0Assigned ID: 5776
----- Attempting Submission 1 (Tue Mar 26 22:48:44 GMT 2024) -----
HST Phase I Proposal 5776 successfully submitted.
Receipt: # 5776-1
----- Attempting Submission 2 (Tue Mar 26 23:52:45 GMT 2024) -----
HST Phase I Proposal 5776 successfully submitted.
Receipt: # 5776-2
----- Attempting Submission 3 (Wed Mar 27 16:31:44 GMT 2024) -----
HST Phase I Proposal 5776 successfully submitted.
Receipt: # 5776-3
----- Attempting Submission 4 (Wed Mar 27 20:12:35 GMT 2024) -----COS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
COS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
COS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
COS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS0----- Attempting Submission 1 (Wed Aug 14 23:12:35 GMT 2024) -----
HST Phase II Proposal 17774 successfully submitted.
Receipt: # 17774-1
----- Attempting Submission 2 (Fri Aug 16 19:04:19 GMT 2024) -----Multiphase gas in eROSITA-detected galaxy groups and clustersGalaxy groups and clusters can be brutal environments for galaxies' star formation, as the hot (>10^6 K) gas permeating these massive halos can readily remove galaxies' cool (<10^4 K) gas reservoirs and prevent fresh cool gas from fueling. However, studying these inherently multiphase environments from a multiphase perspective, i.e., systematically characterizing the diffuse cool and hot gas in groups and clusters, has remained elusive due to the relatively small numbers of X-ray detected halos to target in UV absorption line experiments. The eROSITA All Sky Survey (eRASS) is dramatically changing the landscape with an order-of-magnitude increase in the number of X-ray detected groups and clusters after only the first year of observations. We propose to obtain HST/COS spectra of quasars probing a sample of eRASS-detected galaxy groups and clusters spanning two orders of magnitude in X-ray luminosity, representing the first study of its kind and tripling the previously existing samples. First, we will track the cool gas, traced by H I Ly-alpha and Si III, contents in and around these halos as a function of the X-ray derived properties. Using ongoing follow-up spectroscopic surveys for these groups/clusters, we will characterize the CGM contents of galaxies near the sightlines to investigate the impact of increasing hot gas density and temperature (via the X-ray measurements) on these galaxies. Hydrodynamical simulations have been highly inconsistent in reproducing the few existing observations, and the dataset from our program will stand as a critical benchmark for state-of-the-art models that attempt to capture the salient multiphase gas physics in massive halos.To achieve our science goals, we will employ the G130M grating providing ~20 km s^-1 spectral resolution. We will primarily target H I Lya at the cluster's redshifts. The G130M central wavelength configurations chosen for each target ensures coverage of not only Lya, but also some transitions of silicon. Mission critical for our science is coverage of Lya with sufficient S/N; we have chosen grating configurations to maximize throughput at the H I Lya line. We will also cover Si III 1206 Ang, and additional metal lines (Si II 1190, 1193 Ang, and Si II 1260 Ang for a majority of our targets) will supplement our key scientific objectives but are not the focus of this proposal. Our orbit requests are derived from an S/N = 10 requirement at Lya, which corresponds to a limiting equivalent width ~40 mAng assuming a line width of 6 pixels, with exposure time estimates determined by the COS ETC. We do not require coverage of Lyb because we expect most of the H I Lya absorption to be optically thin. Even in the conditions where this is not the case, we can place reliable lower limits on N (H I). We will employ a routine observing sequence for COS. We will acquire the targets in the near-UV with an ACQ/IMAGE exposure then switch to TIME-TAG for our science exposures. To comply with guidelines as outlined in the COS Handbook and minimize flat-field artifacts, we will use multiple FP-POS settings during each visit.Prof. Joe Burchett is an expert at quasar absorption line studies and the connection with galaxies and has published >10 papers on the topic of this proposal. Prof. Burchett will manage the project and engage in high level science guidance and paper writing. He will be engage in mentoring several of the graduate students.
