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Population synthesis from clustered star formation

Published online by Cambridge University Press:  13 April 2010

M. R. Haas  and
P. Anders
M. R. Haas
Affiliation:
Leiden Observatory, Leiden University, Postbus 9513, NL-2300RA, Leiden, the Netherlands email: haas@strw.leidenuniv.nl
P. Anders
Affiliation:
Sterrenkundig Instituut, University of Utrecht, email: p.anders@uu.nl
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In recent years, a series of papers (Kroupa & Weidner 2003, Weidner & Kroupa 2004, Weidner & Kroupa 2005 and Weidner & Kroupa 2006, WK06 from now on) have proposed that the stellar content of an entire galaxy may not be well described by the same initial mass function (IMF) that describes the distribution of stellar masses in the star clusters, where these stars form. The reason is that star clusters also form with a cluster mass function (CMF), which is a power law with a power law index of ~−2. If the lowest mass clusters are of masses smaller than the physical upper mass limit for stars they will be deficient in high mass stars. Therefore, if the stellar content of all clusters is added together, making up the Integrated Galactic Initial Mass Function (IGIMF), the distribution of stellar masses may be steeper at the high mass end, depending on the exact shape of the CMF.

Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 347 - 348
Copyright
Copyright © International Astronomical Union 2010

References

Bicker, J., Fritze-v. Alvensleben, U., Möller, C. S., & Fricke, K. J. 2004, A&A, 413, 37Google Scholar
Goodwin, S. P. & Pagel, B. E. J. 2005, MNRAS, 359, 707Google Scholar
Haas, M. R. & Anders, P. 2009, A&A, submittedGoogle Scholar
Kotulla, R., Fritze, U., Weilbacher, P., & Anders, P. 2009, MNRAS, 396, 462Google Scholar
Kroupa, P. 2001, MNRAS, 322, 231Google Scholar
Kroupa, P. & Weidner, C 2003, ApJ, 598, 1076Google Scholar
Paturel, G., Petit, C., Prugniel, P., Theureau, G., Rousseau, J., Brouty, M., Dubois, P., & Cambrésy, L. 2003, A&A, 412, 45Google Scholar
Pflamm-Altenburg, J. & Kroupa, P. 2008, Nature, 455, 641CrossRefGoogle Scholar
Recchi, S., Calura, F., & Kroupa, P. 2009, A&A, 499, 711Google Scholar
Salpeter, E. E. 1955, ApJ, 121, 161Google Scholar
Weidner, C. & Kroupa, P. 2004, MNRAS, 348, 187CrossRefGoogle Scholar
Weidner, C. & Kroupa, P. 2005, ApJ, 625, 754Google Scholar
Weidner, C. & Kroupa, P. 2006, MNRAS, 365, 1333Google Scholar