The Scaling Relations of Galaxy Clusters and Their Dark Matter Halos

Like early-type galaxies, also nearby galaxy clusters define a Fundamental Plane, a luminosity-radius, and a luminosity-velocity dispersion relations, whose physical origin is still unclear. By means of high resolution N-body simulations of massive dark matter halos in a LCDM cosmology, we find that scaling relations similar to those observed for galaxy clusters are already defined by their dark matter hosts. The slopes however are not the same, and among the various possibilities in principle able to bring the simulated and the observed scaling relations in mutual agreement, we show that the preferred solution is a luminosity dependent mass-to-light ratio (M/L~ L⁰. 3), that well corresponds to what inferred observationally. We then show that at galactic scales there is a conflict between the cosmological predictions of structure formation, the observed trend of the mass-to-light ratio in ellipticals, and the slope of their luminosity-velocity dispersion relation (that significantly differs from the analogous one followed by clusters). The conclusion is that the scaling laws of elliptical galaxies might be the result of the cosmological collapse of density fluctuations at the epoch when galactic scales became non-linear, plus important modifications afterward due to early-time dissipative merging. Finally, we briefly discuss the possible evolution of the cluster scaling relations with redshift.