0 Assigned ID: 5910 ----- Attempting Submission 1 (Mon Apr 15 13:51:58 GMT 2024) ----- 0 ----- Attempting Submission 1 (Wed Nov 06 17:43:05 GMT 2024) ----- SPT-CLJ2223-5015: RUNAWAY COOLING IN THE ABSENCE OF FEEDBACK? We propose short Chandra (45ks) and Hubble (2 orbits) observations of a unique galaxy cluster, SPT-CLJ2223-5015. This cluster, at z=0.24, hosts a massive starburst at its center, with a star formation rate (50-130 Msun/yr) on par with the central galaxy in Abell 1835. Even more interesting, this central starburst galaxy appears to be radio quiet, with a radio luminosity 200x fainter than necessary to prevent runaway cooling of the ICM. Combining the proposed Chandra+Hubble data with approved ground-based spectroscopy, we will confirm that (i) the starburst galaxy lies in the center of the cluster, (ii) that the cluster is a strong cool core, and (iii) that the starburst is being fueled by runaway cooling of the ICM, in the absence of any radio-mode feedback. The goal of this program is to obtain single-band imaging with WFC3-UVIS and WFC3-IR, using the F475W and F110W filters, respectively. This is a joint Chandra+HST proposal. I am duplicating here the team expertise for the Chandra proposal. M. McDonald is a professor at MIT with extensive experience with both Chandra and Hubble data. He led the analysis of the SPT-Chandra survey, which included Chandra observations of the 100 most massive SPT-selected clusters from z=0.3 to z=1.8, resulting in 8 lead-author papers (McDonald et al. 2012c, 2013b, 2014c, 2015b, 2016b, 2017, 2019a, 2019b) and a larger number of co-authored papers. He also led the SPT-Progenitors survey (~100 clusters at 0.3 < z < 1.2 that are the progenitors of Perseus/Coma), and the CEREAL survey (~100 clusters at z~0.2 that are the descendants of the SPT-Progenitors clusters) and its low-mass extension (~100 clusters at z~0.15 down to group scales). These programs have been awarded a total of ~9Ms of Chandra observations over the past 13 cycles. He lead the discovery and characterization of the Phoenix cluster, which is the only cluster that shows direct evidence of pure cooling in its core, resulting in a massive central starburst. He has a strong track record of publishing Chandra data within 1-2 years of acquisition for all successful programs, and was awarded an NSF CAREER award to push the detailed study of cluster evolution to high redshift. M. Calzadilla is a graduate students at MIT, soon to be Hubble Fellow at SAO, who specializes in multiwavelength studies of galaxy clusters. He is adept at developing pipelines to determine ICM properties for large samples of clusters, and successful at rapidly publishing the results from these studies. He has recently published a series of four papers based on Chandra and Hubble data for his thesis, including a pair of clusters studying sloshing in Abell 1644 and strong AGN feedback in SPT-CLJ0528-5300, as well as larger statistical samples studying the balance between cooling and feedback in massive, distant clusters. T. Somboonpanyakul is a faculty member at Chulalongkorn University in Thailand who specializes in studying large cluster samples, with a focus on studying AGN feedback in galaxy cluster cores. In particular, his PhD thesis demonstrated that X-ray surveys miss a small population of clusters hosting active central galaxies, which can be mis-classified as isolated point sources at moderate redshift. S. Allen and A. Mantz have helped pioneer the development and application of robust analysis approaches to cosmological studies using X-ray observations of galaxy clusters (e.g. 2004, MNRAS 353, 457; 2008, MNRAS 383, 879; 2010, MNRAS 406, 1759; 2010, MNRAS 406, 1773; 2011, AR&A 49, 409; 2014, MNRAS 440, 2077; 2015, MNRAS 446, 2205). They have published broadly on many aspects of galaxy cluster astrophysics (e.g. 2011, Science 331, 1576; 2013 Nature 502, 656; 2014 Nature 515, 85; 2016, Nature 535, 117; 2020 Nature 577, 39). Allen was co-recipient of the 2008 Bruno Rossi Prize for his work in these areas. A. Flores is a graduate student working with Allen and Mantz, who has made significant contributions to the study of the most distant SPT-selected clusters (2021, MNRAS 507, 5195). M. Gaspari is a world leader in the simulation of the cooling/feedback balance in cluster cores. His expertise will be invaluable in interpreting the results of this program, and connecting to theory on SMBH accretion, feedback, and plasma instabilities. J. Hlavacek-Larrondo is a tenured professor of physics at the University of Montreal, specialized in the astrophysics of black holes. She holds a Canada Research Chair, obtained her PhD from the University of Cambridge and was a NASA Einstein fellow at Stanford University. She has published extensively in the fields of AGN feedback and the physics of galaxy clusters, with a particular focus on understanding the impact of black hole jets on their surroundings. She was the first to study the evolution of X-ray cavities in high-redshift clusters observed with Chandra (2012, MNRAS, 421, 1360; 2015, ApJ, 805, 35; 2020, ApJ Letters, 898, 50). Her team has also obtained some of the highest dynamic range images at radio wavelengths of nearby clusters (e.g. 2018, MNRAS, 475, 4704), including the Perseus cluster (2017, MNRAS, 469, 3872; 2017, MNRAS, 468, 2506; 2020, MNRAS, 499, 5791). L. Bleem leads the clusters working group within the South Pole Telescope collaboration, and is responsible for the creation of multiple generations of SPT cluster catalogs. She has led the publication of the SPT-SZ, SPT-ECS, and SPT-Pol surveys (2015, ApJS, 216, 27; 2021, ApJS, 247, 5; 2024, OJAp, 7, 13), and is currently leading the identification and follow-up efforts for SPT-3G. B. Floyd and C. Romero are members of the South Pole Telescope with general interest and expertise in AGN triggering and ICM turbulence, respectively. Between them, they have experience at X-ray, optical, and IR wavelengths, and will contribute their expertise to the interpretation of the results. In summary, this group is fully capable of reducing, analyzing, interpreting, and publishing these data. We have the expertise to supplement these data with data at other wavelengths, and the commitment to publishing our results in a timely manner. Galaxies 6 false false false false false false false false SUPPORTED CLUSTER OF GALAXIES COOLING FLOW EMISSION LINE NEBULA RICH CLUSTER J2000 J2000 WFC3/UVIS Imaging No No F475W WFC3/IR Imaging No No F110W POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1 false POS-TARG DITHER 0.572 WFC3-IR-DITHER-BOX-MIN 0.365 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 2 false /private/var/folders/__/jfl0zfts179f13wfxnb_tbcm0000gn/T/OPVisit5501646512265705387.xml The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. 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