CHEX-MATE: Towards a consistent universal pressure profile and cluster mass reconstruction

In a self-similar paradigm of structure formation, the thermal pressure of the hot intra-cluster gas follows a universal distribution, once the profile of each cluster is normalised based on the proper mass and redshift dependencies. The reconstruction of such a universal pressure profile requires an individual estimate of the mass of each cluster. In this context, we present a method to jointly fit, for the first time, the universal pressure profile and individual cluster M 500 masses over a sample of galaxy clusters, properly accounting for correlations between the profile shape and amplitude, and masses that scale the individual profiles. We demonstrate the power of the method and show that a consistent exploitation of the universal pressure profile and cluster mass estimates when modelling the thermal pressure in clusters is necessary to avoid biases. In particular, the method, informed by a cluster mass scale, outputs individual cluster masses with the same accuracy and greater precision than input masses. Using data from the Cluster HEritage project with XMM-Newton : Mass Assembly and Thermodynamics at the Endpoint of structure formation (CHEX-MATE), we investigate a sample of ∼25 galaxy clusters spanning mass and redshift ranges of 2 ≲ M 500 /10 14 M ⊙ ≲ 14 and 0.07 < z < 0.6.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2025-11-07
DOI
https://doi.org/10.1051/0004-6361/202556045
Citations
2
Primary Topic
Galaxies: Formation, Evolution, Phenomena
Type
article
Field-Weighted Citation Impact
2.31
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article

CHEX-MATE: Towards a consistent universal pressure profile and cluster mass reconstruction

M. Gaspari, J. F. Macías–Pérez, Elena Rasia, M. Muñoz-Echeverría et al.
2 citations
Astronomy and Astrophysics
Galaxies: Formation, Evolution, Phenomena
2.31
article

CHEX-MATE: Towards a consistent universal pressure profile and cluster mass reconstruction

M. Gaspari, J. F. Macías–Pérez, Elena Rasia, M. Muñoz-Echeverría, N. Clerc, S. Ilić, Simon Dupourqué, Myriam Gitti, Adélie Gorce, Mariachiara Rossetti, M. De Petris, I. Bartalucci, L. McBride, F. Gastaldello, D. Eckert, Megan Donahue, M. Sereno, É. Pointecouteau, H Bourdin, Hori Lal Saxena, Scott T. Kay, L. Lovisari, Jack Sayers, Federico De Luca, M. Douspis, S. Ettori, Gabriel W. Pratt, M. Tristram, L. Salvati, Junhan Kim, B.J. Maughan, F Oppizzi, J.-B. Mélin, P. Mazzotta
article en
2 citations

Abstract

In a self-similar paradigm of structure formation, the thermal pressure of the hot intra-cluster gas follows a universal distribution, once the profile of each cluster is normalised based on the proper mass and redshift dependencies. The reconstruction of such a universal pressure profile requires an individual estimate of the mass of each cluster. In this context, we present a method to jointly fit, for the first time, the universal pressure profile and individual cluster M 500 masses over a sample of galaxy clusters, properly accounting for correlations between the profile shape and amplitude, and masses that scale the individual profiles. We demonstrate the power of the method and show that a consistent exploitation of the universal pressure profile and cluster mass estimates when modelling the thermal pressure in clusters is necessary to avoid biases. In particular, the method, informed by a cluster mass scale, outputs individual cluster masses with the same accuracy and greater precision than input masses. Using data from the Cluster HEritage project with XMM-Newton : Mass Assembly and Thermodynamics at the Endpoint of structure formation (CHEX-MATE), we investigate a sample of ∼25 galaxy clusters spanning mass and redshift ranges of 2 ≲ M 500 /10 14 M ⊙ ≲ 14 and 0.07 < z < 0.6.

Astronomy and AstrophysicsVol. 704
University of Geneva (CH), University of Rome Tor Vergata (IT), University of Modena and Reggio Emilia (IT), California Institute of Technology (US), Centre National de la Recherche Scientifique (FR), Université Toulouse III - Paul Sabatier (FR), Korea Advanced Institute of Science and Technology (KR), Université Fédérale de Toulouse Midi-Pyrénées (FR), Université Paris Cité (FR), Commissariat à l'Énergie Atomique et aux Énergies Alternatives (FR), Université Paris-Saclay (FR), University of Michigan (US), Trieste Astronomical Observatory (IT), University of Manchester (GB), University of Bristol (GB), Astrophysique, Instrumentation et Modélisation (FR), Institut d'Astrophysique Spatiale (FR), Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano (IT), Istituto Nazionale di Fisica Nucleare, Roma Tor Vergata (IT), Istituto di Radioastronomia di Bologna (IT), Center for Astrophysics Harvard & Smithsonian (US), Istituto Nazionale di Fisica Nucleare, Sezione di Genova (IT), CEA Paris-Saclay (FR), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (FR), Laboratoire de Physique Subatomique et de Cosmologie (FR), Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (IT), Institute for Fundamental Physics of the Universe (IT), Bristol Robotics Laboratory (GB), Institut de Recherche sur les Lois Fondamentales de l'Univers (FR), Institut de Recherche en Astrophysique et Planétologie (FR), Osservatorio di Astrofisica e Scienza dello Spazio, Sapienza University of Rome (IT), Michigan State University (US), Université Grenoble Alpes (FR), University of Bologna (IT)
Openalex Percentile: Top 10%
Galaxies: Formation, Evolution, Phenomena
2.31
DOIOpen Access PDFOpenAlex
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