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Abundances in the Galactic Bulge: evidence for fast chemical enrichment

Published online by Cambridge University Press:  01 December 2006

M. Zoccali ,
A. Lecureur ,
B. Barbuy ,
V. Hill ,
A. Renzini ,
D. Minniti ,
Y. Momany ,
A. Gómez  and
S. Ortolani
M. Zoccali*
Affiliation:
P. Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile email: [email protected], [email protected]
A. Lecureur
Affiliation:
Observatoire de Paris-Meudon, 92195 Meudon Cedex, France email: [email protected], [email protected], [email protected]
B. Barbuy
Affiliation:
Universidade de São Paulo, IAG, Rua do Matão 1226, Cidade Universitária, São Paulo 05508-900, Brazil email: [email protected]
V. Hill
Affiliation:
Observatoire de Paris-Meudon, 92195 Meudon Cedex, France email: [email protected], [email protected], [email protected]
A. Renzini
Affiliation:
INAF – Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 2, I-35122 Padova, Italy email: [email protected]
D. Minniti
Affiliation:
P. Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile email: [email protected], [email protected]
Y. Momany
Affiliation:
Università di Padova, Dipartimento di Astronomia, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy email: [email protected], [email protected]
A. Gómez
Affiliation:
Observatoire de Paris-Meudon, 92195 Meudon Cedex, France email: [email protected], [email protected], [email protected]
S. Ortolani
Affiliation:
Università di Padova, Dipartimento di Astronomia, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy email: [email protected], [email protected]
*
†Observations collected both at the European Southern Observatory, Paranal, Chile (ESO programmes 71.B-0617 and 73.B-0074) and La Silla, Chile.
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Abstract

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We spectroscopically characterize the Galactic Bulge to infer its star formation timescale, compared to the other Galactic components, through the chemical signature on its individual stars. O, Na, Mg, Al were obtained for 50 K giants in four fields towards the Galactic bulge from UVES spectra (R=45,000), while Fe was measured in more than 400 stars with a slightly low resolution (R=20,000) and the GIRAFFE spectrograph at VLT. Oxygen and Magnesium show a well defined trend with [Fe/H], with abundances larger than those measured in both thin and thick disk stars, supporting a scenario in which the bulge formed before and more rapidly than the disk. On the other hand the iron distribution peaks at solar metallicity and it is slightly narrower than that measured in previous works. Part of the present results have been published by Zoccali et al. (2006) and Lecureur et al. (2006), and part will be discussed in forthcoming papers.

Keywords

Galaxy: bulge – Stars: AbundancesAtmospheres
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S241: Stellar Populations as Building Blocks of Galaxies , December 2006 , pp. 73 - 77
Copyright
Copyright © International Astronomical Union 2007

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