The statistical nature of the galaxy distribution is in a sense remarkably simple. the two-point correlation function ξ(r), which measures the count of galaxies at separation r in excess of that expected for a random distribution, varies as ξ∝;r−1.8 for ξ>1(r ≲15 Mpc). At larger separations ξ apparently decreases more rapidly. the power law behavior is observed in different galaxy catalogs of varying depth and positions in the sky. What is the explanation of this universal behavior of ξ(r), and what do correlation functions tell us about the initial conditions at the recombination epoch and/or the value of Ω?