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Bulges vs elliptical galaxies: some clues from their formation in a cosmological context

Published online by Cambridge University Press:  01 July 2007

R. Domínguez-Tenreiro ,
F. J. Martínez-Serrano ,
A. Serna ,
M. Mollá  and
J. Oñorbe
R. Domínguez-Tenreiro
Affiliation:
Department of Theoretical Physics, Universidad Autónoma de Madrid, 28049 Madrid, Spain email: rosa.dominguez@uam.es
F. J. Martínez-Serrano
Affiliation:
Department of Physics and C.A., Universidad Miguel Hernández, 03206 Elche, Spain
A. Serna
Affiliation:
Department of Physics and C.A., Universidad Miguel Hernández, 03206 Elche, Spain
M. Mollá
Affiliation:
Department of Fundamental Research, CIEMAT, 28040 Madrid, Spain
J. Oñorbe
Affiliation:
Department of Theoretical Physics, Universidad Autónoma de Madrid, 28049 Madrid, Spain email: rosa.dominguez@uam.es
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Abstract

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We report on an extension, through cosmological simulations, of the two-phase formation scenario for elliptical galaxies to classical spiral bulges. In particular, we analyze the possibility that the old stellar population of bulges forms in a fast phase, while the younger stellar component forms or is assembled in a slow phase, in part from disk material suffering instabilities and in part through satellite capture or mergers.

Keywords

methods: hydrodynamicsgalaxies: formationgalaxies: bulgesstars: formation

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