CHEX-MATE: Exploring the kinematical properties of Planck galaxy clusters^⋆

¹ Dipartimento di Fisica G. Occhialini, Università degli Studi di Milano Bicocca, Piazza della Scienza 3, I-20126 Milano, Italy
² Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain
³ Universidad de La Laguna, Departamento de Astrofísica, E-38206 La Laguna, Tenerife, Spain
⁴ INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Piero Gobetti 93/3, I-40129 Bologna, Italy
⁵ INFN, Sezione di Bologna, Viale Berti Pichat 6/2, I-40127 Bologna, Italy
⁶ Dipartimento di Fisica ‘E. Pancini’, Università degli Studi di Napoli Federico II, Via Cinthia, 21, I-80126 Napoli, Italy
⁷ Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Bd de l’Observatoire, CS 34229, 06304 Nice Cedex 4, France
⁸ Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191 Gif-sur-Yvette, France
⁹ Michigan State University, Physics and Astronomy Department, 567 Wilson Road, East Lansing, Michigan 48824, USA
¹⁰ INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano, Via A. Corti 12, 20133 Milano, Italy
¹¹ Laboratoire d’Astrophysique de Marseille, Aix-Marseille Univ., CNRS, CNES, 13013 Marseille, France
¹² Institut d’Astrophysique de Paris, UMR7095 CNRS & Sorbonne Université, 98bis Bd Arago, 75014 Paris, France
¹³ Instituto de Astronomía y Ciencias Planetarias, Universidad de Atacama, Copayapu 485, Copiapó, Chile
¹⁴ Millennium Nucleus for Galaxies (MINGAL), Valparaíso, Chile
¹⁵ Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, University of Manchester, Manchester M13 9PL, UK
¹⁶ Center for Astrophysics | Harvard \AMP Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA
¹⁷ HH Wills Physics Laboratory, University of Bristol, Tyndall Ave, Bristol BS8 1TL, UK
¹⁸ IRAP, CNRS, Université de Toulouse, CNES, Toulouse, France
¹⁹ Osservatorio Astronomico di Trieste, Via Tiepolo 11, I-34131 Trieste, Italy
²⁰ IFPU, Institute for Fundamental Physics of the Universe, Via Beirut 2, 34014 Trieste, Italy
²¹ Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA
²² INAF – Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, I-35122 Padova, Italy
²³ California Institute of Technology, Pasadena, CA 91125, USA

^⋆⋆ Corresponding author.

Received: 7 May 2025
Accepted: 23 May 2025

Abstract

We 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−B₁) = M₅₀₀^SZ/M₅₀₀^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_sub). 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_sub, 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 r₂₀₀ is observed in clusters with larger velocity dispersions.