Dr. Ben Oppenheimer is an expert in global statistics from hydrodynamic cosmological simulations. Dr. Oppenheimer will engage in theoretical interpetation and comparisons with simulations. He will engage in high level science discussions, and paper writing.
Prof. Daisuke Nagai is an expert on theoretical and computational modeling of galaxy cluster formation, and he has experience in the computational simulations that will be required to interpret these data.
Dr. Scott Anderson is Program Head of SDSS-V Black Hole Mapper, part of which is the SPIDERS follow-up program targeting eROSITA-detected galaxy clusters. As SDSS-V will provide a major source of the ancillary observations for this program, and Dr. Anderson has authoritative working knowledge of SDSS data systems and is an expert in AGN.
Dr. John Stocke is long-time user of HST and was a member of the COS GTO team. He is recognized expert on QSO absorption lines, the circumgalactic medium, and the diffuse gas in galaxy groups.
Dr. Nicolas Tejos is an expert in the analysis of low-z QSO absorption line systems and low-z galaxy surveys focused on large-scale structure, combining HST UV spectroscopy with ground-based optical follow-up observations.
Prof. Todd Tripp has more than 25 years of experience with HST spectroscopic data and has led or coauthored 99 refereed papers using ultraviolet spectrographs in space. He has extensive experience with HST spectroscopic data, including both data reduction/processing and analysis.
Dr. Daniel Wang is an expert in multiwavelength studies of galaxies and clusters of galaxies, including X-ray, optical, and radio observations, and has led several past HST observing campaigns with multiple papers published in the past decade on data analysis carried out with HST observations.
Several members of the eROSITA collaboration, all X-ray experts, are on this proposal team and will facilitate data access and analysis. Dr. Andrea Merloni is project senior scientist of the eROSITA project. Dr. Esra Bulbul is the head of the cluster science working group. Dr. Johan Comparat is head of the SDSS-V BHM galaxy clusters working group. Dr. Jeremy Sanders is a veteran expert in X-ray studies of intracluster media. Dr. Mara Salvato is eROSITA Spokesperson and is head of the eROSITA multi-wavelength follow-up working group. Dr. Teng Liu is head of the eROSITA AGN working group
Dr. Christopher N.A. Willmer has extensive experience with using HST data combined with ground-based spectroscopy and has been very active in acquiring wide-field followup galaxy spectroscopy in fields surrounding QSO sightlines.
Priscilla Holguin Luna, Erick Aguirre, and Tim McQuaid are graduate students working with PI Burchett. They are all skilled in analyzing COS spectra.
Maxim Markevitch is a pioneer in galaxy cluster science and has led key aspects of the Chandra X-ray mission, XRISM, and others. He will be a valuable resource for X-ray data analysis and obtaining follow-up X-ray ancillary observations.Intergalactic Medium and the Circumgalactic MediumLarge Scale Structure of the Universe6falsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYQSONOJ2000J2000FUV=17.90416145GALAXYQSOQUASARNOJ2000J2000FUV=18.27466202GALAXYQSOQUASARNOJ2000J2000FUV=18.17481613GALAXYQSOQUASARNOJ2000J2000FUV=17.83533859GALAXYQSOQUASARNOJ2000J2000FUV=18.03486061GALAXYQSOQUASARNOJ2000J2000FUV=16.50211716GALAXYQSOQUASARNOJ2000J2000FUV=17.85335732GALAXYQSOQUASARNOJ2000J2000FUV=18.46393776GALAXYQSOQUASARNOJ2000J2000FUV=18.49046516GALAXYQSOQUASARNOJ2000J2000FUV=18.16498375GALAXYQSOQUASARNOJ2000J2000FUV=18.41496849GALAXYQSOQUASARNOJ2000J2000FUV=17.34727478GALAXYQSOQUASARNOJ2000J2000FUV=17.66121674GALAXYQSOQUASARNOJ2000J2000FUV=17.59754944GALAXYQSOQUASARNOJ2000J2000FUV=17.77166748COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1222The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.1767166916000298.9451845679942(Tic-Visit
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