Textures and Clusters
Abstract
We discuss the properties of galaxy clusters expected in a texture seeded, CDMdominated, {OMEGA} = 1 universe. Assuming that the textures are spherical, we use the spherical collapse model to compute the cluster velocity dispersion (or temperature) distribution function. For objects of mass 10^11^ to 10^15^ M_sun_ we find v is proportional to M^{gamma} with γ ~ 0.25. An unbiased (b = 1) texture model predicts too many highvelocity dispersion clusters. A biased texture model (b~34) appears to be compatible with cluster properties inferred from optical and Xray observations. In the texture model, the cluster velocity distribution function does not evolve rapidly; thus, the model predicts the existence of rich clusters at moderate redshift (z ~ 12).
 Publication:

The Astrophysical Journal
 Pub Date:
 January 1993
 DOI:
 10.1086/172175
 Bibcode:
 1993ApJ...403....1B
 Keywords:

 Astronomical Models;
 Dark Matter;
 Galactic Clusters;
 Universe;
 Computational Astrophysics;
 Gravitational Collapse;
 Red Shift;
 Astrophysics;
 COSMOLOGY: THEORY;
 COSMOLOGY: DARK MATTER;
 GALAXIES: CLUSTERING;
 COSMOLOGY: LARGESCALE STRUCTURE OF UNIVERSE