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Title:
UV to IR SEDs of UV-Selected Galaxies in the ELAIS Fields: Evolution of Dust Attenuation and Star Formation Activity from z = 0.7 to 0.2
Authors:
Iglesias-Páramo, J.; Buat, V.; Hernández-Fernández, J.; Xu, C. K.; Burgarella, D.; Takeuchi, T. T.; Boselli, A.; Shupe, D.; Rowan-Robinson, M.; Babbedge, T.; Conrow, T.; Fang, F.; Farrah, D.; González-Solares, E.; Lonsdale, C.; Smith, G.; Surace, J.; Barlow, T. A.; Forster, K.; Friedman, P. G.; Martin, D. C.; Morrissey, P.; Neff, S. G.; Schiminovich, D.; Seibert, M.; Small, T.; Wyder, T. K.; Bianchi, L.; Donas, J.; Heckman, T. M.; Lee, Y.-W.; Madore, B. F.; Milliard, B.; Rich, R. M.; Szalay, A. S.; Welsh, B. Y.; Yi, S. K.
Affiliation:
AA(Instituto de Astrofísica de Andalucía (IAA, CSIC), Camino Bajo de Huétor 50, 18008 Granada, Spain.), AB(Observatoire Astronomique Marseille Provence, Laboratoire d'Astrophysique de Marseille, 13012, Marseille, France.), AC(Instituto de Astrofísica de Andalucía (IAA, CSIC), Camino Bajo de Huétor 50, 18008 Granada, Spain.), AD(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.), AE(Observatoire Astronomique Marseille Provence, Laboratoire d'Astrophysique de Marseille, 13012, Marseille, France.), AF(Institute for Advanced Research, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan.), AG(Observatoire Astronomique Marseille Provence, Laboratoire d'Astrophysique de Marseille, 13012, Marseille, France.), AH(Spitzer Science Center, California Institute of Technology, Mail Stop 220-6, Pasadena, CA 91125.), AI(Astrophysics Group, Blackett Laboratory, Imperial College of Science, Technology and Medicine, Prince Consort Road, London SW7 2BZ, UK.), AJ(Astrophysics Group, Blackett Laboratory, Imperial College of Science, Technology and Medicine, Prince Consort Road, London SW7 2BZ, UK.), AK(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AL(Spitzer Science Center, California Institute of Technology, Mail Stop 220-6, Pasadena, CA 91125.), AM(Department of Astronomy, Cornell University, Ithaca, NY 14853.), AN(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK.), AO(Infrared Processing and Analysis Center, California Institute of Technology, 100-22, Pasadena, CA 91125.), AP(Center for Astrophysics and Space Sciences, University of California, San Diego, La Jolla, CA 92093-0424.), AQ(Spitzer Science Center, California Institute of Technology, Mail Stop 220-6, Pasadena, CA 91125.), 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(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AV(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AW(Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MD 20771.), AX(Department of Astronomy, Columbia University, New York, NY 10027.), AY(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AZ(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), BA(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), BB(Center for Astrophysical Sciences, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BC(Observatoire Astronomique Marseille Provence, Laboratoire d'Astrophysique de Marseille, 13012, Marseille, France.), BD(Department of Physics and Astronomy, The Johns Hopkins University, Homewood Campus, Baltimore, MD 21218.), BE(Center for Space Astrophysics, Yonsei University, Seoul 120-749, Korea.), BF(Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101.), BG(Observatoire Astronomique Marseille Provence, Laboratoire d'Astrophysique de Marseille, 13012, Marseille, France.), BH(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095.), BI(Department of Physics and Astronomy, The Johns Hopkins University, Homewood Campus, Baltimore, MD 21218.), BJ(Space Sciences Laboratory, University of California at Berkeley, 601 Campbell Hall, Berkeley, CA 94720.), BK(Center for Space Astrophysics, Yonsei University, Seoul 120-749, Korea.)
Publication:
The Astrophysical Journal, Volume 670, Issue 1, pp. 279-294. (ApJ Homepage)
Publication Date:
11/2007
Origin:
UCP
ApJ Keywords:
Galaxies: Evolution, Surveys, Ultraviolet: Galaxies
DOI:
10.1086/521867
Bibliographic Code:
2007ApJ...670..279I

Abstract

We study the ultraviolet to far-infrared (hereafter UV-to-IR) SEDs of a sample of intermediate-redshift (0.2<=z<=0.7) UV-selected galaxies from the ELAIS N1 and ELAIS N2 fields by fitting a multi-wavelength data set to a library of GRASIL templates. Star formation related properties of the galaxies are derived from the library of models by using Bayesian statistics. We find a decreasing presence of galaxies with low attenuation and low total luminosity as redshift decreases, which does not hold for high total luminosity galaxies. In addition, the dust attenuation of low-mass galaxies increases as redshift decreases, and this trend seems to disappear for galaxies with M*>=1011 Msolar. This result is consistent with a mass-dependent evolution of the dust-to-gas ratio, which could be driven by a mass-dependent efficiency of star formation in star-forming galaxies. The specific star formation rates (SSFR) decrease with increasing stellar mass at all redshifts, and for a given stellar mass the SSFR decreases with decreasing redshift. The differences in the slope of the M*-SSFR relation found between this work and others at similar redshift could be explained by the adopted selection criteria of the samples, which for a UV-selected sample, favors blue, star-forming galaxies.
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