0Assigned ID: 4271
----- Attempting Submission 1 (Wed May 24 07:05:05 GMT 2023) -----
HST Phase I Proposal 4271 successfully submitted.
Receipt: # 4271-1
----- Attempting Submission 2 (Wed May 24 21:57:49 GMT 2023) -----
HST Phase I Proposal 4271 successfully submitted.
Receipt: # 4271-2
----- Attempting Submission 3 (Wed May 24 23:42:26 GMT 2023) -----
HST Phase I Proposal 4271 successfully submitted.
Receipt: # 4271-3Corrected BFT for visits 9 - 14.-650969321----- Attempting Submission 1 (Thu Sep 14 15:01:09 GMT 2023) -----
HST Phase II Proposal 17478 successfully submitted.
Receipt: # 17478-1
----- Attempting Submission 2 (Wed Oct 18 01:00:05 GMT 2023) -----
HST Phase II Proposal 17478 successfully submitted.
Receipt: # 17478-2
----- Attempting Submission 3 (Thu Oct 26 17:55:27 GMT 2023) -----A comprehensive survey of diffuse gas in the Fornax ClusterWe propose an HST/COS study of the cool and warm gas contents of the Fornax cluster. Fornax is among the closest massive galaxy clusters, at a distance of only 20 Mpc, enabling a deep characterization of the galaxy populations and intracluster medium. Indeed, much ancillary data exists on Fornax with deep optical imaging, substantial spectroscopic coverage, and X-ray imaging/spectroscopy, and is currently the focus of a deep, high-resolution 21cm HI mapping campaign with the MeerKAT array. The Hubble legacy includes similar COS surveys of QSOs probing two other massive clusters, Coma and Virgo, but Fornax is even more ideal for a study of this kind. These other systems have provided the first glimpses of just how unique cluster environments are relative to the gaseous halos of galaxies, as surveyed by such programs as COS-Halos. For example, clusters do not show the characteristic anti-correlation between HI absorber strength and impact parameters as do galaxy halos. Also, the studies of Virgo and Coma as well as other higher redshift clusters indicate that the virialized medium is devoid of HI relative to the expected HI reservoir contents observed around less massive systems. This indicates that cluster galaxies lack the abundant reservoirs to fuel star formation, a key quenching mechanism. However, Fornax contains several galaxies that appear to be undergoing interactions with the environment and many galaxies that are still forming stars. Combined with the extensive ancillary data available, our survey of Fornax will provide the most comprehensive look at a massive halo in transition in the nearby Universe.To select our QSO targets, we crossmatched the 'Million Quasars Catalog' (Milliquas Flesch, 2015) with both NGC1399 (the central galaxy of Fornax) and individual galaxies in the Fornax spectroscopic census compiled by Maddox et al. (2019). Our version of the Milliquas catalog includes FUV magnitudes from crossmatching the original catalog with GALEX sources. For the crossmatch with NGC1399, we employed a search radius of 1.4 Mpc (twice the Fornax virial radius) at the distance of Fornax; for crossmatching with individual galaxies, we limited to impact parameters of 75 kpc. Clearly, these two crossmatches were redundant in the QSOs they returned, but this enabled prioritizing certain QSOs in our final sample selection due to their likely probing (or not) a cluster galaxy.
