first interaction that these galaxies experienced with the ICM inducing tidal shocks and then a burst of SF. Actually, the dominant processes that quench SF in galaxies depend crucially on the galaxy mass. Dwarf galaxies, given their shallow potential wells, should be more susceptible to environmental processes such as tidal/ram-pressure stripping [e.g. @BWG09]. Indeed their SF histories are completely defined by their local environment, since passive dEs are only found as satellites within massive halos [i.e. cluster, group or massive galaxy; @Haines06; @Haines07]. The formation of many cluster dEs is often rather recent, manifest by young stellar ages (${\sim}2$Gyr) and the significant populations of starburst and post–starburst dwarf galaxies in the outskirts of local clusters [@SLH09; @MHR11].

Relating star formation quenching to ram-pressure stripping {#RPS}
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Ram-pressure stripping (RPS), as originally proposed by @GG72 requires, in principle, the presence of a dense ICM. Thus, its effect would be limited to cluster cores where the gas discs of massive spirals are rapidly truncated. Nevertheless, with a 3–D hydrodynamical simulation, @MBD03 showed that RPS may extend to poorer environments for low-mass galaxies which, thanks to their lower escape velocities, are easier to strip. @RH05, by means of high resolution 2D hydrodynamical simulations, 