The Correlation Strength of Clusters in the Cosmic String Model
It is known that the two-point correlation functions of galaxies and of clusters of galaxies have three systematic characteristics. 1. all correlation functions have power laws with approximately the same index −1.8. i.e. ξ(r)=αr−1.8; 2. the correlation strength α increases with the increase of the mean separations d of the systems considered and 3. α also increases with the increase of the mean richness of the systems (the Bahcall-Soneira relation).
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