Fig. 8
Cluster number overdensity, ΔN, as a function of the halo mass overdensity, ΔM, for pair (grey dots) and richer superclusters (black dots). The best-fit model (solid line) is shown for the CS (upper panel) and the GCS (lower panel). The fitted slope and amplitude for different mass limits for the cluster catalogues are shown in Fig. 9.
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