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Title:
IR and UV Galaxies at z = 0.6: Evolution of Dust Attenuation and Stellar Mass as Revealed by SWIRE and GALEX
Authors:
Xu, C. Kevin; Shupe, David; Buat, Veronique; Rowan-Robinson, Michael; Babbedge, Thomas; Iglesias-Páramo, Jorge; Takeuchi, Tsutomu T.; Barlow, Tom A.; Conrow, Tim; Fang, Fan; Forster, Karl; Friedman, Peter G.; Gonzales-Solares, Eduardo; Lonsdale, Carol; Martin, D. Christopher; Morrissey, Patrick; Neff, Susan G.; Schiminovich, David; Seibert, Mark; Small, Todd; Smith, Gene; Surace, Jason; Wyder, Ted K.
Affiliation:
AA(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.; Infrared Processing and Analysis Center, California Institute of Technology 100-22, Pasadena, CA 91125.), AB(Spitzer Science Center, California Institute of Technology, Mail Stop 220-6, Pasadena, CA 91125.), AC(Observatoire Astronomique Marseille Provence, Laboratoire d'Astrophysique de Marseille, 13012 Marseille, France.), AD(Astrophysics Group, Blackett Laboratory, Imperial College of Science Technology and Medicine, Prince Consort Road, London SW7 2BZ, UK.), AE(Astrophysics Group, Blackett Laboratory, Imperial College of Science Technology and Medicine, Prince Consort Road, London SW7 2BZ, UK.), AF(Instituto de Astrofisica de Andlucia (CSIC), Camino Bajo de Huetor 50, 18008 Granada, Spain.), AG(Astronomical Institute, Tohoku University, Aoba, Aramaki, Aoba-ku, Sendai 980-8578, Japan.), AH(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AI(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AJ(Spitzer Science Center, California Institute of Technology, Mail Stop 220-6, Pasadena, CA 91125.), AK(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AL(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AM(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK.), AN(Infrared Processing and Analysis Center, California Institute of Technology 100-22, Pasadena, CA 91125.), AO(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AP(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AQ(Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MD 20771.), AR(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AS(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AT(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AU(Center for Astrophysics and Space Sciences, University of California, San Diego, La Jolla, CA 92093-0424.), AV(Spitzer Science Center, California Institute of Technology, Mail Stop 220-6, Pasadena, CA 91125.), AW(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.)
Publication:
The Astrophysical Journal Supplement Series, Volume 173, Issue 2, pp. 432-440. (ApJS Homepage)
Publication Date:
12/2007
Origin:
UCP
ApJ Keywords:
ISM: Dust, Extinction, Galaxies: Active, Galaxies: Evolution, Infrared: Galaxies, Ultraviolet: Galaxies
DOI:
10.1086/516641
Bibliographic Code:
2007ApJS..173..432X

Abstract

We study dust attenuation and stellar mass of z~0.6 star-forming galaxies using new SWIRE observations in IR and GALEX observations in UV. Two samples are selected from the SWIRE and GALEX source catalogs in the SWIRE/GALEX field ELAIS-N1-00 (Ω=0.8 deg2). The UV-selected sample has 600 galaxies with photometric redshift (hereafter photo-z) 0.5<=z<=0.7 and NUV<=23.5 (corresponding to LFUV>=109.6 Lsolar). The IR-selected sample contains 430 galaxies with f24μm>=0.2 mJy (Ldust>=1010.8 Lsolar) in the same photo-z range. It is found that the mean Ldust/LFUV ratios of the z=0.6 UV galaxies are consistent with that of their z=0 counterparts of the same LFUV. For IR galaxies, the mean Ldust/LFUV ratios of the z=0.6 LIRGs (Ldust~1011 Lsolar) are about a factor of 2 lower than local LIRGs, whereas z=0.6 ULIRGs (Ldust~1012 Lsolar) have the same mean Ldust/LFUV ratios as their local counterparts. This is consistent with the hypothesis that the dominant component of LIRG population has changed from large, gas-rich spirals at z>0.5 to major mergers at z=0. The stellar mass of z=0.6 UV galaxies of LFUV<=1010.2 Lsolar is about a factor of 2 less than their local counterparts of the same luminosity, indicating growth of these galaxies. The mass of z=0.6 UV luminous galaxies (UVLGs: LFUV>1010.2 Lsolar) and IR-selected galaxies, which are nearly exclusively LIRGs and ULIRGs, is the same as their local counterparts.
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