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This work is focused on the study of the distribution in the CPPS of passiveand star-forming galaxy populations and also, the intense and quiescentstar-forming populations for a set of 9 nearby z<0.05 galaxy clusters.Furthermore, we compare the CPPS distribution of the passive galaxy populationwith the accreted halo population of a set of 28 simulated clusters and thestar-forming population with the non-accreted population. We consider variouscluster accretion epochs and accretion radii where it is assumed that starformation in galaxies becomes quenched, in order to segregate the accretedpopulation from the non-accreted population. Just applying this segregation insimulations, we get a qualitative agreement between the CPPS distributions ofthe passive and the accreted populations and also between the star-forming andthe non-accreted populations. The uncertainty in cluster centering stronglyaffects the pronounced cuspy profiles of the projected density and also, it canexplain the main difference (i.e. inner slope) between the CPPS distribution ofpassive and accreted populations. The CPPS density of star-forming galaxies andthe intensity of ram-pressure stripping present an opposite trend throughoutthe CPPS. This implies that ram-pressure stripping significantly contributes tomodulate the observed CPPS distribution of star-forming galaxies inside andaround cluster virial regions. The significant fraction of star-forminggalaxies at the projected center of clusters are mainly those galaxies with lowl-o-s velocities and they can be mainly identified as those galaxies with aremaining star formation activity (quiescent star-forming galaxies) inside thephysical virial region or, in a lower degree, as galaxy interlopers i.e.outside the physical virial region.(abridged)

Star formation activity and gas stripping in the Cluster Projected Phase-Space (CPPS)