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Title:
Galaxy Groups in the SDSS DR4. III. The Luminosity and Stellar Mass Functions
Authors:
Yang, Xiaohu; Mo, H. J.; van den Bosch, Frank C.
Affiliation:
AA(Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, the Partner Group of MPA, Nandan Road 80, Shanghai 200030, China ), AB(Department of Astronomy, University of Massachusetts, Amherst, MA 01003-9305, USA ), AC(Max-Planck-Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany)
Publication:
The Astrophysical Journal, Volume 695, Issue 2, pp. 900-916 (2009). (ApJ Homepage)
Publication Date:
04/2009
Origin:
IOP
ApJ Keywords:
dark matter, galaxies: halos, large-scale structure of universe, methods: statistical
DOI:
10.1088/0004-637X/695/2/900
Bibliographic Code:
2009ApJ...695..900Y

Abstract

Using a large galaxy group catalog constructed from the Sloan Digital Sky Survey Data Release 4 (SDSS DR4) with an adaptive halo-based group finder, we investigate the luminosity and stellar mass functions for different populations of galaxies (central versus satellite, red versus blue, and galaxies in groups of different masses) and for groups themselves. The conditional stellar mass function (CSMF), which describes the stellar distribution of galaxies in halos of a given mass for central and satellite galaxies can be well modeled with a log-normal distribution and a modified Schechter form, respectively. On average, there are about three times as many central galaxies as satellites. Among the satellite population, there are in general more red galaxies than blue ones. For the central population, the luminosity function is dominated by red galaxies at the massive end, and by blue galaxies at the low-mass end. At the very low mass end (M * lsim 109 h -2 M sun), however, there is a marked increase in the number of red centrals. We speculate that these galaxies are located close to large halos so that their star formation is truncated by the large-scale environments. The stellar mass function of galaxy groups is well described by a double power law, with a characteristic stellar mass at ~4 × 1010 h -2 M sun. Finally, we use the observed stellar mass function of central galaxies to constrain the stellar mass-halo mass relation for low-mass halos, and obtain M *,c vprop M 4.9 h for Mh Lt 1011 h -1 M sun.
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