The XXL Survey

XXXV. The role of cluster mass in AGN activity^★

¹ AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, 91191 Gif-sur-Yvette, France
e-mail: ilias.koulouridis@cea.fr
² Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Bd de l’Observatoire, CS 34229, 06304 Nice cedex 4, France
³ School of Physics, HH Wills Physics Laboratory, Tyndall Avenue, Bristol BS8 1TL, UK
⁴ Aix Marseille Univ., CNRS, CNES, LAM, Marseille, France
⁵ Argelander-Institut für Astronomie, University of Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
⁶ National Observatory of Athens, Lofos Nymfon, 11810 Athens, Greece
⁷ Physics Department of Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
⁸ Australian Astronomical Observatory, North Ryde, NSW 2113, Australia
⁹ Institute for Astronomy & Astrophysics, Space Applications & Remote Sensing, National Observatory of Athens, 15236 Palaia Penteli, Greece
¹⁰ INAF - IASF - Milano, Via Bassini 15, 20133 Milano, Italy
¹¹ Main Astronomical Observatory, Academy of Sciences of Ukraine, 27 Akademika Zabolotnoho St., 03680 Kyiv, Ukraine
¹² Dipartimento di Fisica e Astronomia, Universitá di Bologna, via Gobetti 93/2, 40129 Bologna, Italy
¹³ INAF - Osservatorio Astronomico di Bologna, via Pietro Gobetti 93/3, 40129 Bologna, Italy
¹⁴ INFN, Sezione di Bologna, viale Berti Pichat 6/2, 40127 Bologna, Italy
¹⁵ Center for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK
¹⁶ Department of Astronomy, University of Geneva, ch. d’Ecogia 16, 1290 Versoix, Switzerland

Received: 6 March 2018
Accepted: 19 July 2018

Abstract

Context. We present the results of a study of the active galactic nucleus (AGN) density in a homogeneous and well-studied sample of 167 bona fide X-ray galaxy clusters (0.1 < z < 0.5) from the XXL Survey, from the cluster core to the outskirts (up to 6r₅₀₀). The results can provide evidence of the physical mechanisms that drive AGN and galaxy evolution within clusters, testing the efficiency of ram pressure gas stripping and galaxy merging in dense environments.

Aims. The XXL cluster sample mostly comprises poor and moderately rich structures (M = 10¹³–4 × 10¹⁴ M_⊙), a poorly studied population that bridges the gap between optically selected groups and massive X-ray selected clusters. Our aim is to statistically study the demographics of cluster AGNs as a function of cluster mass and host galaxy position.

Methods. To investigate the effect of the environment on AGN activity, we computed the fraction of spectroscopically confirmed X-ray AGNs (L_{X [0.5-10 keV]} > 10⁴² erg cm⁻¹) in bright cluster galaxies with M_i^* − 2 < M < M_i^* + 1, up to 6r₅₀₀ radius. The corresponding field fraction was computed from 200 mock cluster catalogues with reshuffled positions within the XXL fields. To study the mass dependence and the evolution of the AGN population, we further divided the sample into low- and high-mass clusters (below and above 10¹⁴M_⊙, respectively) and two redshift bins (0.1–0.28 and 0.28–0.5).

Results. We detect a significant excess of X-ray AGNs, at the 95% confidence level, in low-mass clusters between 0.5r₅₀₀ and 2r₅₀₀, which drops to the field value within the cluster cores (r < 0.5r₅₀₀). In contrast, high-mass clusters present a decreasing AGN fraction towards the cluster centres, in agreement with previous studies. The high AGN fraction in the outskirts is caused by low-luminosity AGNs, up to L_{X [0.5-10 keV]} = 10⁴³ erg cm⁻¹. It can be explained by a higher galaxy merging rate in low-mass clusters, where velocity dispersions are not high enough to prevent galaxy interactions and merging. Ram pressure stripping is possible in the cores of all our clusters, but probably stronger in deeper gravitational potentials. Compared with previous studies of massive or high-redshift clusters, we conclude that the AGN fraction in cluster galaxies anti-correlates strongly with cluster mass. The AGN fraction also increases with redshift, but at the same rate with the respective fraction in field galaxies.