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Star formation quenching in galaxies

Published online by Cambridge University Press:  17 September 2012

T. Kimm ,
R.S. Somerville ,
S.K. Yi ,
van den Bosch F.C. ,
S. Salim ,
F. Fontonot ,
P. Monaco ,
H.J. Mo ,
A. Pasquali  and
R.M. Rich
...Show all authors
T. Kimm
Affiliation:
Department of Astronomy, Yonsei University, Seoul 120-749, Korea. email: tskim@galaxy.yonsei.ac.kr;
R.S. Somerville
Affiliation:
Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USA Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
S.K. Yi
Affiliation:
Department of Astronomy, Yonsei University, Seoul 120-749, Korea. email: tskim@galaxy.yonsei.ac.kr;
van den Bosch F.C.
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
S. Salim
Affiliation:
National Optical Astronomy Observatory, 950 North Cherry Ave., Tucson, AZ 85719, USA
F. Fontonot
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
P. Monaco
Affiliation:
Dipartimento di Astronomia, Università di Trieste, via Tiepolo 11, 34143 Trieste, Italy INAF-Osservatorio Astronomico, via Tiepolo 11, 34143 Trieste, Italy
H.J. Mo
Affiliation:
Department of Astronomy, University of Massachusetts, Amherst, MA 01003-9305, USA
A. Pasquali
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
R.M. Rich
Affiliation:
Department of Physics and Astronomy, University of California, USA
X. Yang
Affiliation:
Shanghai Astronomical Observatory, China
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Abstract

We investigate the correlation of star formation quenching with internal galaxy properties and environment by comparing observation and theoretical models. We first classify galaxies as the most massive “central” or “satellite” in each halo in order to investigate the environmental effect. For observed central galaxies, we are unable to determine whether star formation quenching is primarily connected with halo mass or stellar mass, because these two quantities are strongly correlated. For satellite galaxies, a nearly equal dependence on halo mass and stellar mass is seen. We find that theoretical models with AGN feedback reproduce the dependence on colours and specific star formation rates for central galaxies reasonably. However, the same models seriously fail to reproduce the star formation rates of satellite galaxies by over-quenching star formation via strong strangulation: satellite over-quenching problem.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 56: The Role of the Disk-Halo Interaction in Galaxy Evolution: Outflow vs. Infall? , 2012 , pp. 167 - 170
Copyright
© EAS, EDP Sciences, 2012

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