The kinematics of dense clusters of galaxies. 3: Comparison with cosmological models

Details The kinematics of dense clusters of galaxies. 3: Comparison with cosmological models The kinematics of dense clusters of galaxies. 3: Comparison with cosmological models

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aj....107.1929z&link_type=abstract

The Astronomical Journal (ISSN 0004-6256), vol. 107, no. 6, p. 1929-1936

Astronomy and Astrophysics

Astronomy

8

Astronomical Models, Galactic Clusters, Red Shift, Spiral Galaxies, Star Distribution, Dark Matter, Galactic Evolution, Galactic Structure, Mass Distribution

Scientific paper

We compare the combined distribution of 31 group and 25 cluster velocity dispersions with the ensemble of 32 models for the formation and evolution of large-scale structure examined by Weinberg & Cole (1992). The models include Gaussian and non-Gaussian initial fluctuations, different power law spectra (n = -1, n = 0, n = -2, 'pancake'), flat (Omega = 1) and open (Omega = 0.2) cosmologies, and unbiased (b8 = 1) and biased (b8 = 2) galaxy formation. The set of initial conditions we test, although limited, samples enough parameter space to indicate which general classes of models are consistent with the data. The two Gaussian, n = -1 models which best approximate the standard and open Cold Dark Matter (CDM) models do not match the observed distribution of velocity dispersions; models with b8 = 2 and Omega = 1 ('standard') or b8 = 1 and Omega = 0.2 ('open') predict too large a ratio of low to high velocity dispersion systems. A 'COBE-normalized' CDM model with b8 = 1 and Omega = 1 produces clusters with velocity dispersions higher than those measured. All three models overestimate the total abundance of systems.

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