Probing Multiphase Cooling Via OVI Emission in the Cores of the Most Extreme Cooling Flows

For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. 0 Assigned ID: 5471 ----- Attempting Submission 1 (Tue Mar 26 16:26:42 GMT 2024) ----- HST Phase I Proposal 5471 successfully submitted. Receipt: # 5471-1 ----- Attempting Submission 2 (Tue Mar 26 23:31:08 GMT 2024) ----- Based on Fig 9.1 in Section 9.5 of the COS Instrument Handbook, visits longer than 1 orbit in G160M do not require any additional actions. https://hst-docs.stsci.edu/cosihb/chapter-9-scheduling-observations/9-5-science-exposure-overheads COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Reduced visits to be <=5 orbits in duration. Adjusted FP-POS cycling 1839002040 ----- Attempting Submission 1 (Tue Aug 06 20:08:23 GMT 2024) ----- ----- Attempting Submission 2 (Fri Aug 09 20:30:00 GMT 2024) ----- ----- Attempting Submission 3 (Sat Oct 19 13:14:32 GMT 2024) ----- ----- Attempting Submission 4 (Mon Nov 04 14:54:11 GMT 2024) ----- I have reviewed the warnings and resolved most. The majority of the remaining warnings have to do with our targets being extended (nothing to be done about that!) and inefficient ordering of FP-POS. I'm not sure how to make these orderings more efficient for visits with more than 4 pointings, since you need to go 4->1 at some point. Or should we go 1->2->3->4->3->2->1? Let me know if we missed anything! Probing Multiphase Cooling Via OVI Emission in the Cores of the Most Extreme Cooling Flows The cores of galaxy clusters represent one of the few places in the Universe where large-scale cooling and feedback processes can be readily observed. Unlike isolated galaxies, where some of the energy injected into the ISM from the AGN often escapes into the low-density IGM, the denser ICM in cluster cores retains an imprint of this feedback in the form of bubbles or ripples. Similarly, the accretion of hot gas from the IGM onto isolated galaxies is challenging to observe due to the very low densities, while such phenomena have been studied in depth for decades in galaxy clusters. These so-called "cooling flows" in galaxy clusters, which were once thought to be massive flows of cool gas on the order of hundreds of Msun/yr, are now understood to be considerably less massive, with AGN feedback preventing the majority of the gas from cooling. Despite significant progress, the details of the cooling/feedback cycle still elude us. One of the most promising paths forward is the use of the OVI emission line, probing 10^5.5K gas, to detect the multi-phase cooling flow. This line should be especially sensitive to the instantaneous cooling rate of the hot gas, compared to lines in the X-ray. Here we propose to target the three most strongly cooling clusters in the known universe that do not also harbor central QSOs, with a goal of measuring the instantaneous cooling rate in these clusters. This program would double the number of OVI detections in non-QSO clusters, providing critical constraints for subgrid models of AGN feedback in simulations, providing a measurement of the level of turbulence in the cooling gas, and constraining the age of the cooling-fed starburst. The primary goal of this program is to obtain spectra of the OVI (1032,1038) doublet in three giant elliptical galaxies, which will be redshifted to 1291-1532A, depending on the source. Our secondary goal is to obtain broad UV continuum coverage. We are targeting relatively diffuse/clumpy regions. Thus, pointing revision via ACQ/SEARCH is not possible. We instead must center on a nearby star (<60" away) in all cases and perform offsets. According to the COS users manual, such offsets should be accurate enough for our purposes. We have identified stars that are bright in the bluest HST band that is available, and are using their GAIA positions as a starting point. All of our 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. We separate our visits into 4+ orbits, cycling through FP-POS with each new visit. This observing strategy is adopted to reduce the fixed pattern noise and fill up the wavelength hole produced by the chip gap without excessive overheads. Since our targets are faint (<0.001 cts/s), we use a BUFFER-TIME equal to the exposure time minus 110s, as suggested by Julia Duval for a similar 2012 program. We choose our central wavelengths in order to keep the OVI line (1032,1038A rest frame) as far from the chip gap as possible. We are open to suggestions on this, if we are pushing the line into a low-sensitivity regime. The team for this proposal consists of several experts in cooling and feedback in galaxy clusters, as well as some students who will benefit greatly from these new data. Below we highlight a few key individuals who will carry out the bulk of the analysis and publication. Prof. Michael McDonald is an expert in studying the evolution of galaxies and clusters of galaxies. He has extensive experience with a wide variety of data, including all of the data assembled for this study. In particular, he has acquired and published data from a wide array of space telescopes, including Chandra, XMM-Newton, Hubble, Spitzer, Herschel, and GALEX. He has a publication record of 136 papers over the past 10 years. His research group at MIT is focused on understanding the balance between cooling and feedback in the centers of galaxy clusters. He has been awarded time with HST-COS to study two galaxy clusters (Abell 1795 and Phoenix), and published both of these data sets shortly after obtaining the data. Graduate student Michael Reefe is studying coronal emission in galaxy cluster cores for his PhD thesis. This work is currently centered on JWST observations of the Phoenix cluster, but will expand to include a re-analysis of all archival FUSE and HST-COS data as well as these additional observations if awarded. Graduate student Michael Calzadilla has worked for the past several years on understanding the extreme limits of AGN feedback in clusters, ultimately leading to this proposal. He will continue to contribute to this program as a postdoc. Prof. Andy Fabian is a world leader in the study of cooling flows in galaxy clusters, and has written multiple reviews on the topic. He pioneered much of the early work on the discovery of cooling flows, the X-ray spectroscopic follow-up of cooling flows, and most recently the study of highly obscurred "hidden cooling flows". He will provide valuable expertise in interpreting the results of this study. Prof. Brian McNamara is a world leader in the study of AGN feedback in galaxy clusters, and has written multiple reviews on the mechanism by which AGN prevent runaway cooling of the hot intracluster gas in galaxy clusters. He will prove invaluable during the interpretation stage of these data. Dr. Massimo Gaspari is a world leader in the simulation of the cooling/feedback cycle in galaxy clusters, and has pioneered the concept of Chaotic Cold Accretion as a feeding mode for the central black holes in galaxy groups and clusters. He will bring his expertise in understanding the multiphase condensation of hot gas to this work. Dr. Taweewat Somboonpanyakul led the discovery of CHIPS1911, and has obtained a large Chandra program to understand the hot X-ray gas in this runaway cooling system. These ancillary data will be critical in interpreting the HST-COS observations, if awarded, on CHIPS1911. Prof. Marios Chatzikos is a developer of the CLOUDY code and has published several papers utilizing this software to model properties of multiphase gas. He will provide the necessary modeling to interpret the OVI luminosities in the context of a cooling model. Galaxies Intergalactic Medium and the Circumgalactic Medium 6 false false false false false false false false SUPPORTED STAR UNDESIGNATED NO J2000 CLUSTER OF GALAXIES COOLING FLOW STAR FORMING REGION YES J2000 STAR UNDESIGNATED NO J2000 CLUSTER OF GALAXIES COOLING FLOW STAR FORMING REGION YES J2000 STAR UNDESIGNATED NO J2000 CLUSTER OF GALAXIES COOLING FLOW STAR FORMING REGION YES J2000 COS/FUV Spectroscopic No No G130M 1327 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G160M 1600 COS/NUV Imaging No No MIRRORA COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 1729343049954 The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. 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