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Evolution of the Stellar-to-dark Matter Relation: Separating Star-forming and Passive Galaxies from z = 1 to 0

Tinker, Jeremy L. and Leauthaud, Alexie and Bundy, Kevin and George, Matthew R. and Behroozi, Peter and Massey, Richard and Rhodes, Jason and Wechsler, Risa H. (2013) Evolution of the Stellar-to-dark Matter Relation: Separating Star-forming and Passive Galaxies from z = 1 to 0. Astrophysical Journal, 778 (2). Art. No. 93. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20140103-083737842

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Abstract

We use measurements of the stellar mass function, galaxy clustering, and galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo mass relation (SHMR) of star forming and quiescent galaxies over the redshift range z = [0.2, 1.0]. For massive galaxies, M^* ≳ 10^(10.6) M_☉, our results indicate that star-forming galaxies grow proportionately as fast as their dark matter halos while quiescent galaxies are outpaced by dark matter growth. At lower masses, there is minimal difference in the SHMRs, implying that the majority low-mass quiescent galaxies have only recently been quenched of their star formation. Our analysis also affords a breakdown of all COSMOS galaxies into the relative numbers of central and satellite galaxies for both populations. At z = 1, satellite galaxies dominate the red sequence below the knee in the stellar mass function. But the number of quiescent satellites exhibits minimal redshift evolution; all evolution in the red sequence is due to low-mass central galaxies being quenched of their star formation. At M^* ~ 10^(10) M_☉, the fraction of central galaxies on the red sequence increases by a factor of 10 over our redshift baseline, while the fraction of quenched satellite galaxies at that mass is constant with redshift. We define a "migration rate" to the red sequence as the time derivative of the passive galaxy abundances. We find that the migration rate of central galaxies to the red sequence increases by nearly an order of magnitude from z = 1 to z = 0. These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://iopscience.iop.org/0004-637X/778/2/93/PublisherArticle
http://dx.doi.org/10.1088/0004-637X/778/2/93DOIArticle
http://arxiv.org/abs/1308.2974arXivDiscussion Paper
Additional Information:© 2013 American Astronomical Society. Received 2013 June 3; accepted 2013 September 3; published 2013 November 8. We thank the referee for many helpful comments and suggestions that have improved this work. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. The HSTCOSMOS Treasury program was supported through NASA grant HST-GO-09822. We wish to thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at http://cosmos.astro.caltech.edu/. It is a pleasure the acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman and John Good) in providing online archive and server capabilities for the COSMOS data-sets.
Group:COSMOS
Funders:
Funding AgencyGrant Number
World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan UNSPECIFIED
NASAHST-GO-09822
Subject Keywords: cosmology: observations; galaxies: evolution; galaxies: halos
Record Number:CaltechAUTHORS:20140103-083737842
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20140103-083737842
Official Citation:Evolution of the Stellar-to-dark Matter Relation: Separating Star-forming and Passive Galaxies from z = 1 to 0 Jeremy L. Tinker et al. 2013 ApJ 778 93
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:43195
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:03 Jan 2014 21:59
Last Modified:09 Jul 2015 19:48

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