CLASH-VLT: The variance in the velocity anisotropy profiles of galaxy clusters

Context. The velocity anisotropy profiles, β(r), of galaxy clusters are directly related to the shape of the orbits of their member galaxies. Knowledge of β(r) is important in order to understand the assembly process of clusters and the evolutionary processes of their galaxies, and to improve the determination of cluster masses based on cluster kinematics. Aims. We determined the β(r) of nine massive clusters at redshift 0.19 ≤ z ≤ 0.45 from the CLASH-VLT dataset, with ≃150–950 spectroscopic members each, to understand how much cluster-to-cluster variance exists in the β(r) of different clusters and what the main driver of this variance is. Methods. We selected spectroscopic cluster members with the <ns0:monospace>CLUMPS</ns0:monospace> algorithm calibrated on cosmological simulations. We applied the <ns0:monospace>MAMPOSSt</ns0:monospace> code to the distribution of cluster members in projected phase-space to constrain the cluster mass profile, M(r), using priors derived from a previous gravitational lensing analysis. Given the <ns0:monospace>MAMPOSSt</ns0:monospace> best-fit solution for M(r), we then solved the inversion of the Jeans equation to determine β(r) without assumptions of its functional form. We also ran the <ns0:monospace>DS+</ns0:monospace> code to identify subclusters and characterize the dynamical status of our clusters. Results. The average ⟨β(r)⟩ is slightly radial; the anisotropy increases from β ≃ 0.2 at the cluster center to β ≃ 0.5 at the virial radius. There is substantial variance in the β(r) of the individual clusters that cannot be entirely accounted for by the observational uncertainties. Clusters of lower mass and with a low concentration per given mass have more tangential β(r) profiles. A comparison with previous works in the literature suggests that orbits are more radial in clusters at higher z. A comparison with cluster-sized halos in cosmological hydrodynamical simulations indicates a very good agreement for the average ⟨β(r)⟩, but a smaller variance in the profiles than observed. Conclusions. Massive clusters cannot be characterized by a unique universal β(r). The orbital distribution of cluster galaxies carries information on the merging history of the cluster.