Cluster temperature function normalization ($k_{B}T\propto M^{2/3}[{\Delta }_v{\rho }_c(z){]}^{1/3}$)

The virial theorem and hydrostatic equilibrium relate a cluster's gas temperature to $GM/R$, while $M=(4\pi /3){\Delta }_v{\rho }_c{R}^3$. A calibrated mass-temperature relation converts the Press-Schechter halo mass function into $dn/dT=(dn/dM)|dM/dT|$. Its exponential rare-cluster tail is sensitive to the density contrast variance on cluster scales, hence to the power-spectrum amplitude, often parameterized by ${\sigma }_8$. Mass calibration, temperature scatter, nonthermal pressure, sample selection and the matter density must be included rather than treating temperature counts as an independent measurement of amplitude alone.