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Ultraviolet and Far-Infrared-selected Star-forming Galaxies at z = 0: Differences and Overlaps

Xu, Kevin C. and Barlow, Tom A. and Forster, Karl and Friedman, Peter G. and Madore, Barry F. and Martin, D. Christopher and Morrissey, Patrick and Schiminovich, David and Small, Todd and Wyder, Ted K. (2006) Ultraviolet and Far-Infrared-selected Star-forming Galaxies at z = 0: Differences and Overlaps. Astrophysical Journal, 646 (2). pp. 834-840. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20110616-113836578

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Abstract

We study two samples of local galaxies, one UV (GALEX) selected and the other FIR (IRAS) selected, to address the question of whether UV and FIR surveys see two sides ("bright" and "dark") of the star formation of the same population of galaxies or two different populations of star-forming galaxies. No significant difference between the L_(tot) (=L_(60) + L_(FUV)) luminosity functions of the UV and FIR samples is found. In addition, after the correction for the "Malmquist bias" (bias for flux-limited samples), the FIR-to-UV ratio versus L_(tot) relations of the two samples are consistent with each other. In the range of 9 ≾ log(L_(tot)/L_⊙) ≾ 12, both can be approximated by a simple linear relation of log(L_(60)/L_(FUV)) = log(L_(tot)/L_⊙) - 9.66. These are consistent with the hypothesis that the two samples represent the same population of star-forming galaxies, and their well-documented differences in L_(tot) and in FIR-to-UV ratio are due only to the selection effect. A comparison between the UV luminosity functions shows marginal evidence for a population of faint UV galaxies missing in the FIR-selected sample. The contribution from these "FIR-quiet" galaxies to the overall UV population is insignificant, given that the K-band luminosity functions (i.e., the stellar mass functions) of the two samples do not show any significant difference.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/504974DOIArticle
http://iopscience.iop.org/0004-637X/646/2/834PublisherArticle
ORCID:
AuthorORCID
Madore, Barry F.0000-0002-1576-1676
Additional Information:© 2006 The American Astronomical Society. Received 2005 December 22; accepted 2006 April 3. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA’s support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the South Korean Ministry of Science and Technology. We thank an anonymous referee for very constructive comments. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
Group:Space Astrophysics Laboratory
Funders:
Funding AgencyGrant Number
NASAUNSPECIFIED
Subject Keywords:dust: extinction; galaxies: active; galaxies: luminosity function, mass function; galaxies: starburst; infrared: galaxies; stars: formation; ultraviolet: galaxies
Issue or Number:2
Record Number:CaltechAUTHORS:20110616-113836578
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20110616-113836578
Official Citation:Ultraviolet and Far-Infrared-selected Star-forming Galaxies at z = 0: Differences and Overlaps C. Kevin Xu, Veronique Buat, Jorge Iglesias-Páramo, Tsutomu T. Takeuchi, Tom A. Barlow, Luciana Bianchi, Jose Donas, Karl Forster, Peter G. Friedman, Timothy M. Heckman, Patrick N. Jelinsky, Young-Wook Lee, Barry F. Madore, Roger F. Malina, D. Christopher Martin, Bruno Milliard, Patrick Morrissey, R. Michael Rich, Susan G. Neff, David Schiminovich, Oswald H. W. Siegmund, Todd Small, Alex S. Szalay, Barry Y. Welsh, Ted K. Wyder, and Sukyoung Yi doi: 10.1086/504974
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:24033
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:16 Jun 2011 20:24
Last Modified:03 Oct 2019 02:52

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