Evolution of galaxy clustering

We show that the galaxy correlation function does not evolve in proportion with the correlation function of the underlying mass distribution. Earliest galaxies cluster very strongly and the amplitude of the galaxy correlation function decreases from this large value. This continues till the average peaks have collapsed, after which, the galaxy correlation function does not evolve very strongly. 1 The Halo Grail We begin by addressing the simpler problem of halo correlation. In later sections we will test the model presented here using N-Body simulations. Lastly, we will comment on applying the results for halo clustering to galaxy clustering and discuss some of its implications. Consider the distribution of halos of mass M, before typical halos of this mass have collapsed. To quantify this, we first define a bias parameter ν(M) = δc/σ(M), where σ(M) is the (linearly extrapolated) rms dispersion in density at mass scale M and δc = 1.68 is the linearly extrapolated density contrast at which halos are expected to virialise. We can write the linear correlation