https://creativecommons.org/licenses/by/4.0/Pizzuti, LorenzoLorenzoPizzutiBarrena, RafaelRafaelBarrenaSereno, MauroMauroSerenoStreblyanska, AlinaAlinaStreblyanskaFerragamo, AntonioAntonioFerragamoMaurogordato, SophieSophieMaurogordatoCappi, AlbertoAlbertoCappiEttori, StefanoStefanoEttoriPratt, Gabriel W.Gabriel W.PrattCastignani, GianlucaGianlucaCastignani2025-10-102025-10-10202500046361; 14320746https://hdl.handle.net/20.500.12740/23379We analysed the kinematical properties of the CHEX-MATE galaxy cluster sample. Our study is based on the radial velocities retrieved from the SDSS DR18, DESI, and NED spectroscopic databases and new data obtained with the 10.4 m GTC and ESO-NTT telescopes. We derived cluster mass profiles for 75 clusters using the MG-MAMPOSST procedure, which recovers the gravitational potential and the anisotropy profiles from line-of-sight velocities and projected positions of galaxy members. The standard Navarro- Frenk- White (NFW) model and the Burkert model, with flatter cores than the NFW, both adequately fit the kinematic data, with only a marginal statistical preference for one model over the other. An estimation of the mass bias (1- B<inf>1</inf>) = M<inf>500</inf>SZ/M<inf>500</inf>M was performed via a comparison with Sunyaev-Zel'dovich- X-ray-calibrated mass estimates, resulting in a value of 0.54 ± 0.11 when four evidently disturbed clusters are removed from the sample. We assessed the dynamical state of the clusters by inferring the Anderson-Darling coefficient (A2) and the fraction of galaxies in substructures (f<inf>sub</inf>). Except for a few cases, we find relatively low values for A2, which suggests that CHEX-MATE clusters are not too far from relaxation. Moreover, no significant trends emerge between A2 and f<inf>sub</inf>, nor between the log-masses estimated by MG-MAMPOSST and those based on the Sunyaev- Zel'dovich effect calibrated through X-rays measurements. We studied the concentration- mass relation for the sample; despite the large scatter, we observe signs of an increasing trend for high-mass clusters, in agreement with recent theoretical expectations. Finally, our analysis of the radial anisotropy profiles of member galaxies - stacked in five bins of mass and redshift - reveals that orbits tend to be isotropic at the centre and more radial towards the edge, as found in previous studies. A slight trend of increasing radial orbits at r<inf>200</inf> is observed in clusters with larger velocity dispersions. © 2025 Elsevier B.V., All rights reserved.openAccessGALAXIES: CLUSTERS: GENERALGALAXIES: KINEMATICS AND DYNAMICSANISOTROPYGALAXIESGRAVITATIONCLUSTER MASSESO/NTTGALAXIES CLUSTERSGRAVITATIONAL POTENTIALLINE OF SIGHTPROPERTYRADIAL VELOCITYSPECTROSCOPIC DATABASEKINEMATICSArtículo https://doi.org/10.1051/0004-6361/202555417