Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.0Assigned ID: 2747
----- Attempting Submission 1 (Wed Mar 16 11:48:58 GMT 2022) -----Warnings are for G160M lifetime positions. Following the COS handbook, as the observations are of faint targets and long exposures, these warning are not relevant.The number of orbits used exceeds the number allocated29 Sept 2023 9:39 PST - Berg - Edited repeat visit for J1427 (HOPR (Z1))
18 Apr 2023 13:10 PDT - Berg - Added repeat visit for J1342 and updated HOPR Z2 (J0959 HOPR (Z2))
18 Apr 2023 12:27 EDT - Armstrong- created HOPR Z2 for failed 12
18 Apr 2023 12:30 EDT - Armstrong- last checkin showed NO Change analysis
V2 of phase 2 for Program 17076. Visits 12 and 14 updated to have FP-POS 1 and 4. Visits 5-7 updated to have CENWAVE 1900 for exposures with "1806" in title.
V1 comments: The observations have been broken up into typically <3 orbit visits, with a single FP-POS per orbit in the visit. Feedback on which FP-POS should be prioritized for observations that only use two or three FP-POS would be appreciated. To meet our S/N requirements, some visits ideally require 4 or 5 orbits. We acknowledge this is difficult to schedule, and have only selected targets with large observability windows to have 4 or 5 orbit visits.-1451269363----- Attempting Submission 1 (Mon Jul 11 20:22:15 GMT 2022) -----
HST Phase II Proposal 17076 successfully submitted.
Receipt: # 17076-1
----- Attempting Submission 2 (Fri Nov 04 21:15:12 GMT 2022) -----
----- Attempting Submission 3 (Tue Apr 18 20:16:36 GMT 2023) -----
----- Attempting Submission 4 (Fri Sep 29 16:40:14 GMT 2023) -----We follow the guidelines of COS2025, and the warnings for the 4 FP-POS are not applicable for our requested S/N.
Given that we have archival data to help with the wavelength solution, we acknowledge the potential reduction in walvelength calibration at LP6.The C IV in L* galaxies (CIViL*) survey -- Pinpointing the physical conditions and evolutionary stages of gaseous halosThe circumgalactic medium (CGM) plays a crucial role in galaxy evolution, hosting the gaseous reservoirs that feeds accreting material to replenish fuel for future star formation whilst retaining a record of material ejected by winds and feedback processes. Quantifying the connection between these gaseous reservoirs and their host galaxies provides essential constraints on the specific events that transform galaxies. The Cosmic Origins Spectrograph (COS) has played a significant role in studying the CGM over the past decade by providing an unbiased census of the gas around galaxies over a mass range that spans dwarfs to L* galaxies, as well as special evolutionary phases (such as active galactic nuclei [AGN] or starbursts). However, despite CIV being arguably the best tracer of galactic gas reservoirs across cosmic time, these galaxy-selected COS surveys lack spectral coverage of CIV surrounding a necessary benchmark sample of L* galaxies. Our proposed survey aims to quantify the amount of CIV in the CGM of 13 L* galaxies, and for the first time: (i) constrain feedback processes from AGN and starbursts within 200 kpc, (ii) quantify the radial CIV profile to guide modeled stellar wind and black hole feedback perscriptions across three decades of stellar mass, and (iii) derive the physical conditions within the CGM by studying its ionization structure. Our carefully crafted representative L* galaxy sample will add to the legacy of COS-CGM studies by including a key ion for diagnosing the physical properties of the CGM.Description of Observations:
----------------------------------
Our sample of 11 FUV-bright QSOs (GALEX FUV < 19) has been selected from the COS-Halos and COS-GASS surveys to obtain a census of CIV in the circumgalactic medium of a control-matched sample of L* galaxies. Our science goals require quantifying the column density of CIV down to a limit of logN(CIV) = 13.5, which corresponds to an asborption profile with a minimum rest-frame equivalent width of 50 mA. We therefore require a minimum signal-noise ratio of 10 per spectral element in our spectrum at the position of CIV in the CGM of the host galaxy. We require the highest spectral resolution in order to fit the profile of the CIV line, and thus require observations with the G160M (redshift z~0.2 galaxy sub-sample) and G185M (z~0.03 sub-sample) gratings, covering the corresponding CIV 1548 and 1550 angstrom doublet.
Phase II Observing Strategy:
-----------------------
We are taking COS/FUV and COS/NUV spectra of QSOs with GALEX FUV magnitudes that range from 17.0 - 18.4. We are using the G160M and G185M gratings centered at various, single CENWAVE settings to obtain the CIV doublet at ~1549 angstroms. We require only one CENWAVE setting per intervening galaxy for this experiment since we are targeting specific absorption lines that will not fall near the gap between segments nor will they fall in the regions of siginficant gain sag with this set up in LP6. For the two QSOs with two intervening galaxies each, two CENWAVES are required as there is no single CENWAVE to observe both CIV doublets simultaneously (i.e. one always falls in a wavelength gap). Because we have coordinates that are accurate to within 0.1", we skip the ACQ/SEARCH step, and acquire the targets with a NUV ACQ/IMAGE using MIRRORB to guard against QSO brightening. All of these objects are faint enough that this method of acquisition is safe. The Exposure times for these acquisitions are set by requiring a S/N of 20 and assuming a FOS QSO template in the imaging target acquisition ETC (e.g. COS.ta.1811459).
