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A census of the physical parameters of nearby galaxies

Published online by Cambridge University Press:  01 December 2006

Anna Gallazzi ,
J. Brinchmann ,
S. Charlot  and
S. D. M. White
Anna Gallazzi
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany email: gallazzi@mpia-hd.mpg.de Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching bei München, Germany
J. Brinchmann
Affiliation:
Centro de Astrofísica da Universidade do Porto, Rua das Estrelas – 4150-762 Porto, Portugal
S. Charlot
Affiliation:
Institut d'Astrophysique du CNRS, 98 bis Boulevard Arago, F-75014 Paris, France
S. D. M. White
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching bei München, Germany
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Abstract

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We combine together physical parameters estimates for a large sample of galaxies drawn from the Sloan Digital Sky Survey Data Release Two (SDSS DR2), spanning wide ranges in galaxy properties, in order to provide a census of the physical parameters of galaxies in the local Universe. Stellar metallicities, masses and ages for this sample have been estimated comparing the strengths of selected absorption features in each observed spectrum to a comprehensive Monte Carlo library of star formation histories, following a Bayesian statistical approach. This allows us also to derive the total amount of metals locked up in stars today, and hence the average stellar metallicity of galaxies in the local Universe, finding a value of . We also quantify the relative contribution to the total densities of mass and metals in stars from galaxies with different properties.

Keywords

galaxies: formationgalaxies: evolutiongalaxies: stellar content
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S241: Stellar Populations as Building Blocks of Galaxies , December 2006 , pp. 556 - 560
Copyright
Copyright © International Astronomical Union 2007

References

Abazajian, K. et al. , 2004, AJ, 128, 502CrossRefGoogle Scholar
Balogh, M. L., Pearce, F. R., Bower, R. G., & Kay, S. T., 2001, MNRAS, 326, 1228CrossRefGoogle Scholar
Chabrier, G., 2003, PASP, 115, 763CrossRefGoogle Scholar
Bruzual, G., & Charlot, S., 2003, MNRAS, 344, 1000CrossRefGoogle Scholar
Calura, F., & Matteucci, F., 2004, MNRAS, 350, 351CrossRefGoogle Scholar
Cid Fernandes, R., Mateus, A., Sodré, L., Stasińska, G. & Gomes, J. M., 2005, MNRAS, 358, 363CrossRefGoogle Scholar
Davé, R. & Oppenheimer, B. D., 2007, MNRAS, 374, 427CrossRefGoogle Scholar
Edmunds, M. G., 1990, MNRAS, 246, 678Google Scholar
Finoguenov, A., Burkert, A., & Böhringer, H., 2003, APJ, 594, 136CrossRefGoogle Scholar
Fukugita, M., Hogan, C. J., & Peebles, P. J. E., 1998, APJ, 503, 518CrossRefGoogle Scholar
Gallazzi, A., Charlot, S., Brinchmann, J., White, S. D. M., & Tremonti, C. A., 2005, MNRAS, 362, 41CrossRefGoogle Scholar
Gallazzi, A., Charlot, S., Brinchmann, J., & White, S. D. M., 2006, MNRAS, 370, 1106CrossRefGoogle Scholar
Glazebrook, K. et al. , 2003, APJ, 587, 55CrossRefGoogle Scholar
Huang, J.-S., Glazebrook, K., Cowie, L. L., & Tinney, C., 2003, APJ, 584, 203CrossRefGoogle Scholar
Kannappan, S. J., 2004, APJL, 611, L89CrossRefGoogle Scholar
Kauffmann, G. et al. , 2003, MNRAS, 341, 33CrossRefGoogle Scholar
Lilly, S. J., Le, Fevre O., Hammer, F., & Crampton, D., 1996, APJL, 460, L1CrossRefGoogle Scholar
Madau, P., Pozzetti, L., & Dickinson, M., 1998, APJ, 498, 106CrossRefGoogle Scholar
Panter, B., Heavens, A., & Jimenez, R., 2003, MNRAS, 343, 1145CrossRefGoogle Scholar
Thomas, D., Maraston, C., Bender, R., & de Oliveira, C. M., 2005, APJ, 621, 673CrossRefGoogle Scholar
Vazdekis, A., 1999, APJ, 513, 224CrossRefGoogle Scholar