The Extended GMRT Radio Halo Survey

II. Further results and analysis of the full sample^⋆

¹ INAF-Istituto di Radioastronomia, via Gobetti 101, 40129 Bologna Italy
² Dipartimento di Fisica e Astronomia, Universita di Bologna, via Ranzani 1, 40127 Bologna, Italy
³ National Centre for Radio Astrophysics, TIFR, Ganeshkhind, 411007 Pune, India
e-mail: ruta@ncra.tifr.res.in
⁴ Department of Astronomy, University of Maryland, College Park, MD 20742, USA
⁵ Joint Space-Science Institute, University of Maryland, College Park, MD 20742-2421, USA
⁶ Laboratoire Lagrange, UMR 7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, 06300 Nice, France
⁷ Indian Institute of Science Education and Research (IISER), 411008 Pune, India

Received: 20 January 2015
Accepted: 25 February 2015

Abstract

The intra-cluster medium contains cosmic rays and magnetic fields that are manifested through the large scale synchrotron sources, termed radio haloes, relics, and mini-haloes. The Extended Giant Metrewave Radio Telescope (GMRT) Radio Halo Survey (EGRHS) is an extension of the GMRT Radio Halo Survey (GRHS) designed to search for radio haloes using GMRT 610/235 MHz observations. The GRHS and EGRHS consists of 64 clusters in the redshift range 0.2−0.4 that have an X-ray luminosity larger than 5 × 10⁴⁴ erg s^-1 in the 0.1−2.4 keV band and declination, δ > −31° in the REFLEX and eBCS X-ray cluster catalogues. In this second paper in the series, GMRT 610/235 MHz data on the last batch of 11 galaxy clusters and the statistical analysis of the full sample are presented. A new mini-halo in RX J2129.6+0005 and candidate diffuse sources in Z5247, A2552, and Z1953 have been discovered. A unique feature of this survey are the upper limits on the detections of 1 Mpc sized radio haloes; 4 new are presented here, making a total of 31 in the survey. Of the sample, 58 clusters with adequately sensitive radio information were used to obtain the most accurate occurrence fractions so far. The occurrence fractions of radio haloes, mini-haloes and relics in our sample are ~22%, ~16% and ~5%, respectively. The P_{1.4 GHz}−L_X diagrams for the radio haloes and mini-haloes are presented. The morphological estimators – centroid shift (w), concentration parameter (c), and power ratios (P₃/P₀) derived from the Chandra X-ray images – are used as proxies for the dynamical states of the GRHS and EGRHS clusters. The clusters with radio haloes and mini-haloes occupy distinct quadrants in the c−w, c−P₃/P₀ and w−P₃/P₀ planes, corresponding to the more and less morphological disturbance, respectively. The non-detections span both the quadrants.