Radial distribution of nearby (satellite) galaxies, from the centers of TNG-Cluster halos at z = 0. We show the surface number density, that is, the number of galaxies per Mpc², as a function of distance. We stack around clusters in five halo mass bins, as indicated in the legend for M_200c in log M_⊙. We include galaxies with M_r < −20.5 mag (thick solid lines including dust modeling, dotted lines without; see text) in order to match observational constraints from SDSS (Budzynski et al. 2012, black circles and dashed lines;). We also compare to data from GAMA (black squares and dot-dash line; Riggs et al. 2022). In addition we include stellar mass based constraints with three additional sets of dashed colored lines: M_⋆ > {10⁹, 10^10.5, 10^11.5} M_⊙. The first (highest) set of colored curves are comparable to observational constraints from van der Burg et al. (2015, as described in the text).