The correlation function for density perturbations in an expanding universe. IV - The evolution of the correlation function

Details The correlation function for density perturbations in an expanding universe. IV - The evolution of the correlation function The correlation function for density perturbations in an expanding universe. IV - The evolution of the correlation function

Apr 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...229...14m&link_type=abstract

Astrophysical Journal, Part 1, vol. 229, Apr. 1, 1979, p. 14-24.

Mathematics

Logic

1

Big Bang Cosmology, Correlation, Density Distribution, Galactic Clusters, Perturbation Theory, Spatial Distribution, Boundary Value Problems, Graphs (Charts), Virial Theorem

Scientific paper

The evolution of the two-point correlation function for the large-scale distribution of galaxies in an expanding universe is studied on the assumption that the perturbation densities lie in a Gaussian distribution centered on any given mass scale. The perturbations are evolved according to the Friedmann equation, and the correlation function for the resulting distribution of perturbations at the present epoch is calculated. It is found that: (1) the computed correlation function gives a satisfactory fit to the observed function in cosmological models with a density parameter (Omega) of approximately unity, provided that a certain free parameter is suitably adjusted; (2) the power-law slope in the nonlinear regime reflects the initial fluctuation spectrum, provided that the density profile of individual perturbations declines more rapidly than the -2.4 power of distance; and (3) both positive and negative contributions to the correlation function are predicted for cosmological models with Omega less than unity.

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