Galaxy Clusters in Cosmology: Cluster Abundance as a Probe of Structure Formation

In gaussian theories of structure formation, the galaxy cluster abundance is an extremely sensitive probe of the density fluctuation power spectrum and of the density parameter, $\mathrm{\Omega }$. We develop this theme by deriving and studying in detail the mass function of collapsed objects and its relation to these quantities. Application to current data yields constraints which are degenerate between the amplitude of the perturbations and the density parameter; we nevertheless obtain an important limit on the present day mass perturbation amplitude as a function of $\mathrm{\Omega }$ and can rule-out the `standard’ cold dark matter (CDM) model. Future observations of the evolution of the cluster abundance will break the degeneracy and provide important constraints on both the power spectrum and the density parameter, individually. We focus primarily on X-ray clusters in the discussion, and finish with a presentation of the promising new field of Sunyaev-Zel’dovich observations of cluster evolution.