Velocity dispersion σ within clusters of a given mass M_200m for a subset of the studied cosmologies at z = 0. The shaded region shows the standard deviation found in our simulations. We note that most systems are virialised, either to the ΛCDM value or the boosted unscreened f(R) equilibrium. Neutrinos do not have any detectable effect on the velocity dispersion inside of clusters, and we just show the case with |f_R0| = 10⁻⁵ and ∑m_ν = 0.15 eV for clarity. The relative deviations are shown separately in Fig. 4.