The projected mass distribution and the transition to homogeneity

We make a statistical analysis of the angular projection of the large-scale stellar mass distribution, obtained from the Sloan Digital Sky Survey (data release 7) with the stellar masses of galaxies. We obtain a clustering length $r_0= 5.9$--$6.5\,h^{-1}$Mpc and a two-point correlation function power-law exponent $\gamma=1.83$--$1.97$, but we find that the projected stellar mass distribution is not very useful to study strong clustering and, in particular, fractal properties. Taking into account the results of the statistical analysis of volume limited samples from the same data, we conclude that a multifractal cosmic-web model with a transition to homogeneity at about $10\,h^{-1}$Mpc is adequate, but there is a considerable uncertainty in both this scale and the correlation dimension.