Multi-probe analysis of the galaxy cluster CL J1226.9+3332

Hydrostatic mass and hydrostatic-to-lensing bias

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 LLR (Laboratoire Leprince-Ringuet), CNRS, École Polytechnique, Institut Polytechnique de Paris, Av. Chasles, 91120 Palaiseau, France
⁴ School of Physics and Astronomy, Cardiff University, Queen’s Buildings, The Parade, Cardiff CF24 3AA, UK
⁵ INAF, IASF-Milano, Via A. Corti 12, 20133 Milano, Italy
⁶ Aix-Marseille Univ., CNRS, CNES, LAM (Laboratoire d’Astrophysique de Marseille), 38 rue Frédéric Joliot Curie, 13013 Marseille, France
⁷ Institut Néel, CNRS, Université Grenoble Alpes, 25 Av. des Martyrs, 38042 Grenoble, France
⁸ Institut de RadioAstronomie Millimétrique (IRAM), 300 rue de la Piscine, 38400 Saint-Martin-d’Hères, France
⁹ Dipartimento di Fisica, Sapienza Università di Roma, Piazzale Aldo Moro 5, 00185 Roma, Italy
¹⁰ Univ. Grenoble Alpes, CNRS, IPAG, 414 rue de la Piscine, 38400 Saint-Martin-d’Hères, France
¹¹ Centro de Astrobiología (CSIC-INTA), Torrejón de Ardoz, 28850 Madrid, Spain
¹² High Energy Physics Division, Argonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA
¹³ Instituto de Radioastronomía Milimétrica (IRAM), Av. Divina Pastora, 7, 18012 Granada, Spain
¹⁴ LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Université, UPMC, 75014 Paris, France
¹⁵ School of Earth and Space Exploration and Department of Physics, Arizona State University, Tempe, AZ 85287, USA
¹⁶ IRFU, CEA, Université Paris-Saclay, 91191 Gif-sur-Yvette, France
¹⁷ Univ. de Toulouse, UPS-OMP, CNRS, IRAP, 31028 Toulouse, France
¹⁸ Laboratoire de Physique de l’École Normale Supérieure, ENS, PSL Research University, CNRS, Sorbonne Université, Université de Paris, 75005 Paris, France
¹⁹ INAF-Osservatorio Astronomico di Cagliari, Via della Scienza 5, 09047 Selargius, Italy
²⁰ Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104, USA
²¹ Institut d’Astrophysique de Paris, CNRS (UMR7095), 98 bis boulevard Arago, 75014 Paris, France
²² Univ. Lyon, Univ. Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, 69622 Villeurbanne, France
²³ Caltech, 1200 E California Blvd, Pasadena, CA 91125, USA
²⁴ Departamento de Física Teórica and CIAFF, Facultad de Ciencias, Modulo 8, Universidad Autánoma de Madrid, 28049 Madrid, Spain

Received: 15 September 2022
Accepted: 18 December 2022

Abstract

The precise estimation of the mass of galaxy clusters is a major issue for cosmology. Large galaxy cluster surveys rely on scaling laws that relate cluster observables to their masses. From the high-resolution observations of ∼45 galaxy clusters with the NIKA2 and XMM-Newton instruments, the NIKA2 Sunyaev-Zel’dovich Large Program should provide an accurate scaling relation between the thermal Sunyaev-Zel’dovich effect and the hydrostatic mass. In this paper we present an exhaustive analysis of the hydrostatic mass of the well-known galaxy cluster CL J1226.9+3332, the highest-redshift cluster in the NIKA2 Sunyaev-Zel’dovich Large Program at z = 0.89. We combined the NIKA2 observations with thermal Sunyaev-Zel’dovich data from the NIKA, Bolocam, and MUSTANG instruments and XMM-Newton X-ray observations, and tested the impact of the systematic effects on the mass reconstruction. We conclude that slight differences in the shape of the mass profile can be crucial when defining the integrated mass at R₅₀₀, which demonstrates the importance of the modelling in the mass determination. We prove the robustness of our hydrostatic mass estimates by showing the agreement with all the results found in the literature. Another key factor for cosmology is the bias of the masses estimated assuming the hydrostatic equilibrium hypothesis. Based on the lensing convergence maps from the Cluster Lensing And Supernova survey with Hubble (CLASH) data, we obtain the lensing mass estimate for CL J1226.9+3332. From this we are able to measure the hydrostatic-to-lensing mass bias for this cluster, which spans from 1 − b_HSE/lens ∼ 0.7 to 1, presenting the impact of data sets and mass reconstruction models on the bias.