Key points are not available for this paper at this time.
The abundance of rich clusters is a strong constraint on the mass power spectrum. The current constraint can be expressed in the form σ₈ Ωₘ^γ = 0. 5 0. 1 where σ₈ is the rms mass fluctuation on 8 h^-1 Mpc scales, Ωₘ is the ratio of matter density to the critical density, and γ is model-dependent. In this paper, we determine a general expression for γ that applies to any models with a mixture of cold dark matter plus cosmological constant or quintessence (a time-evolving, spatially-inhomogeneous component with negative pressure) including dependence on the spectral index n, the Hubble constant h, and the equation-of-state of the quintessence component w. The cluster constraint is combined with COBE measurements to identify a spectrum of best-fitting models. The constraint from the evolution of rich clusters is also discussed.
Wang et al. (Thu,) studied this question.