To achieve our science goals, we will employ the G130M grating to achieve ~20 km/s spectral resolution and to cover, primarily, H I Lya. The G130M 1309 cenwave setting covers not only Lya but also the Si II 1260 Ang, 1190, 1193 Ang, Si III 1206 Ang, Si IV 1393, 1402 Ang, and C II 1334 Ang transitions at the Fornax redshift (z = 0.0047). Mission critical to our science are the coverage and sufficient S/N of these lines. Therefore, we requested the use of LP3 for the G130 grating, as the COS2025 default lifetime positions do not include Segment B, which covers the observed wavelengths where these lines would fall. This will enable us to also search for associated metal lines, enabling more rigorous constraints on our Key Science Objectives. Our orbit requests are driven by exposure time estimates from the COS ETC to deliver S/N = 10 at Lya, which corresponds to a limiting equivalent width Wlim ~40 mAng assuming a line width of 6 pixels. This detection limit is commensurate with that achieved in the Yoon et al. (2012) and Yoon & Putman (2017a) surveys, enabling comparison with those samples (Science Objective 2). Given the variable sensitivity across the bandpass, our COS ETC calculations return that we should achieve S/N of 9.5, 10.5, and 8.5 at the accompanying metal lines Si III 1206 Ang, Si II 1260 Ang, and C II 1334 Ang, respectively. These sensitivities will yield approximate 3 sigma equivalent width detection limits of 44 mAng, 40 mAng, and 49 mAng, respectively. From the linear part of the curve of growth, these detection limits translate to column density detection limits of log (N(Si III)/cm^-2) = 12.3, log (N(Si II)/cm^-2) = 12.4, and log (N(C II)/cm^-2) = 13.4. Hence, we will meet or exceed the detection limits of the Yoon et al. (2012) and Yoon & Putman (2017a) surveys that serve as our primary comparison samples.
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 flatfield artifacts, we will use multiple FP-POS settings during each visit. We have verified that the spectral lines we intend to cover are attainable complying with the COS 2025 guidelines for allowed grating/cenwave/FP-POS modes.Principal Investigator Prof. Joseph N. Burchett has led 4 successful HST proposals and 7 refereed papers featuring HST/COS data, including two studies focusing on the role of large-scale environment in transforming the circumgalactic medium (CGM). Key elements of the analysis to be employed in this program were presented in Burchett et al. 2018 (MNRAS, 475, 2067), which synthesized optical/X-ray observations of galaxy clusters with COS spectroscopy of background QSOs.
Dr. Paolo Serra is the PI of the MeerKAT Fornax Survey, which will serve as a key ancillary dataset to the observations we are proposing.
Dr. Natasha Maddox is leading the MIGHTEE-HI survey with the MeerKAT array, which is a blind, deep survey of the 21cm sky over 20 sq. deg. in the southern hemisphere. Dr. Maddox compiled the Fornax spectroscopic census, which forms a core ancillary dataset to associate absorbers with galaxies.
Prof. Mary Putman was PI of the two successful HST/COS surveys targeting Virgo and Coma. Prof. Putman is also a leading expert on the CGM and 21cm observations.
Dr. Stephanie Tonnesen has led some of the pioneering computational work on ram-pressure stripping in dense environments; she will leverage her experience with high-resolution simulations to assist with interpreting these data. Dr. Tonnesen is also an expert in diffuse media in the cosmic web.
Prof. Todd Tripp has more than 25 years of experience with HST spectroscopic data and has led or coauthored >100 refereed papers using ultraviolet spectrographs in space. He has extensive experience with HST spectroscopic data, including both data reduction/processing and analysis.
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.
Prof. Q. Daniel Wang is a veteran expert on galaxy clusters and galaxy evolution more broadly, with expertise across virtually all wavelength regimes from radio to X-ray and gamma-ray. He has led some of the pioneering work on combining UV and X-ray observations of galaxy clusters.
Dr. Avinash Chaturvedi is an expert on the mass distribution of the Fornax cluster as traced by globular clusters. He is also experienced in making mock HI observations from the cosmological TNG simulations.
Priscilla Holguin Luna is a graduate student at New Mexico State University working with PI Burchett. She is trained in spectroscopic data analysis with COS and this work would comprise a portion of her thesis.Intergalactic Medium and the Circumgalactic Medium6falsefalsetruefalsefalsefalsefalsefalseAVAILABLEGALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000mFUV = 19.35GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000mFUV = 17.85GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000mFUV = 18.01GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000mFUV = 19.69GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000mFUV = 17.59GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000mFUV = 17.32GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000mFUV = 18.99GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000mFUV = 18.19COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309The scheduling data was generated by CASM 31.1.CASM was run in Phase II mode.170926930100095.41804411980269(Tic-Visit
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