Mobasher, Bahram and Dahlen, Tomas and Hopkins, Andrew and Scoville, Nick Z. and Capak, Peter and Rich, R. Michael and Sanders, David B. and Schinnerer, Eva and Ilbert, Olivier and Salvato, Mara and Sheth, Kartik (2009) Relation between stellar mass and star-formation activity in galaxies. Astrophysical Journal, 690 (2). pp. 1074-1083. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:MOBapj09
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Abstract
For a mass-selected sample of 66544 galaxies with photometric redshifts (z phot) from the Cosmic Evolution Survey (COSMOS), we examine the evolution of star-formation activity as a function of stellar mass in galaxies. We estimate the cosmic star-formation rates (SFRs) over the range 0.2 < z phot < 1.2, using the rest-frame 2800 Å flux (corrected for extinction). We find the mean SFR to be a strong function of the galactic stellar mass at any given redshift, with massive systems (log(M/M☉) > 10.5) contributing less (by a factor of ~5) to the total star-formation rate density (SFRD). Combining data from the COSMOS and Gemini Deep Deep Survey, we extend the SFRD-z relation as a function of stellar mass to z ~ 2. For massive galaxies, we find a steep increase in the SFRD-z relation to z ~ 2; for the less-massive systems, the SFRD which also increases from z = 0 to 1 levels off at z ~ 1. This implies that the massive systems have had their major star-formation activity at earlier epochs (z > 2) than the lower-mass galaxies. We study changes in the SFRDs as a function of both redshift and stellar mass for galaxies of different spectral types. We find that the slope of the SFRD-z relation for different spectral types of galaxies is a strong function of their stellar mass. For low- and intermediate-mass systems, the main contribution to the cosmic SFRD comes from the star-forming galaxies while, for more-massive systems, the evolved galaxies are the most dominant population.
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| Additional Information: | © 2009 The American Astronomical Society. Received 2008 April 8, accepted for publication 2008 August 18. Published 2008 December 2. Print publication: Issue 2 (2009 January 10). Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc., under NASA contract NAS 5-26555; also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory under Large Program 175.A-0839, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; and the Canada-France-Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the National Research Council of Canada, the Canadian Astronomy Data Centre, the Centre National de la Recherche Scientifique de France, TERAPIX and the University of Hawaii. Online-only material: color figure. | ||||||||||||||||||
| Group: | COSMOS, Infrared Processing and Analysis Center (IPAC) | ||||||||||||||||||
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| Subject Keywords: | galaxies: evolution; galaxies: starburst | ||||||||||||||||||
| Record Number: | CaltechAUTHORS:MOBapj09 | ||||||||||||||||||
| Persistent URL: | http://resolver.caltech.edu/CaltechAUTHORS:MOBapj09 | ||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||
| ID Code: | 12515 | ||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||
| Deposited By: | Archive Administrator | ||||||||||||||||||
| Deposited On: | 12 Dec 2008 03:37 | ||||||||||||||||||
| Last Modified: | 10 Oct 2017 17:57 |
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