SEEDED HOT DARK MATTER MODELS FOR LARGE-SCALE STRUCTURE

We examine a class of models in which the universe is dominated by hot dark matter and density perturbations are generated by randomly distributed relic seed masses, such as primordial black holes or nontopological solitons. For h = 1/2 and omega-b = 0.08, the seed mass m(s) and number density n(s) are chosen to satisfy m(s)2n(2) = 7 x 10(16) M2. Mpc-3, in order to produce a pairwise radial velocity dispersion of 300 km s-1 on scales of a few Mpc. With this choice of m(s)2n(s), the two-point galaxy correlation function is zeta(r) = (r/r(o))-1.8, with r(o) = 5h-1 Mpc. This model produces galaxies much earlier than standard hot dark matter, and the high redshift galaxies are strongly clustered. The evolved density distribution is characterized by a smooth distribution of matter in the low-density void regions. These results are independent of n(s) over the regime we have examined. There is no correlation between the number of seed masses and the number of galaxies. The cleanest test of this model is the prediction that high-redshift galaxies will be strongly clustered.