Using the COS spectroscopic ETC, we model the QSOs as COS-based QSOs and normalizing the spectra to the QSO's GALEX FUV AB magnitude (e.g. COS.sp.1809369). None of these QSOs will pose a bright limit threat to COS and we have no timing or orientation constraints. Our targets each require between 2 and 10 orbits, and are generally split into 1-3 visits each of 3 orbits or fewer. For some targets, we do not reach our total exposure time required without using either a 4-orbit or 5-orbit visit per target. We have added an additional justification to the relevant visits, explaining that our total exposure time required can only be achieved by using a 4-orbit or 5-orbit visit, understanding that visits longer than 3 orbits can be challenging to schedule. As such, we only use 4 or 5 orbit visits on targets that show signficantly long or frequent visibilities in the visit planner tool to ensure ease of scheduling. Buffer times have been set to the suggested value of 2/3 of the full buffer time provided by the ETC.
We note that, in order to minimize overheads (especially for targets observed with G160M), we only observe one FP-POS per orbit. While we try to observe with all four FP-POS whenever possible, targets only observed with 2-3 orbits will not get the full four FP-POS. As such, we have a minimum of 2-3 FP-POS per target, which meets the minimum FP-POS requirements outlined by the COS2025 documentation. While this may cause issues in the wavelength calibration and increase the fixed-pattern noise, these targets all have archival COS data so we can further pin-down the wavelength solution using the archival data. Additionally, for the two QSOs that have two intervening absorbers, we mix both CENWAVE set-ups within a single visit. This is required in order for the minimum S/N threshold to be met for both set-ups by only including the acquisition overhead of the first orbit for the CENWAVE setup that requires a lower exposure time to reach the minimum S/N. A comment has been added in the relevant visits where this applies.
In our final set-up we achieve S/N of ~10 per resolution element at the position of the CIV doublet for the target galaxy, which is in line with the requirements we outlined in the science case of Phase 1.Dr. Trystyn Berg's research uses quasar absorption lines to understand various facets of galaxy evolution, and has published eight first author papers on this work to date. Dr. Berg has previously reduced HST/COS data and led the investigation of the gaseous halos surrounding active galactic nuclei as part of the COS-AGN program. He is the PI of the proposed CIViL* survey, where he will lead the data reduction and analysis of the comparison of the gaseous halos of L* galaxies to active galactic nuclei, starbursts, and dwarf galaxies.
Dr. Jessica Werk is the PI on 2 previous successful HST-GO proposals, is a first author on 5 papers that focus on results from COS data, and a co-author on over 25 publications that present results based on HST/COS data. She is primarily an observer who seeks to understand the intricate relationship between galaxies and their extended gaseous envelopes. In particular, her experience using CLOUDY, a full radiative-transfer code, to determine the physical properties of the absorption features will be highly useful for our planned analysis.
Dr. Benjamin Oppenheimer is an expert in computational hydrodynamic simulations of galaxies and their gaseous environments. He specializes in understanding how the physical and evolutionary parameters of the IGM/CGM can be quantified through observational campaigns. He has published over ten papers as first author on the IGM/CGM, and has been a co-author on over 60 papers relating to his area of expertise. Dr. Oppenheimer will be providing the simulated predictions for the CIViL* survey.
Prof. Sara Ellison has been working in the field of QSO absorption lines for over 25 years. Notably, she was the PI of the HST COS-AGN program, one of the pre-cursors to the proposed CIViL* survey. Prof. Ellison has appeared on almost 200 peer-reviewed papers, many of them relevant to this HST proposal. In the proposed project, Prof. Ellison will contribute to the survey design, provide input on the analysis and interpretation of results.
Dr. Rongmon Bordoloi is an expert in studying CGM and galaxy-halo gas connections, and imaging+spectroscopic observations from both ground and space (specially with HST/COS). In the proposed program, Dr. Bordoloi will contribute to the program design, data analysis and data reduction from HST/COS and science results. He will also contribute to comparison of the proposed sample with archival data.Intergalactic Medium and the Circumgalactic Medium6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYQSOQUASARNOJ2000J2000FUV=17.87GALAXYQSOQUASARNOJ2000J2000FUV=18.33GALAXYQSOQUASARNOJ2000J2000FUV=18.37GALAXYQSOQUASARNOJ2000J2000FUV=17.86GALAXYQSOQUASARNOJ2000J2000FUV=17.99GALAXYQSOQUASARNOJ2000J2000FUV=17.42GALAXYQSOQUASARNOJ2000J2000FUV=17.83GALAXYQSOQUASARNOJ2000J2000FUV=17.53GALAXYQSOQUASARNOJ2000J2000FUV=17.74GALAXYQSOQUASARNOJ2000J2000FUV=17.97GALAXYQSOQUASARNOJ2000J2000FUV=17.97COS/NUVSpectroscopicNoNoG185M1900COS/NUVSpectroscopicNoNoG185M1882COS/NUVSpectroscopicNoNoG185M1953COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M1941COS/NUVSpectroscopicNoNoG185M1913COS/NUVSpectroscopicNoNoG185M1986COS/NUVSpectroscopicNoNoG185M1953COS/NUVSpectroscopicNoNoG185M1921COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG160M1623The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.1695736714000283.059512477219(Tic-Visit
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This is a partial 1-orbit repeat of failed visit 131709767472000241.0(Tic-Visit
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)
(Tic-Orbit
:proposal-id 17076
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)true20The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.Require 5-orbit visit to meet minimum S/N of 10 at position of CIV doublet at redshift of intervening galaxy169594544700067.52696199868589(Tic-Visit
:proposal-id 17076
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:proposal-version -1
:trans-version "20220630"
:date "18-Apr-2023 13:05:33.0"
:trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
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)
(Tic-Obset
:proposal-id 17076
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)
(Tic-Orbit
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)
(Tic-Orbit
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)
(Tic-Orbit
:proposal-id 17076
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)
(Tic-Orbit
:proposal-id 17076
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)
(Tic-Orbit
:proposal-id 17076
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:dark-offset NIL
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)true50