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Title:
The local mean mass density of the universe - New methods for studying galaxy clustering
Authors:
Davis, M.; Geller, M. J.; Huchra, J.
Affiliation:
AA(Harvard College Observatory and Smithsonian Astrophysical Observatory, Cambridge, Mass.), AB(Harvard College Observatory and Smithsonian Astrophysical Observatory, Cambridge, Mass.), AC(Harvard College Observatory and Smithsonian Astrophysical Observatory, Cambridge, Mass.)
Publication:
Astrophysical Journal, Part 1, vol. 221, Apr. 1, 1978, p. 1-18. (ApJ Homepage)
Publication Date:
04/1978
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
COSMOLOGY, GALACTIC CLUSTERS, MASS DISTRIBUTION, RED SHIFT, SPATIAL DISTRIBUTION, CORRELATION, GALACTIC EVOLUTION, LUMINOSITY, LUMINOUS INTENSITY, UNIVERSE, VELOCITY DISTRIBUTION
Comment:
A&AA ID. AAA021.162.027
DOI:
10.1086/156000
Bibliographic Code:
1978ApJ...221....1D

Abstract

Methods for analyzing redshift catalogs are presented and demonstrated by examining the constraints which currently available data place on the ratio (OmegaG) of the local mean mass density associated with galaxies to the critical density for an Einstein-de Sitter universe. Methods are outlined which are used to estimate OmegaG from a data set that includes nearly complete redshift information for galaxies brighter than a limiting blue magnitude of 13.0. The mean luminosity density is reevaluated and found to be consistent with the result of Gott and Turner (1976) but smaller than the result obtained by Shapiro (1971). Techniques for applying the virial theorem to estimate OmegaG are discussed, two redshift-weighted estimators are computed for the two-point spatial correlation function, and an estimate of the amplitude of that function in a specific power-law model is derived which is almost a factor of 2 smaller than previous estimates. The one-dimensional rms relative peculiar velocity dispersion is estimated to be 300 + or - 30 km/s, practically independent of physical separation. The statistical virial theorems are shown to suggest a value of 0.2 to approximately 0.7 for Omega sub G.

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