TY - JOUR
T1 - An Assessment of the in Situ Growth of the Intracluster Light in the High-redshift Galaxy Cluster SpARCS1049+56
AU - Barfety, Capucine
AU - Valin, Félix Antoine
AU - Webb, Tracy M.A.
AU - Yun, Min
AU - Shipley, Heath
AU - Boone, Kyle
AU - Hayden, Brian
AU - Hlavacek-Larrondo, Julie
AU - Muzzin, Adam
AU - Noble, Allison G.
AU - Perlmutter, Saul
AU - Rhea, Carter
AU - Wilson, Gillian
AU - Yee, H. K.C.
N1 - Funding Information:
C.B. and T.M.A.W. acknowledge support from NSERC via the Discovery and from the Fonds de Recherche du Québec—Nature et Technologies (FRQNT). J.H.-L. acknowledges support from NSERC via the Discovery grant program, the Accelerator grant program, and the Canada Research Chair program. G.W. gratefully acknowledges support from the National Science Foundation through grant AST-1517863, from HST program No. GO-15294, and from grant No. 80NSSC17K0019 issued through the NASA Astrophysics Data Analysis Program (ADAP). Support for program No. GO-15294 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. We thank Vivian Tan and Visal Sok for their help with the Voronoi binning. We thank the JVLA staff for their immense help reducing and analyzing the data. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5?26555. These observations are associated with program Nos. GO-13677 and GO-13747.
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/5/1
Y1 - 2022/5/1
N2 - The formation of the stellar mass within galaxy cluster cores is a poorly understood process. It features the complicated physics of cooling flows, active galactic nucleus feedback, star formation, and more. Here we study the growth of the stellar mass in the vicinity of the brightest cluster galaxy (BCG) in a z = 1.7 cluster, SpARCS1049+56. We synthesize a reanalysis of existing Hubble Space Telescope imaging, a previously published measurement of the star formation rate, and the results of new radio molecular gas spectroscopy. These analyses represent the past, present, and future star formation, respectively, within this system. We show that a large amount of stellar mass - between (2.2 ± 0.5) × 1010 M ⊙ and (6.6 ± 1.2) × 1010 M ⊙ depending on the data processing - exists in a long and clumpy tail-like structure that lies roughly 12 kpc off the BCG. Spatially coincident with this stellar mass is a similarly massive reservoir ((1.0 ± 0.7) × 1011 M ⊙) of molecular gas that we suggest is the fuel for the immense star formation rate of 860 ± 130 M ⊙ yr-1, as measured by infrared observations. Hlavacek-Larrondo et al. surmised that massive, runaway cooling of the hot intracluster X-ray gas was feeding this star formation, a process that had not been observed before at high redshift. We conclude, based on the amount of fuel and current stars, that this event may be rare in the lifetime of a cluster, producing roughly 15%-21% of the intracluster light mass in one go, though perhaps a common event for all galaxy clusters.
AB - The formation of the stellar mass within galaxy cluster cores is a poorly understood process. It features the complicated physics of cooling flows, active galactic nucleus feedback, star formation, and more. Here we study the growth of the stellar mass in the vicinity of the brightest cluster galaxy (BCG) in a z = 1.7 cluster, SpARCS1049+56. We synthesize a reanalysis of existing Hubble Space Telescope imaging, a previously published measurement of the star formation rate, and the results of new radio molecular gas spectroscopy. These analyses represent the past, present, and future star formation, respectively, within this system. We show that a large amount of stellar mass - between (2.2 ± 0.5) × 1010 M ⊙ and (6.6 ± 1.2) × 1010 M ⊙ depending on the data processing - exists in a long and clumpy tail-like structure that lies roughly 12 kpc off the BCG. Spatially coincident with this stellar mass is a similarly massive reservoir ((1.0 ± 0.7) × 1011 M ⊙) of molecular gas that we suggest is the fuel for the immense star formation rate of 860 ± 130 M ⊙ yr-1, as measured by infrared observations. Hlavacek-Larrondo et al. surmised that massive, runaway cooling of the hot intracluster X-ray gas was feeding this star formation, a process that had not been observed before at high redshift. We conclude, based on the amount of fuel and current stars, that this event may be rare in the lifetime of a cluster, producing roughly 15%-21% of the intracluster light mass in one go, though perhaps a common event for all galaxy clusters.
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U2 - 10.3847/1538-4357/ac61dd
DO - 10.3847/1538-4357/ac61dd
M3 - Article
AN - SCOPUS:85130053685
SN - 0004-637X
VL - 930
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 25
ER -