We discuss the properties of galaxy clusters expected in a texture-seeded, CDM-dominated, Ω = 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 1011 to 1015 M⊙, we find v ∝ Mγ with γ ≃ 0.25. An unbiased (b = 1) texture model predicts too many high-velocity dispersion clusters. A biased texture model (b ∼ 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 ≈ 1-2).
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
- Cosmology: theory
- Dark matter
- Galaxies: clustering
- Large-scale structure of universe