Cosmological density fluctuations and large-scale structure From N-point correlation functions to the probability distribution

Details Cosmological density fluctuations and large-scale structure From N-point correlation functions to the probability distribution Cosmological density fluctuations and large-scale structure From N-point correlation functions to the probability distribution

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...289...10f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 289, Feb. 1, 1985, p. 10-17. NASA-supported research.

Statistics

Computation

90

Computational Astrophysics, Cosmology, Galactic Clusters, Correlation, Density Distribution, Probability Distribution Functions

Scientific paper

Knowledge of N-point correlation functions for all N allows one to invert and obtain the probability distribution of mass fluctuations in a fixed volume. This method is applied to the hierarchical sequence of higher order correlations with dimensionless amplitudes suggested by the BBGKY equations. The resulting distribution is significantly non-Gaussian, even for quite small mean square fluctuations. The qualitative and to some degree quantitative results are to a large degree independent of the exact sequence of amplitudes. An ensemble of such models compared with N-body simulations fails to account for the low-density frequency distribution.

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