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We study the dependence of star-formation quenching on galaxy mass andenvironment, in the SDSS (z~0.1) and the AEGIS (z~1). It is crucial that wedefine quenching by low star-formation rate rather than by red colour, giventhat one third of the red galaxies are star forming. We address stellar massM*, halo mass Mh, density over the nearest N neighbours deltaN, and distance tothe halo centre D. The fraction of quenched galaxies appears more stronglycorrelated with Mh at fixed M* than with M* at fixed Mh, while for satellitesquenching 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 morepronounced than at z~0, but the quenched fraction is low (10%) and the haloesare less massive. For satellites, M*-dependent quenching is noticeable at highD, suggesting a quenching dependence on sub-halo mass for recently capturedsatellites. At small D, where satellites likely fell in more than a few Gyrago, quenching strongly depends on Mh, and not on M*. The Mh-dependence ofquenching is consistent with theoretical wisdom where virial shock heating inmassive haloes shuts down accretion and triggers ram-pressure stripping,causing quenching. The interpretation of deltaN is complicated by the fact thatit depends on the number of observed group members compared to N, motivatingthe use of D as a better measure of local environment.

Dependence of Galaxy Quenching on Halo Mass and Distance from its Centre