We analyze high resolution, N-body hydrodynamical simulations of fiducialgalaxy clusters to probe tidal stripping of the dark matter subhalos. Thesesimulations include a prescription for star formation allowing us to track thefate of the stellar component as well. We investigate the effect of tidalstripping on cluster galaxies hosted in these dark matter subhalos as afunction of cluster-centric radius. To quantify the extent of the dark matterhalos of cluster galaxies, we introduce the half mass radius r_half as adiagnostic, and study its evolution with projected cluster-centric distance Ras a function of redshift. We find a well defined trend for (r_half,R): thecloser the galaxies are to the center of the cluster, the smaller the half massradius. Interestingly, this trend is inferred in all redshift frames examinedin this work ranging from z=0 to z=0.7. At z=0, galaxy halos in the centralregions of clusters are found to be highly truncated, with the most compacthalf mass radius of 10 kpc. We also find that r_half depends on luminosity andwe present scaling relations of r_half with galaxy luminosity. Thecorresponding total mass of the cluster galaxies is also found to increase withprojected cluster-centric distance and luminosity, but with more scatter thanthe (r_half,R) trend. Comparing the distribution of stellar mass to total massfor cluster galaxies, we find that the dark matter component is preferentiallystripped, whereas the stellar component remains protected by the halo and ismuch less affected by tidal forces. We compare these results with galaxy-galaxylensing probes of r_half and find qualitative agreement. (Abridged)
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