Local density maxima - Progenitors of structure

Beginning with a short review of the observational data and of some previous theoretical ideas and numerical simulations, the question is addressed of how the large-scale structure that emerges around local density maxima depends on the nature of the primordial density perturbations field. The density contrast profile around local maxima is given, to a good approximation, by the primordial two-point correlation function. The mean number density of objects of a given core mass is calculated as a function of the primordial power spectrum, p(k). In an open universe, rich clusters should have halos steeper than galactic haloes. The observed structure is found to be consistent with omega-sub-zero less than 1.0 and n = -1.