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Stellar parameters in the bulge cluster NGC 6553

Published online by Cambridge University Press:  25 May 2016

B. Barbuy ,
S. Ortolani ,
E. Bica ,
A. Renzini  and
M.D. Guarnieri
B. Barbuy
Affiliation:
University of Sao Paulo, CP 9638, Sao Paulo 01065-970, Brazil
S. Ortolani
Affiliation:
University of Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
E. Bica
Affiliation:
University of Rio Grande do Sul, CP 15051, Porto Alegre 91500-970, Brazil
A. Renzini
Affiliation:
European Southern Observatory, Karl-Schwarzschild Str. 2, D-85748 Garching bei München, Germany
M.D. Guarnieri
Affiliation:
European Southern Observatory, Karl-Schwarzschild Str. 2, D-85748 Garching bei München, Germany

Extract

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Globular clusters in the Galactic bulge form a flattened system, extending from the Galactic center to about 4.5 kpc from the Sun (Barbuy et al. 1997). A study of abundance ratios in these clusters is very important for a more complete understanding of the bulge formation. In this work we present a spectroscopic analysis of individual stars in NGC 6553. This cluster is a key one because it is located at d⊙ ≍ 5.1 kpc, therefore relatively close to us, and at the same time it is representative of the Galactic bulge stellar population: (a) Ortolani et al. (1995) showed that NGC 6553 and NGC 6528 show very similar Colour-Magnitude Diagrams (CMDs), and NGC 6528 is located at d⊙ ≍ 7.83 kpc, very close to the Galactic center; (b) the stellar populations of the Baade Window is also very similar to that of NGC 6553 and NGC 6528 as Ortolani et al. (1995) have shown by comparing their luminosity functions.

Type
Stellar Abundances
Information
Symposium - International Astronomical Union , Volume 189: Fundamental Stellar Properties: The Interaction Between Observation and Theory , 1997 , pp. 203 - 206
Copyright
Copyright © Kluwer 1997 

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