%0 Journal Article
%T Dependence of Galaxy Quenching on Halo Mass and Distance from its Centre
%A Joanna Woo
%A Avishai Dekel
%A S. M. Faber
%A Kai Noeske
%A David C. Koo
%A Brian F. Gerke
%A Michael C. Cooper
%A Samir Salim
%A Aaron A. Dutton
%A Jeffrey Newman
%A Benjamin J. Weiner
%A Kevin Bundy
%A Christopher N. A. Willmer
%A Marc Davis
%A Renbin Yan
%J Physics
%D 2012
%I arXiv
%R 10.1093/mnras/sts274
%X We study the dependence of star-formation quenching on galaxy mass and environment, in the SDSS (z~0.1) and the AEGIS (z~1). It is crucial that we define quenching by low star-formation rate rather than by red colour, given that one third of the red galaxies are star forming. We address stellar mass M*, halo mass Mh, density over the nearest N neighbours deltaN, and distance to the halo centre D. The fraction of quenched galaxies appears more strongly correlated with Mh at fixed M* than with M* at fixed Mh, while for satellites quenching also depends on D. We present the M*-Mh relation for centrals at z~1. At z~1, the dependence of quenching on M* at fixed Mh is somewhat more pronounced than at z~0, but the quenched fraction is low (10%) and the haloes are less massive. For satellites, M*-dependent quenching is noticeable at high D, suggesting a quenching dependence on sub-halo mass for recently captured satellites. At small D, where satellites likely fell in more than a few Gyr ago, quenching strongly depends on Mh, and not on M*. The Mh-dependence of quenching is consistent with theoretical wisdom where virial shock heating in massive haloes shuts down accretion and triggers ram-pressure stripping, causing quenching. The interpretation of deltaN is complicated by the fact that it depends on the number of observed group members compared to N, motivating the use of D as a better measure of local environment.
%U http://arxiv.org/abs/1203.1625v2