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Stellar metallicity distributions in local dwarf spheroidal galaxies: a comparison between model and observations

Published online by Cambridge University Press:  13 April 2010

Gustavo A. Lanfranchi  and
Francesca Matteucci
Gustavo A. Lanfranchi
Affiliation:
Núcleo de Astrofísica Teórica, Universidade Cruzeiro do Sul, R. Galvão Bueno 868, Liberdade, 01506-000, São Paulo, SP, Brazil email: [email protected]
Francesca Matteucci
Affiliation:
Dipartimento di Astronomia-Universitá di Trieste, Via G. B. Tiepolo 11, 34131 Trieste, Italy
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Abstract

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We analyze the main populations of 6 local Dwarf Spheroidal Galaxies by comparing the observed stellar metallicity distributions with the predictions of chemical evolution models. The predicted metallicity distributions of stars generally exhibit a low range of metallicities, a peak below the one of the MW disc in the solar neighborhood (but similar to the Halo), and a sharp decrease at higher metallicities in agreement with observations. The position of the peak is related to the low star formation rates adopted whereas the sharp decrease is a consequence of the occurrence of strong galactic winds. In the low metallicity tail of the distributions we predict a low number of stars in agreement with observations.

Keywords

stars: abundancesgalaxies: dwarfLocal Group
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 370 - 371
Copyright
Copyright © International Astronomical Union 2010

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