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Simulating the Flattening – Metallicity Relation of Dwarf Elliptical Galaxies

Published online by Cambridge University Press:  21 April 2007

E. Emsellem ,
H. Wozniak ,
G. Massacrier ,
J.-F. Gonzalez ,
J. Devriendt ,
N. Champavert ,
D. Michielsen ,
S. Valcke  and
S. De Rijcke
D. Michielsen*
Affiliation:
School of Physics and Astronomy, University of Nottingham, University Park, Nottingham NG7 2RD, UK
S. Valcke
Affiliation:
Sterrenkundig Observatorium, Ghent University, Krijgslaan 281, 9000 Ghent, Belgium
S. De Rijcke
Affiliation:
Sterrenkundig Observatorium, Ghent University, Krijgslaan 281, 9000 Ghent, Belgium
*
[email protected]
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Abstract

Elliptical galaxies follow a well-known luminosity – metallicity (L − Z) relation, in the sense that more luminous ellipticals are observed to be more metal-rich than less luminous systems. Obviously this is a mass – Z relation, and its interpretation is that less massive galaxies had more significant outflows of metal-enriched gas at an early evolutionary stage. The apparent ellipticity (ϵ) had already been invoked to explain the large scatter in the L − Z relation, but Barazza & Binggeli (2002) observed that the relation between Z and ϵ in cluster dwarf elliptical galaxies (dEs) could even be stronger than the relation with mass. The idea is that outflow of metal-enriched gas preferentially occurs along the minor axis, making ϵ a critical parameter for Z in dwarfs. Here, we test this hypothesis using high-resolution N-body/SPH simulations including chemical feedback of dEs with different flattenings.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 24: CRAL-2006. Chemodynamics: From First Stars to Local Galaxies , 2007 , pp. 287 - 288
Copyright
© EAS, EDP Sciences, 2007

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