0Assigned ID: 75
----- Attempting Submission 1 (Mon Aug 13 12:26:19 GMT 2018) -----
HST Phase I Proposal 75 (prop_v1.apt) successfully submitted.
Receipt: # 75-1
----- Attempting Submission 2 (Wed Aug 15 06:41:56 GMT 2018) -----
HST Phase I Proposal 75 (prop_v2.apt) successfully submitted.
Receipt: # 75-2
----- Attempting Submission 3 (Wed Aug 15 12:03:59 GMT 2018) -----
HST Phase I Proposal 75 (prop_v2.apt) successfully submitted.
Receipt: # 75-3
----- Attempting Submission 4 (Thu Aug 16 06:01:16 GMT 2018) -----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.Resubmission by the PI, following recommendations of contact scientist Will Fischer. All four FP-POS settings are used for all targets except those with cenwave=1291 A. For these targets (#1, 9, 13, 15), only FP-POS = 3 and 4 are used to get equal exposure for segments A and B.-299579438----- Attempting Submission 1 (Wed Dec 05 16:10:32 GMT 2018) -----
----- Attempting Submission 2 (Mon Jan 14 16:26:06 GMT 2019) -----
----- Attempting Submission 3 (Wed Jan 16 16:48:24 GMT 2019) -----
----- Attempting Submission 4 (Thu Jan 17 10:28:42 GMT 2019) -----As explained in the Submission Comments, we follow Will Fischer's recommendations and use all four FP-POS settings for all targets except those with cenwave = 1291 A. For these four targets (#1, 9, 13, 15), only FP-POS = 3 and 4 are used to get equal exposure for segments A and B.Galactic Winds across the Gas-Rich Merger SequenceGalactic winds in gas-rich mergers are an essential element of galaxy and SMBH evolution. The most powerful of these outflows are driven by quasars and likely feed the circumgalactic medium. The outflow energetics are often dominated by the outer (> kpc) and cooler dusty molecular and neutral atomic gas phase, but the driving mechanism is best probed by the inner (sub-kpc) highly ionized gas phase. While current X-ray observatories are not sensitive enough to carry out a systematic survey of these inner winds, recent results from two independent FUV studies have shown that COS is very well suited for this task. Prominent, highly blueshifted (1000 km/s) Ly-alpha emission has been detected in most ULIRGs, often accompanied by blueshifted absorption features. The internal kinematics of ULIRGs seem to be the single most important factor determining the profile and escape fraction of the Ly-alpha emission. However, the trends so far are entirely driven by the few AGN-ULIRGs in the current sample and are therefore highly uncertain. So here we propose to more than triple the sample size of AGN-ULIRGs (from 6 to 21 objects) and combine the results from our analysis of the new data and archival COS spectra to study, for the first time, the gaseous environments of gas-rich mergers as a function of host properties and age across the merger sequence ULIRG --> QSO. These data will allow us to distinguish between quasar-driven outflows, starburst-driven winds, and tidal debris around the mergers. They will also provide new constraints on the critically important warm-hot gas phase associated with the cooling shocked ISM predicted in some quasar feedback models.We requested and were allocated 50 orbits to observe 15 targets with COS G130M. The requested number of orbits per target ranges from 1 to 5 orbits so the observing time for each target fits within a single visit.
For each visit, we first use ACQ/IMAGE to obtain a NUV image of the field and center the aperture on the intensity peak. For this procedure, we make use of MIRRORA for all of the targets except for #3 and 13, where the ETC count rate is above 50 counts per pixel, so we use MIRRORB for these two brighter targets. There is also a BOT warning for target #8 but the ETC count rate is less than 50 counts per pixel so we keep MIRRORA. The exposure times are generous to make sure that S/N > 20.
The spectroscopic exposures are split into 1, 2, or 4 equal-duration segments per orbit with different FP-POS values to reduce the fixed pattern noise. The number of segments per orbit is chosen to minimize the overhead and maximize the on-target exposure time. We get all four FP-POS settings for all targets, except targets #1, 9, 13, and 15 with cenwave =1291 A. For these targets, we only use FP-POS = 3 and 4 to get equal exposures for segments A and B. All of the observations are done in TIME-TAG mode. This temporal sampling will allow us to exclude poor quality data and get improved thermal correction and background removal. The wavelength setting is adjusted according to the redshift of the target and is selected to optimize the number of strong lines that can be observed with G130M. At all but the highest redshifts (z < 0.2), Ly-alpha, the high-ionization lines from N V, and weaker low-ionization lines from Si and Si III fit within the wavelength coverage of the data. At the highest redshifts (z = 0.20-0.37), we lose N V and Ly-alpha but gain Ly-beta and O VI as well as several weaker low-ionization lines. Following the COS 2025 policy (Table 2.1 of COS Handbook), Segment B is turned off for lambda_c = 1291 (FP-POS = 1, 2) and 1327 (FP-POS = 1, 2, 3, 4). For simplicity and to guard against the (unlikely) possibility that our targets are more than ~50% brighter than expected, we set buffer-time = exposure-time.Massive Black Holes And Their Host Galaxies6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 20.2 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 19.1 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 17.6 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 19.1 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 21.4 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 19.4 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 19.5 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 18.6 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 21.0 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 20.3 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 18.5 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 20.9 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 17.3 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 20.2 (AB)GALAXYQUASARULTRALUMINOUS IR GALNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000m_FUV = 20.9 (AB)COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.(Tic-Visit
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