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An Extreme Starburst in the Core of a Rich Galaxy Cluster at z = 1.7

Webb, Tracy and Noble, Allison and DeGroot, Andrew and Wilson, Gillian and Muzzin, Adam and Bonaventura, Nina and Cooper, Mike and Delahaye, Anna and Foltz, Ryan and Lidman, Chris and Surace, Jason and Yee, H. K. C. and Chapman, Scott and Dunne, Loretta and Geach, James and Hayden, Brian and Hildebrandt, Hendrik and Huang, Jiasheng and Pope, Alexandra and Smith, Matthew W. L. and Perlmutter, Saul and Tudorica, Alex (2015) An Extreme Starburst in the Core of a Rich Galaxy Cluster at z = 1.7. Astrophysical Journal, 809 (2). Art. No. 173. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20151020-104723834

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Abstract

We have discovered an optically rich galaxy cluster at z = 1.7089 with star formation occurring in close proximity to the central galaxy. The system, SpARCS104922.6+564032.5, was detected within the Spitzer Adaptation of the red-sequence Cluster Survey, and confirmed through Keck-MOSFIRE spectroscopy. The rest-frame optical richness of N_(gal) (500 kpc) = 30 ± 8 implies a total halo mass, within 500 kpc, of ~3.8 ± 1.2 × 10^(14) M⊙, comparable to other clusters at or above this redshift. There is a wealth of ancillary data available, including Canada–France–Hawaii Telescope optical, UKIRT-K, Spitzer-IRAC/MIPS, and Herschel-SPIRE. This work adds submillimeter imaging with the SCUBA2 camera on the James Clerk Maxwell Telescope and near-infrared imaging with the Hubble Space Telescope. The mid/far-infrared (M/FIR) data detect an Ultra-luminous Infrared Galaxy spatially coincident with the central galaxy, with L_(IR) = 6.2 ± 0.9 × 10^(12) L⊙. The detection of polycyclic aromatic hydrocarbons at z = 1.7 in a Spitzer-IRS spectrum of the source implies the FIR luminosity is dominated by star formation (an Active Galactic Nucleus contribution of 20%) with a rate of ~860 ± 130 M⊙ yr^(−1). The optical source corresponding to the IR emission is likely a chain of >10 individual clumps arranged as "beads on a string" over a linear scale of 66 kpc. Its morphology and proximity to the Brightest Cluster Galaxy (BCG) imply a gas-rich interaction at the center of the cluster triggered the star formation. This system indicates that wet mergers may be an important process in forming the stellar mass of BCGs at early times.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/809/2/173DOIArticle
http://iopscience.iop.org/article/10.1088/0004-637X/809/2/173/metaPublisherArticle
ORCID:
AuthorORCID
Noble, Allison0000-0003-1832-4137
Wilson, Gillian0000-0002-6572-7089
Muzzin, Adam0000-0002-9330-9108
Lidman, Chris0000-0003-1731-0497
Surace, Jason0000-0001-7291-0087
Geach, James0000-0003-4964-4635
Pope, Alexandra0000-0001-8592-2706
Additional Information:© 2015 The American Astronomical Society. Received 2015 February 17; accepted 2015 July 2; published 2015 August 21. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Financial support for this work was provided by NASA through program GO-13677 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. This material is based upon work supported in part by the US Department of Energy, Office of Science, Office of High Energy Physics, under contract No. AC02-05CH11231. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. L.D. acknowledges support from European Research Council Advanced Grant: cosmicism. T.M.A.W. acknowledges the support of an NSERC Discovery Grant. Financial support for this work was provided by NASA through programs GO-13306, GO-13677, GO-13747, GO-13845, and GO-14327 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. Facilities: HST (WFC3) - Hubble Space Telescope satellite, Spitzer - Spitzer Space Telescope satellite, JCMT - James Clerk Maxwell Telescope, Keck:I - , Herschel - European Space Agency's Herschel space observatory, CFHT - Canada-France-Hawaii Telescope, UKIRT - United Kingdom Infrared Telescope.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
NASAGO-13677
NASANAS 5-26555
Department of Energy (DOE)AC02-05CH11231
European Research Council (ERC)UNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
NASAGO-13306
NASAGO-13677
NASAGO-13747
NASAGO-13845
NASAGO-14327
Association of Universities for Research in Astronomy (AURA)UNSPECIFIED
Subject Keywords:galaxies: clusters: general – galaxies: evolution – galaxies: interactions – galaxies: starburst
Issue or Number:2
Record Number:CaltechAUTHORS:20151020-104723834
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20151020-104723834
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:61322
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:20 Oct 2015 18:11
Last Modified:07 Nov 2019 23:47

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