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Modeling of star formation histories of dwarf ellipticals

Published online by Cambridge University Press:  08 November 2005

N. Arimoto
N. Arimoto
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan email: [email protected]
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Abstract

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Cosmological numerical simulations suggest that dSphs and dEs formed hierarchically via assembling much smaller stellar/gas clumps. Star formation had occurred intensively during the building up phase that is shorter than ∼1 Gyr. Dark matter assembled hierarchically, while gas collapsed dissipatively; as a result the metallicity gradient was built up and stars at the galaxy centre tend to have larger rotational velocity and smaller velocity dispersion. There are increasing evidences, however, that suggest rather long-lasted star formation in dwarf galaxies with much smaller SFRs, with which cosmological simulations need to be reconciled.

Keywords

galaxies: abundancesgalaxies: dwarfgalaxies: elliptical and lenticularcDgalaxies: evolutiongalaxies: formation(galaxies:) Local Groupgalaxies: stellar content
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Colloquium C198: Near-Field Cosmology with Dwarf Elliptical Galaxies , March 2005 , pp. 17 - 24
Copyright
© 2005 International Astronomical Union