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Observations of clusters with ages from 0.01 to 1.0 Gyr in the Large Magellanic Cloud

Published online by Cambridge University Press:  01 April 2008

Q. Liu ,
R. de Grijs ,
L. C. Deng ,
Y. Hu  and
I. Baraffe
Q. Liu
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, P. R. China email: liuq@bao.ac.cn Graduate University of ChineseAcademy of Sciences, Beijing, 100049, P. R. China
R. de Grijs
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, P. R. China email: liuq@bao.ac.cn Department of Physics & Astronomy, The University of Sheffield, Sheffield S3 7RH, UK
L. C. Deng
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, P. R. China email: liuq@bao.ac.cn
Y. Hu
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, P. R. China email: liuq@bao.ac.cn Graduate University of ChineseAcademy of Sciences, Beijing, 100049, P. R. China
I. Baraffe
Affiliation:
CRAL, École Normale Supérieure, 46 allée d'Italie, 69007 Lyon, France
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Abstract

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The stellar initial mass function (IMF) is a very important question in modern astrophysics. Globular clusters (GCs) are good samples for studying the IMF, but the Galactic GCs can provide only one time-scale evolutionary stage. The Large Magellanic Cloud (LMC) is an ideal environment for studying the IMF because it contains compact clusters at different evolutionary stages. By studying the IMF at different evolutionary stages, we can see how the mass function evolves with time.

Keywords

Stars: mass functionLarge Magellanic Cloudgalaxy: star clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 121 - 122
Copyright
Copyright © International Astronomical Union 2008

References

Baraffe, I., Chabrier, G., Allard, F., & Hauschildt, P. H. 1998, A&A 337, 403Google Scholar
de Grijs, R., Gilmore, G. F., Johnson, R. A., & Mackey, A. D 2002, MNRAS 331, 245CrossRefGoogle Scholar
Girardi, L., Bressan, A., Bertelli, G., & Chiosi, C. 2000, A&As 141, 371Google Scholar
Holtzman, J. A., Burrows, C. J., Casertano, S., Hester, J. J., Trauger, J. T., Watson, A. M., & Worthey, G. 1995, PASP 107, 1065CrossRefGoogle Scholar
Paresce, F. & De Marchi, G. 2000, ApJ 534, 870Google Scholar
Salpeter, E. E. 1955, AJ 101, 1865Google Scholar