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The UV-Optical Galaxy Color-Magnitude Diagram. I. Basic Properties

Wyder, Ted K. and Martin, D. Christopher and Schiminovich, David and Seibert, Mark and Budavári, Tamás and Treyer, Marie A. and Barlow, Tom A. and Forster, Karl and Friedman, Peter G. and Morrissey, Patrick and Neff, Susan G. and Small, Todd and Bianchi, Luciana and Donas, José and Heckman , Timothy M. and Lee, Young-Wook and Madore, Barry F. and Milliard, Bruno and Rich, R. Michael and Szalay, Alex S. and Welsh, Barry Y. and Yi, Sukyoung K. (2007) The UV-Optical Galaxy Color-Magnitude Diagram. I. Basic Properties. Astrophysical Journal Supplement Series, 173 (2). pp. 293-314. ISSN 0067-0049. http://resolver.caltech.edu/CaltechAUTHORS:20091117-113251451

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Abstract

We have analyzed the bivariate distribution of galaxies as a function of ultraviolet-optical colors and absolute magnitudes in the local universe. The sample consists of galaxies with redshifts and optical photometry from the Sloan Digital Sky Survey (SDSS) main galaxy sample matched with detections in the near-ultraviolet (NUV) and far-ultraviolet (FUV) bands in the Medium Imaging Survey being carried out by the Galaxy Evolution Explorer (GALEX) satellite. In the (NUV − r)_(0.1) versus M_(r,0.1) galaxy color-magnitude diagram, the galaxies separate into two well-defined blue and red sequences. The (NUV − r)_(0.1) color distribution at each M_(r,0.1) is not well fit by the sum of two Gaussians due to an excess of galaxies in between the two sequences. The peaks of both sequences become redder with increasing luminosity, with a distinct blue peak visible up to M_(r,0.1) ~ − 23. The r_(0.1)-band luminosity functions vary systematically with color, with the faint-end slope and characteristic luminosity gradually increasing with color. After correcting for attenuation due to dust, we find that approximately one-quarter of the color variation along the blue sequence is due to dust, with the remainder due to star formation history and metallicity. Finally, we present the distribution of galaxies as a function of specific star formation rate and stellar mass. The specific star formation rates imply that galaxies along the blue sequence progress from low-mass galaxies with star formation rates that increase somewhat with time to more massive galaxies with a more or less constant star formation rate. Above a stellar mass of ~10^(10.5) M_☉, galaxies with low ratios of current to past averaged star formation rate begin to dominate.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/521402DOIArticle
http://www.iop.org/EJ/abstract/0067-0049/173/2/293/PublisherArticle
ORCID:
AuthorORCID
Madore, Barry F.0000-0002-1576-1676
Additional Information:© 2007 American Astronomical Society. Print publication: Issue 2 (2007 December); received 2006 November 14, accepted for publication 2007 June 26. 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 Korean Ministry of Science and Technology. Facilities: GALEX
Group:Space Radiation Laboratory, Space Astrophysics Laboratory
Subject Keywords:galaxies: evolution; galaxies: fundamental parameters; galaxies: luminosity function, mass function; galaxies: statistics; ultraviolet: galaxies
Record Number:CaltechAUTHORS:20091117-113251451
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20091117-113251451
Official Citation:The UV-Optical Galaxy Color-Magnitude Diagram. I. Basic Properties Ted K. Wyder, D. Christopher Martin, David Schiminovich, Mark Seibert, Tamás Budavári, Marie A. Treyer, Tom A. Barlow, Karl Forster, Peter G. Friedman, Patrick Morrissey, Susan G. Neff, Todd Small, Luciana Bianchi, José Donas, Timothy M. Heckman, Young-Wook Lee, Barry F. Madore, Bruno Milliard, R. Michael Rich, Alex S. Szalay, Barry Y. Welsh, and Sukyoung K. Yi 2007 ApJS 173 293-314 doi: 10.1086/521402
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:16731
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:25 Nov 2009 17:49
Last Modified:22 May 2017 17:07

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