TY - JOUR
T1 - Dependence of galaxy quenching on halo mass and distance from its centre
AU - Woo, Joanna
AU - Dekel, Avishai
AU - Faber, S. M.
AU - Noeske, Kai
AU - Koo, David C.
AU - Gerke, Brian F.
AU - Cooper, Michael C.
AU - Salim, Samir
AU - Dutton, Aaron A.
AU - Newman, Jeffrey
AU - Weiner, Benjamin J.
AU - Bundy, Kevin
AU - Willmer, Christopher N.A.
AU - Davi, Marc
AU - Yan, Renbin
PY - 2013/2/1
Y1 - 2013/2/1
N2 - We study the dependence of star formation quenching on galaxy mass and environment, in the Sloan Digital Sky Survey (SDSS; z ~ 0.1) and the All-Wavelength Extended Groth Strip International Survey (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 dN 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 per cent) and the haloes are less massive. For satellites, M*-dependent quenching is noticeable at high D, suggesting a quenching dependence on subhalo 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 dN 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.
AB - We study the dependence of star formation quenching on galaxy mass and environment, in the Sloan Digital Sky Survey (SDSS; z ~ 0.1) and the All-Wavelength Extended Groth Strip International Survey (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 dN 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 per cent) and the haloes are less massive. For satellites, M*-dependent quenching is noticeable at high D, suggesting a quenching dependence on subhalo 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 dN 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.
KW - Galaxies: evolution
KW - Galaxies: groups: general
KW - Galaxies: haloes
KW - Galaxies: star formation
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U2 - 10.1093/mnras/sts274
DO - 10.1093/mnras/sts274
M3 - Article
AN - SCOPUS:84873727569
SN - 0035-8711
VL - 428
SP - 3306
EP - 3326
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -