Local density maxima - Progenitors of structure

Details Local density maxima - Progenitors of structure Local density maxima - Progenitors of structure

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...297...16h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 297, Oct. 1, 1985, p. 16-22.

Statistics

Computation

197

Astronomical Models, Density Distribution, Galactic Evolution, Galactic Structure, Maxima, Computational Astrophysics, Cosmology, Universe

Scientific paper

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.

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