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Comparing six evolutionary population synthesis models

Published online by Cambridge University Press:  13 April 2010

Y. C. Liang ,
X. Y. Chen ,
F. Hammer ,
M. Rodrigues ,
Y. H. Zhao  and
G. H. Zhong
Y. C. Liang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, A 20 Datun Road Chaoyang District, Beijing 100012, China; email: ycliang@nao.cas.cn
X. Y. Chen
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, A 20 Datun Road Chaoyang District, Beijing 100012, China; email: ycliang@nao.cas.cn Graduate School of the Chinese Academy of Sciences, Beijing 100049, China
F. Hammer
Affiliation:
GEPI, Observatoire de Paris-Meudon, 92195, MeudonFrance
M. Rodrigues
Affiliation:
GEPI, Observatoire de Paris-Meudon, 92195, MeudonFrance
Y. H. Zhao
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, A 20 Datun Road Chaoyang District, Beijing 100012, China; email: ycliang@nao.cas.cn
G. H. Zhong
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, A 20 Datun Road Chaoyang District, Beijing 100012, China; email: ycliang@nao.cas.cn Graduate School of the Chinese Academy of Sciences, Beijing 100049, China
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Abstract

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We compare six evolutionary population synthesis (EPS) models, which have been popularly used in stellar populations analyses for galaxies. The resulted stellar populations of star-forming galaxies and E+A galaxies from these EPS models show that the dominated contribution (fraction) from young, intermediate and old populations to their lights are consistent, although the individual numbers may change significantly, 3-30%, which could relate to the different ingredients in EPS models, such as the stellar library, the stellar evolution tracks etc.

Keywords

galaxies: abundancesgalaxies: evolutiongalaxies: spiralgalaxies: stellar content
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 372 - 373
Copyright
Copyright © International Astronomical Union 2010

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