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Satellite galaxies in groups and clusters are more likely to have low starformation rates (SFR) and lie on the red-sequence than central (field)galaxies. Using galaxy group/cluster catalogs from SDSS DR7, together with acosmological N-body simulation to track satellite orbits, we examine the starformation histories and quenching timescales of satellites of M_star > 5 x 10^9M_sun at z=0. We first explore satellite infall histories: group preprocessingand ejected orbits are critical aspects of satellite evolution, and properlyaccounting for these, satellite infall typically occurred at z~0.5, or ~5 Gyrago. To obtain accurate initial conditions for the SFRs of satellites at theirtime of first infall, we construct an empirical parametrization for theevolution of central galaxy SFRs and quiescent fractions. With this, weconstrain the importance and efficiency of satellite quenching as a function ofsatellite and host halo mass, finding that satellite quenching is the dominantprocess for building up all quiescent galaxies at M_star < 10^10 M_sun. We thenconstrain satellite star formation histories, finding a 'delayed-then-rapid'quenching scenario: satellite SFRs evolve unaffected for 2-4 Gyr after infall,after which star formation quenches rapidly, with an e-folding time of < 0.8Gyr. These quenching timescales are shorter for more massive satellites but donot depend on host halo mass: the observed increase in satellite quiescentfraction with halo mass arises simply because of satellites quenching in alower mass group prior to infall (group preprocessing), which is responsiblefor up to half of quenched satellites in massive clusters. Because of the longtime delay before quenching starts, satellites experience significant stellarmass growth after infall, nearly identical to central galaxies. This factprovides key physical insight into the subhalo abundance matching method.

Galaxy evolution in groups and clusters: satellite star formation histories and quenching timescales in a hierarchical Universe