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Star formation is observed to be suppressed in group and cluster galaxiescompared to the field. To gain insight into the quenching process, we haveanalysed ~2000 galaxies formed in the GIMIC suite of cosmologicalhydrodynamical simulations. The time of quenching varies from ~2 Gyr beforeaccretion (first crossing of r200,c) to >4 Gyr after, depending on satelliteand host mass. Once begun, quenching is rapid (>~ 500 Myr) in low-mass galaxies(M* < 10^10 M_Sun), but significantly more protracted for more massivesatellites. The simulations predict a substantial role of outflows driven byram pressure -- but not tidal forces -- in removing the star-forminginterstellar matter (ISM) from satellite galaxies, especially dwarfs (M* ~ 10^9M_Sun) where they account for nearly two thirds of ISM loss in both groups andclusters. Immediately before quenching is complete, this fraction rises to ~80%even for Milky Way analogues (M* ~ 10^10.5 M_Sun) in groups (M_host ~ 10^13.5M_Sun). We show that (i) ISM stripping was significantly more effective atearly times than at z = 0; (ii) approximately half the gas is stripped from`galactic fountains' and half directly from the star forming disk; (iii)galaxies undergoing stripping experience ram pressure up to ~100 times theaverage at a given group/cluster-centric radius, because they arepreferentially located in overdense ICM regions. Remarkably, stripping causesat most half the loss of the extended gas haloes surrounding our simulatedsatellites. These results contrast sharply with the current picture ofstrangulation -- removal of the ISM through star formation after stripping ofthe hot halo -- being the dominant mechanism quenching group and clustersatellites.

Star formation quenching in simulated group and cluster galaxies: When, how, and why?