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Stellar populations of local infrared-selected galaxies

Published online by Cambridge University Press:  13 April 2010

X. Y. Chen ,
Y. C. Liang ,
F. Hammer ,
Y. H. Zhao  and
G. H. Zhong
X. Y. Chen
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, Chaoyang District, Beijing 100012, China; email: chenxy@nao.cas.cn; ycliang@nao.cas.cn Graduate School of the Chinese Academy of Sciences, Beijing 100049, China
Y. C. Liang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, Chaoyang District, Beijing 100012, China; email: chenxy@nao.cas.cn; ycliang@nao.cas.cn
F. Hammer
Affiliation:
GEPI, Observatoire de Paris-Meudon, Meudon 92195, France
Y. H. Zhao
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, Chaoyang District, Beijing 100012, China; email: chenxy@nao.cas.cn; ycliang@nao.cas.cn
G. H. Zhong
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, Chaoyang District, Beijing 100012, China; email: chenxy@nao.cas.cn; ycliang@nao.cas.cn Graduate School of the Chinese Academy of Sciences, Beijing 100049, China
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Abstract

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The stellar populations of 849 local infrared-selected galaxies from SDSS and IRAS (including 419 star-forming galaxies, 326 composite galaxies, 35 Seyfert 2s, and 69 LINERs in 4 spectral classes) are studied by using STARLIGHT. Among the 4 spectral classes, the importance of young populations decreases from star-forming, composite, Seyfert 2 to LINER; and Seyfert 2 and LINER are more metal-rich; ULIGs (ultra luminous infrared galaxies) & LIGs present the youngest populations among 3 infrared luminosity bins; and normal galaxies are more metal-rich. The dominant contributors to masses are all old populations.

Keywords

galaxies: evolutiongalaxies: stellar contentinfrared: galaxies
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 313 - 314
Copyright
Copyright © International Astronomical Union 2010

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