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The Star-Formation History of BCGs to z = 1.8 from the SpARCS/SWIRE Survey: Evidence for significant in-situ star formation at high-redshift

Webb, Tracy M. A. and Muzzin, Adam and Noble, Alison and Bonaventura, Nina and Geach, James and Hezevah, Yashar and Lidman, Chris and Wilson, Gillian and Yee, H. K. C. and Surace, Jason and Shupe, David (2015) The Star-Formation History of BCGs to z = 1.8 from the SpARCS/SWIRE Survey: Evidence for significant in-situ star formation at high-redshift. Astrophysical Journal, 814 (2). Art. No. 96. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20151222-105600116

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Abstract

We present the results of an MIPS-24 μm study of the brightest cluster galaxies (BCGs) of 535 high-redshift galaxy clusters. The clusters are drawn from the Spitzer Adaptation of the Red-Sequence Cluster Survey, which effectively provides a sample selected on total stellar mass, over 0.2 < z < 1.8 within the Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey fields. Twenty percent, or 106 clusters, have spectroscopically confirmed redshifts, and the rest have redshifts estimated from the color of their red sequence. A comparison with the public SWIRE images detects 125 individual BCGs at 24 μm ≳ 100 μJy, or 23%. The luminosity-limited detection rate of BCGs in similar richness clusters (N_(gal) > 12) increases rapidly with redshift. Above z ~ 1, an average of ~20% of the sample have 24 μm inferred infrared luminosities of L_(IR) > 10^(12) L_⊙, while the fraction below z ~ 1 exhibiting such luminosities is <1%. The Spitzer-IRAC colors indicate the bulk of the 24 μm detected population is predominantly powered by star formation, with only 7/125 galaxies lying within the color region inhabited by active galactic nuclei (AGNs). Simple arguments limit the star formation activity to several hundred million years and this may therefore be indicative of the timescale for AGN feedback to halt the star formation. Below redshift z ~ 1, there is not enough star formation to significantly contribute to the overall stellar mass of the BCG population, and therefore BCG growth is likely dominated by dry mergers. Above z ~ 1, however, the inferred star formation would double the stellar mass of the BCGs and is comparable to the mass assembly predicted by simulations through dry mergers. We cannot yet constrain the process driving the star formation for the overall sample, though a single object studied in detail is consistent with a gas-rich merger.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/814/2/96DOIArticle
http://iopscience.iop.org/article/10.1088/0004-637X/814/2/96PublisherArticle
http://arxiv.org/abs/1508.07302arXivDiscussion Paper
ORCID:
AuthorORCID
Muzzin, Adam0000-0002-9330-9108
Noble, Alison0000-0003-1832-4137
Geach, James0000-0003-4964-4635
Surace, Jason0000-0001-7291-0087
Shupe, David0000-0003-4401-0430
Additional Information:© 2015 American Astronomical Society. Received 2015 March 13; accepted 2015 August 19; published 2015 November 20. Funding for PRIMUS is provided by NSF (AST-0607701, AST-0908246, AST-0908442, AST-0908354) and NASA (Spitzer-1356708, 08-ADP08-0019, NNX09AC95G). T.M.A.W. acknowledges the support of an NSERC Discovery Grant. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. 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: Spitzer Space Telescope (MIPS; IRAC) - , Magellan (IMACS) - , CTIO - , CFHT - Canada-France-Hawaii Telescope
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NSFAST-0607701
NSFAST-0908246
NSFAST-0908442
NSFAST-0908354
NASASpitzer-1356708
NASA08-ADP08-0019
NASANNX09AC95G
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
NASAGO-13306
NASAGO-13677
NASAGO-13747
NASAGO-13845
NASAGO-14327
Space Telescope Science InstituteUNSPECIFIED
NASANAS 5-26555
Subject Keywords:galaxies: clusters: general; galaxies: evolution; galaxies: formation; galaxies: star formation
Issue or Number:2
Record Number:CaltechAUTHORS:20151222-105600116
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20151222-105600116
Official Citation:Tracy M. A. Webb et al 2015 ApJ 814 96
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:63140
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:22 Dec 2015 19:59
Last Modified:07 Nov 2019 23:24

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