I show that the correlation function on small scales measures the galaxy distribution within dark-matter halos in the HOD model of galaxy clustering. My measurements of the LRG auto-correlation function imply that the inner slope of the radial profile where the density of the galaxies n goes like r-tau, has tau = 2. This is much steeper than the results found by the N-body simulations for dark matter alone (tauNFW = 1). This result suggest that either the galaxies do not follow the dark matter distribution on all scales or that the baryons substantially change the dark matter profile in the very inner parts of the halos.In this picture, the first transition at about 2 Mpc is basically the size of the largest halos that host LRGs or simply the size ... This scale is close to the radial size of the smallest halo that can host an LRG plus the size of the smallest halo that can anbsp;...
|Title||:||Massive Galaxy Merging and Cosmogony|
|Publisher||:||ProQuest - 2007|