TEXTURES AND CLUSTERS

We discuss the properties of galaxy clusters expected in a texture-seeded, CDM-dominated, 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., we find v is-proportional-to M(gamma) with gamma congruent-to 0.25. An unbiased (b = 1) texture model predicts too many high-velocity dispersion clusters. A biased texture model (b approximately 3-4) appears to be compatible with cluster properties inferred from optical and X-ray 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 almost-equal-to 1-2).