The XXL Survey

LI. Pressure profile and Y_SZ − M scaling relation in three low-mass galaxy clusters at z ∼ 1 observed with NIKA2^⋆

¹ Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Blvd de l’Observatoire, CS 34229, 06304 Nice Cedex 4, France
e-mail: remi.adam@oca.eu
² LLR, CNRS, École Polytechnique, Institut Polytechnique de Paris, Paris, France
³ Université Paris Cité, CNRS, Astroparticule et Cosmologie, 75013 Paris, France
⁴ Laboratoire d’Annecy de Physique des Particules, Université Savoie Mont Blanc, CNRS/IN2P3, 74941 Annecy, France
⁵ Department of Astronomy, University of Geneva, ch. d’Ecogia 16, 1290 Versoix, Switzerland
⁶ School of Physics and Astronomy, Cardiff University, Queen’s Buildings, The Parade, Cardiff CF24 3AA, UK
⁷ Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191 Gif-sur-Yvette, France
⁸ European Space Astronomy Centre (ESA/ESAC), Operations Department, Villanueva de la Canãda, Madrid, Spain
⁹ Laboratoire de Physique Subatomique et de Cosmologie, Université Grenoble Alpes, CNRS/IN2P3, 53 Avenue des Martyrs, Grenoble, France
¹⁰ , 13388 Marseille, France
¹¹ Institut Néel, CNRS and Université Grenoble Alpes, Paris, France
¹² Institut de RadioAstronomie Millimétrique (IRAM), Grenoble, France
¹³ HH Wills Physics Laboratory, University of Bristol, Tyndall Avenue, Bristol BS8 1TL, UK
¹⁴ Istituto Nazionale di Astrofisica (INAF)–Osservatorio di Astrofisica e Scienza dello Spazio (OAS), Via Gobetti 93/3, 40127 Bologna, Italy
¹⁵ Dipartimento di Fisica, Sapienza Università di Roma, Piazzale Aldo Moro 5, 00185 Roma, Italy
¹⁶ Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
¹⁷ INAF – IASF Milan, Via A. Corti 12, 20133 Milano, Italy
¹⁸ Department of Physics and Astronomy, University of Sussex, Brighton BN1 9QH, UK
¹⁹ Centro de Astrobiología (CSIC-INTA), Torrejón de Ardoz, 28850 Madrid, Spain
²⁰ Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden
²¹ High Energy Physics Division, Argonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA
²² Institute for Astronomy & Astrophysics, Space Applications & Remote Sensing, National Observatory of Athens, 15236 Palaia Penteli, Greece
²³ Institut de RadioAstronomie Millimétrique (IRAM), Granada, Spain
²⁴ LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, 75014 Paris, France
²⁵ School of Earth and Space Exploration and Department of Physics, Arizona State University, Tempe, AZ 85287, USA
²⁶ Argelander Institut für Astronomie, Universität Bonn, Auf dem Huegel 71, 53121 Bonn, Germany
²⁷ European Southern Observatory, Alonso de Cordova 3107, Vitacura, 19001, Casilla, Santiago 19, Chile
²⁸ INAF – Osservatorio Astronomico di Cagliari, Via della Scienza 5, 09047 Selargius, Italy
²⁹ LPENS, Ecole Normale Supérieure, 24 rue Lhomond, 75005 Paris, France
³⁰ Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104, USA
³¹ Institut d’Astrophysique de Paris, Sorbonne Universités, UPMC Univ. Paris 06, CNRS UMR 7095, 75014 Paris, France
³² Univ. Lyon, Univ. Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, 69622 Villeurbanne, France
³³ INFN, Sezione di Bologna, Viale Berti Pichat 6/2, 40127 Bologna, Italy

Received: 22 September 2023
Accepted: 6 October 2023

Abstract

Context. The thermodynamical properties of the intracluster medium (ICM) are driven by scale-free gravitational collapse, but they also reflect the rich astrophysical processes at play in galaxy clusters. At low masses (∼10¹⁴ M_⊙) and high redshift (z ≳ 1), these properties remain poorly constrained, observationally speaking, due to the difficulty in obtaining resolved and sensitive data.

Aims. We aim to investigate the inner structure of the ICM as seen through the Sunyaev–Zel’dovich (SZ) effect in this regime of mass and redshift. We focused on the thermal pressure profile and the scaling relation between SZ flux and mass, namely the Y_SZ − M scaling relation.

Methods. The three galaxy clusters XLSSC 072 (z = 1.002), XLSSC 100 (z = 0.915), and XLSSC 102 (z = 0.969), with M₅₀₀ ∼ 2 × 10¹⁴ M_⊙, were selected from the XXL X-ray survey and observed with the NIKA2 millimeter camera to image their SZ signal. XMM-Newton X-ray data were used as a complement to the NIKA2 data to derive masses based on the Y_X − M relation and the hydrostatic equilibrium.

Results. The SZ images of the three clusters, along with the X-ray and optical data, indicate dynamical activity related to merging events. The pressure profile is consistent with that expected for morphologically disturbed systems, with a relatively flat core and a shallow outer slope. Despite significant disturbances in the ICM, the three high-redshift low-mass clusters follow the Y_SZ − M relation expected from standard evolution remarkably well.

Conclusions. These results indicate that the dominant physics that drives cluster evolution is already in place by z ∼ 1, at least for systems with masses above M₅₀₀ ∼ 10¹⁴ M_⊙.