The hydrostatic-to-lensing mass bias from resolved X-ray and optical-IR data

¹ Univ. Grenoble Alpes, CNRS, LPSC-IN2P3, 53 avenue des Martyrs, 38000 Grenoble, France
e-mail: miren.munoz@lpsc.in2p3.fr
² Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191 Gif-sur-Yvette, France
³ Univ. de Toulouse, UPS-OMP, CNRS, IRAP, 31028 Toulouse, France
⁴ High Energy Physics Division, Argonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA
⁵ Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain
⁶ Dipartimento di Fisica, Sapienza Università di Roma, Piazzale Aldo Moro 5, 00185 Roma, Italy
⁷ INAF, IASF-Milano, Via A. Corti 12, 20133 Milano, Italy
⁸ Departamento de Física Teórica and CIAFF, Facultad de Ciencias, Modulo 8, Universidad Autónoma de Madrid, 28049 Madrid, Spain
⁹ Centro de Investigación Avanzada en Física Fundamental (CIAFF), Universidad Autónoma de Madrid, Cantoblanco, 28049 Madrid, Spain

Received: 21 July 2023
Accepted: 13 November 2023

Abstract

An accurate reconstruction of galaxy cluster masses is key to use this population of objects as a cosmological probe. In this work we present a study on the hydrostatic-to-lensing mass scaling relation for a sample of 53 clusters whose masses were reconstructed homogeneously in a redshift range between z = 0.05 and 1.07. The M₅₀₀ mass for each cluster was indeed inferred from the mass profiles extracted from the X-ray and lensing data, without using a priori observable-mass scaling relations. We assessed the systematic dispersion of the masses estimated with our reference analyses with respect to other published mass estimates. Accounting for this systematic scatter does not change our main results, but enables the propagation of the uncertainties related to the mass reconstruction method or used dataset. Our analysis gives a hydrostatic-to-lensing mass bias of (1−b) = 0.739_−0.070^+0.075 and no evidence of evolution with redshift. These results are robust against possible subsample differences.