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High resolution spectral models for solar scaled and α-enhanced compositions

Published online by Cambridge University Press:  01 December 2006

P. Coelho ,
G. Bruzual ,
S. Charlot ,
A. Weiss  and
B. Barbuy
P. Coelho
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, Garching, Germany Universidade de São Paulo, IAG, Rua do Matão 1226, São Paulo 05508-900, Brazil
G. Bruzual
Affiliation:
Centro de Investigaciones de Astronomia, Merida, Venezuela
S. Charlot
Affiliation:
Institut d'Astrophysique, 98bis Bd. Arago, 75014 Paris, France
A. Weiss
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, Garching, Germany
B. Barbuy
Affiliation:
Universidade de São Paulo, IAG, Rua do Matão 1226, São Paulo 05508-900, Brazil
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Abstract

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In the last years, observations made by large international consortia made available hundreds of thousands of high-resolution spectra of galaxies in the local and distant Universe. The interpretation of these spectra in terms of stellar ages and metallicities is the key to reconstructing the star formation and chemical enrichment histories of the Universe. However, current spectral models rely on libraries of observed stars in the solar neighborhood, hampering our hability in interpreting populations that had undergone different star formation histories. Although it is available in the literature Lick/IDS model indices with variable chemical mixtures, we were still lacking high resolution spectral energy distribution models. Those models are required if we want to exploit the total amount of information contained in observed galaxy spectra. We present here our work aiming at the development of such models, constructed with a consistent set of synthetic stellar library and new stellar evolution models.

Keywords

galaxies: stellar contentgalaxies: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S241: Stellar Populations as Building Blocks of Galaxies , December 2006 , pp. 138 - 142
Copyright
Copyright © International Astronomical Union 2007

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