The scale of galaxy clustering and the mean matter density of the universe

Details The scale of galaxy clustering and the mean matter density of the universe The scale of galaxy clustering and the mean matter density of the universe

Aug 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975mnras.172p..23f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 172, Aug. 1975, p. 23p-26p.

Astronomy and Astrophysics

Astronomy

23

Astronomical Models, Cosmology, Density Distribution, Galactic Clusters, Universe, Correlation, Covariance, Galactic Evolution, Gravitational Effects

Scientific paper

The correlation energy computed from Peebles' (1974) power-law galaxy covariance function suggests that if the gravitational instability picture is correct, there must be a feature in the covariance function where it steepens. The scale of this cut-off cannot be accurately determined by this argument, but a comparison of the random kinetic energies of galaxies with their correlation energy gives an estimate of the mean matter density of the universe. The suggested value is less than 5 per cent of the closure density if most matter is distributed in the same way as galaxies.

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