Too dense to go through: the role of low-mass clusters in the pre-processing of satellite galaxies

ABSTRACT We study the evolution of satellite galaxies in clusters c-eagle simulations, a suite 30 high-resolution cosmological hydrodynamical zoom-in simulations based on eagle code. find that majority are quenched at z = 0 (?80${{\ \rm per\ cent}}$) reached this state dense environment (log10M200[M?] ?13.5). At low redshift, regardless final cluster mass, appear to reach their quenching low-mass clusters. Moreover, inside they reside dominant population clusters, while different halo dominate most massive When looking > 0.5, situ dominates all masses. This suggests first fall into. After cross cluster’s r200 rapidly become (?1 Gyr). Just small fraction ($\lesssim 15{{\ is capable retaining gas for longer period time, but after 4 Gyr, almost quenched. phenomenon related ram pressure stripping and produced when density intracluster medium reaches threshold $\rho _{\rm ICM}\, \sim 3 \times 10 ^{-5}$ nH (cm?3). These results suggest start rapid-quenching phase shortly infall that, by time r500, them already