AFTER BY" constraint for Visit 59, which is 25 to 40 days after Visit 54.The Angular Momentum of the Warm-Hot Circumgalactic MediumHow much of the circumgalactic medium around nearby galaxies is rotating? Quasar sightline observations reveal that the Doppler shift of low-ionization-state gas shares the sign expected from gas rotation in the disk plane. The projected velocities are lower than predicted for gas on circular orbits in a thin disk, suggesting that this cool gas will spiral towards the galactic disk. This result raises important questions about the kinematics of the warm-hot circumgalactic medium which must be rapidly cooling given its temperature near the peak of the radiative cooling curve. If this warm-hot phase is also corotating with the galactic disks, then it would seem likely that both phases of corotating gas are dynamically related. A number of HST/COS programs have established the prevalence of substantial column densities of O+5 ions in the halos of star-forming galaxies. These OVI absorbers are widely believed to trace the warm-hot phase, although alternative scenarios where the gas is photoionized instead of collisionally ionized imply different conditions. Several known examples of corotating OVI absorbers exist; yet a recent analysis of a small sample of galaxy -- quasar pairs did not detect net corotation. We propose new Cosmic Origins Spectrograph observations of eight quasars paired with galaxies for which we have measured rotation curves. We will combine these results with ground-based rotation curves for 15 galaxies having OVI detections in their existing COS spectra. If most of the OVI systems turn out to be corotating, then 23 pairs will be sufficient to obtain a statistically significant result.Using the BOT/GALEX tool, we find that all the fields are safe. The BOT/GSCII tool flags four of the target quasars (#1, #3, #7, and #8), but the GALEX photometry indicates these targets are safe. Seven of the quasars will acquired using NUV ACQ/IMAGE mode with MIRRORA; the NUV brightest target requires MIRRORB. No ACQ/SEARCH should be necessary because the targets are point sources at ultraviolet wavelengths, and coordinates are known to an accuracy better than 0.4 arcseconds. We used the TA ETC to calculate the exposure time required to reach SNR of 20; the GALEX NUV magnitudes were used to normalize a power law SED of slope F_lambda ~ lambda^(-0.59). A non-interruptible sequence links the spectroscopic exposures to the target acquisition. The G130M spectra need to cover the intervening O VI 1032, 38 A absorption lines from foreground galaxies. The galaxy redshifts (0.13629 to 0.28940) place the observed doublet at 1175 to 1335 A. The 1291 central wavelength provides the highest throughput at these wavelengths, and following COS2025 Policy, we observe at FP-POS3 and FP-POS4. We observe one target, J0919+2914, with CWL 1222 because the OVI absorption from the CGM of the target galaxy (z=0.23288) would fall in the detector gap with CWL 1291, and we use all the FP-POS positions for this observation. With one exception, we structured the visits to contain 2 to 3 orbits to facilitate scheduling. We request 4 consecutive orbits for J0852+1711 because it is more challenging to obtain the desired SNR for this target.Our team has published the following papers related to the scientific goals of this proposal:
Ho, S. H., Martin, C. L. et al. 2017, ApJ, 835, 267
Martin, C. L., Ho, S. H. et al 2019, ApJ, submitted (arXiv:1901.09123)
Ho, S. H., Martin, C. L. & Turner, M. L. 2019, ApJ, accepted (arXiv:1903.06840)
Ho, S. H. & Martin, C. L. 2019, ApJ, submitted (arXiv:1901.11182)
For Crystal Martin:
* GO-13407: This COS program required pre-imaging with ACS/SBC sand WFC3/UVIS. The images turned out to be important to the scientific analysis. They were reduced, analyzed, and published in Martin et al. 2015 ApJ, 803, 6.
* GO-12533: This COS program required pre-imaging with ACS/SBC sand WFC3/UVIS. The images turned out to be important to the scientific analysis. They were reduced, analyzed, and published in Martin et al. 2015 ApJ, 803, 6.
* GO-12928: As a Co-I of this COS program (PI: Alaina Henry).
For Stephanie Ho:
* GO-14754: As a Co-I of this WFC3 program, she redrizzled the images, processed the images to identify spiral structures of galaxies, and used the inferred 3D disk orientation to develop analytical models for explaining the kinematics of absorption-line systems (PI: Crystal Martin).Galaxies and the IGM6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYQSOQUASARNOJ2000J2000GALEX FUV = 19.61 GALEX_NUV = 18.70GALAXYQSOQUASARNOJ2000J2000GALEX FUV = 18.60 GALEX_NUV =17.87GALAXYQSOQUASARNOJ2000J2000GALEX FUV = 18.89 GALEX_NUV =17.84GALAXYQSOQUASARNOJ2000J2000GALEX FUV = 19.61 GALEX_NUV =18.20GALAXYQSOQUASARNOJ2000J2000GALEX FUV = 19.25 GALEX_NUV =18.54GALAXYQSOQUASARNOJ2000J2000GALEX FUV = 19.01 GALEX_NUV =17.43GALAXYQSOQUASARNOJ2000J2000GALEX FUV = 18.89 GALEX_NUV =17.89GALAXYQSOQUASARNOJ2000J2000GALEX FUV = 19.18 GALEX_NUV =18.18COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.1590889920000103.5(Tic-Visit
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)
(Tic-Orbit
:proposal-id 15866
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)
(Tic-Orbit
:proposal-id 15866
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)true20The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.1590954262000172.89964788426278(Tic-Visit
:proposal-id 15866
:visit-id "10"
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:trans-version "20190514"
:date "21-Nov-2019 15:23:44.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
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)
(Tic-Obset
:proposal-id 15866
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)
(Tic-Orbit
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)
(Tic-Orbit
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:dark-offset NIL
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:low-sky "N"
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)true20