  We discuss some of the basic implications of recent results on galaxy
correlations published by the SDSS collaboration. In particular we focus on the
evidence which has been recently presented for the scale and nature of the
transition to homogeneity in the galaxy distribution, and results which
describe the dependence of clustering on luminosity. The two questions are in
fact strictly entangled, as the stability of the measure of the amplitude of
the correlation function depends on the scale at which the mean density becomes
well defined. We note that the recent results which indicate the convergence to
well defined homogeneity in a volume equivalent to that of a sphere of radius
70 Mpc/h, place in doubt previous detections of ``luminosity bias'' from
measures of the amplitude of the correlation function. We emphasize that the
way to resolve these issues is to first use, in volume limited samples
corresponding to different ranges of luminosity, the unnormalized two point
statistics to establish the scale (and value) at which the mean density becomes
well defined. We note also that the recent SDSS results for these statistics
are in good agreement with those obtained by us through analyses of many
previous samples, confirming in particular that the galaxy distribution is well
described by a fractal dimension D ~ 2 up to a scale of at least 20 Mpc/h. We
discuss critically the agreement of this new data with current theoretical
models.
