NIKA2 observations of 3 low-mass galaxy clusters at z ~ 1: Pressure profile and YSZ – M relation

R. Adam; M. Ricci; D. Eckert; P. Ade; H. Ajeddig; B. Altieri; P. André; E. Artis; H. Aussel; A. Beelen; C. Benoist; A. Benoît; S. Berta; L. Bing; M. Birkinshaw; O. Bourrion; D. Boutigny; M. Bremer; M. Calvo; A. Cappi; A. Catalano; M. De Petris; F.-X. Désert; S. Doyle; E.F.C. Driessen; L. Faccioli; C. Ferrari; F. Gastaldello; P. Giles; A. Gomez; J. Goupy; O. Hahn; C. Hanser; C. Horellou; F. Kéruzoré; E. Koulouridis; C. Kramer; B. Ladjelate; G. Lagache; S. Leclercq; J.-F. Lestrade; J.F. Macías-Pérez; S. Madden; B. Maughan; S. Maurogordato; A. Maury; P. Mauskopf; A. Monfardini; M. Muñoz-Echeverría; F. Pacaud; L. Perotto; M. Pierre; G. Pisano; E. Pompei; N. Ponthieu; V. Revéret; A. Rigby; A. Ritacco; C. Romero; H. Roussel; F. Ruppin; M. Sereno; K. Schuster; A. Sievers; G. Tintoré Vidal; C. Tucker; R. Zylka

doi:10.1051/epjconf/202429300002

All issues

Volume 293 (2024)

EPJ Web Conf., 293 (2024) 00002

Abstract

Open Access

Issue		EPJ Web Conf. Volume 293, 2024 mm Universe 2023 - Observing the Universe at mm Wavelengths


Article Number		00002
Number of page(s)		6
DOI		https://doi.org/10.1051/epjconf/202429300002
Published online		28 March 2024

EPJ Web of Conferences 293, 00002 (2024)
https://doi.org/10.1051/epjconf/202429300002

NIKA2 observations of 3 low-mass galaxy clusters at z ~ 1: Pressure profile and Y_SZ – M relation

R. Adam¹^,2^*, M. Ricci³^,4^,1, D. Eckert⁵, P. Ade⁶, H. Ajeddig⁷, B. Altieri⁸, P. André⁷, E. Artis⁹, H. Aussel⁷, A. Beelen¹⁰, C. Benoist¹, A. Benoît¹¹, S. Berta¹², L. Bing¹⁰, M. Birkinshaw¹³^**, O. Bourrion⁹, D. Boutigny⁴, M. Bremer¹³, M. Calvo¹¹, A. Cappi¹^,14, A. Catalano⁹, M. De Petris¹⁵, F.-X. Désert¹⁶, S. Doyle⁶, E.F.C. Driessen¹², L. Faccioli⁷, C. Ferrari¹, F. Gastaldello¹⁷, P. Giles¹⁸, A. Gomez¹⁹, J. Goupy¹¹, O. Hahn¹, C. Hanser⁹, C. Horellou²⁰, F. Kéruzoré²¹, E. Koulouridis²²^,7, C. Kramer¹², B. Ladjelate²³, G. Lagache¹⁰, S. Leclercq¹², J.-F. Lestrade²⁴, J.F. Macías-Pérez⁹, S. Madden⁷, B. Maughan¹³, S. Maurogordato¹, A. Maury⁷, P. Mauskopf⁶^,25, A. Monfardini¹¹, M. Muñoz-Echeverría⁹, F. Pacaud²⁶, L. Perotto⁹, M. Pierre⁷, G. Pisano¹⁵, E. Pompei²⁷, N. Ponthieu¹⁶, V. Revéret⁷, A. Rigby⁶, A. Ritacco²⁸^,29, C. Romero³⁰, H. Roussel³¹, F. Ruppin³², M. Sereno¹⁴^,33, K. Schuster¹², A. Sievers²³, G. Tintoré Vidal², C. Tucker⁶ and R. Zylka¹²

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
² LLR, CNRS, École Polytechnique, Institut Polytechnique de Paris, France
³ Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-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, CH-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 Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
¹¹ Institut Néel, CNRS and Université Grenoble Alpes, 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, I-40127 Bologna, Italy
¹⁵ Dipartimento di Fisica, Sapienza Università di Roma, Piazzale Aldo Moro 5, I-00185 Roma, Italy
¹⁶ Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
¹⁷ INAF - IASF Milan, via A. Corti 12, I-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, SE-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, GR-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
²⁶ Argelander Institut für Astronomic, Universität Bonn, Auf dem Huegel 71, D-53121 Bonn, Germany
²⁷ European Southern Observatory, Alonso de Cordova 3107, Vitacura, 19001 Casilla, Santiago 19, Chile
²⁸ INAE-Osservatorio Astronomico di Cagliari, Via della Scienza 5, 09047 Selargius, Italy
²⁹ LPENS, Ecole Normale Supéricure, 24 rue Lhomond, 75005, Paris ( FR )
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 INPN, Sezione di Bologna, viale Berti Pichat 6/2, 40127 Bologna, Italy

^* e-mail: remi.adam@oca.eu
^** Deceased

Published online: 28 March 2024

Abstract

Three galaxy clusters selected from the XXL X-ray survey at high redshift and low mass (z ~ 1 and M₅₀₀ ~ 1 – 2 × 10¹⁴ M_⊙) were observed with NIKA2 to image their Sunyaev-Zel'dovich effect (SZ) signal. They all present an SZ morphology, together with the comparison with X-ray and optical data, that indicates dynamical activity related to merging events. Despite their disturbed intracluster medium, their high redshifts, and their low masses, the three clusters follow remarkably well the pressure profile and the SZ flux-mass relation expected from standard evolution. This suggests that the physics that drives cluster formation is already in place at z ~ 1 down to M₅₀₀ ~ 10¹⁴ M_⊙.

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