  The Planck Collaboration has shown that the number of clusters as a function
of their mass and redshift is an extremely powerful tool for cosmological
analyses. However, the true cluster mass is not directly measurable. Among the
possible approaches, clusters mass could be related to different observables
via self similar scaling law. These observables are related to the baryonic
components of which a cluster is composed. However, the theoretical relations
that allow the use of these proxies often are affected by observational and
physical biases, which impacts on the determination of the cluster mass.
Fortunately, cosmological simulations are an extremely powerful tool to assess
these problems. We present our calibration of the scaling relation between mass
and velocity dispersion of galaxy members from the study of the simulated
clusters of \THP{} project with mass above $10^{13} M_\odot$. In order to
investigate the presence of a redshift dependence, we analyzed 16 different
redshifts between $z = 0$ and $z = 2$. Finally, we investigated the impact of
different AGN feedback models.
