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Title:
UV Star Formation Rates in the Local Universe
Authors:
Salim, Samir; Rich, R. Michael; Charlot, Stéphane; Brinchmann, Jarle; Johnson, Benjamin D.; Schiminovich, David; Seibert, Mark; Mallery, Ryan; Heckman, Timothy M.; Forster, Karl; Friedman, Peter G.; Martin, D. Christopher; Morrissey, Patrick; Neff, Susan G.; Small, Todd; Wyder, Ted K.; Bianchi, Luciana; Donas, José; Lee, Young-Wook; Madore, Barry F.; Milliard, Bruno; Szalay, Alex S.; Welsh, Barry Y.; Yi, Sukyoung K.
Affiliation:
AA(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095.; Current address: National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719; .), AB(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095.), AC(Institut d'Astrophysique de Paris, CNRS, 98 bis Boulevard Arago, F-75014 Paris, France.), AD(Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal.), AE(Department of Astronomy, Columbia University, New York, NY 10027.), AF(Department of Astronomy, Columbia University, New York, NY 10027.), AG(Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101.), AH(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095.), AI(Department of Physics and Astronomy, Johns Hopkins University, Homewood Campus, Baltimore, MD 21218.), AJ(California Institute of Technology, MC 405-47, 1200 East California Boulevard, 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(California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125.), AN(Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MD 20771.), 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(Center for Astrophysical Sciences, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AR(Laboratoire d'Astrophysique de Marseille, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, France.), AS(Center for Space Astrophysics, Yonsei University, Seoul 120-749, Korea.), AT(Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101.), AU(Laboratoire d'Astrophysique de Marseille, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, France.), AV(Department of Physics and Astronomy, Johns Hopkins University, Homewood Campus, Baltimore, MD 21218.), AW(Space Sciences Laboratory, University of California, Berkeley, 601 Campbell Hall, Berkeley, CA 94720.), AX(Center for Space Astrophysics, Yonsei University, Seoul 120-749, Korea.)
Publication:
The Astrophysical Journal Supplement Series, Volume 173, Issue 2, pp. 267-292. (ApJS Homepage)
Publication Date:
12/2007
Origin:
UCP
ApJ Keywords:
Galaxies: Active, Galaxies: Evolution, Galaxies: Fundamental Parameters, Surveys, Ultraviolet: Galaxies
DOI:
10.1086/519218
Bibliographic Code:
2007ApJS..173..267S

Abstract

We measure star formation rates (SFRs) of ~50,000 optically selected galaxies in the local universe (z~0.1)-from gas-rich dwarfs to massive ellipticals. We obtain dust-corrected SFRs by fitting the GALEX (ultraviolet) and SDSS photometry to a library of dust-attenuated population synthesis models. For star-forming galaxies, our UV-based SFRs compare remarkably well with those from SDSS-measured emission lines (Hα). Deviations from perfect agreement are shown to be due to differences in the dust attenuation estimates. In contrast to Hα measurements, UV provides reliable SFRs for galaxies with weak Hα, and where Hα is contaminated with AGN emission (1/2 of the sample). Using full-SED SFRs, we calibrate a simple prescription that uses GALEX far- and near-UV magnitudes to produce dust-corrected SFRs for normal star-forming galaxies. The specific SFR is considered as a function of stellar mass for (1) star-forming galaxies with no AGNs, (2) those hosting an AGN, and (3) galaxies without Hα emission. We find that the three have distinct star formation histories, with AGNs lying intermediate between the star-forming and the quiescent galaxies. Star-forming galaxies without an AGN lie on a relatively narrow linear sequence. Remarkably, galaxies hosting a strong AGN appear to represent the massive continuation of this sequence. On the other hand, weak AGNs, while also massive, have lower SFRs, sometimes extending to the realm of quiescent galaxies. We propose an evolutionary sequence for massive galaxies that smoothly connects normal star-forming galaxies to quiescent galaxies via strong and weak AGNs. We confirm that some galaxies with no Hα show signs of star formation in the UV. We derive a cosmic star formation density at z=0.1 with significantly smaller total error than previous measurements.
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