Fractional polarization and magnetic fields in the ICM

TL;DR

This study investigates the magnetic field properties of the intra-cluster medium in galaxy clusters by analyzing radio polarization data, revealing a radial trend in polarization linked to magnetic field strength and cluster features.

Contribution

It provides new insights into the magnetic field distribution in galaxy clusters and its relation to thermal and non-thermal properties, using a novel analysis of polarization data across multiple clusters.

Findings

Fractional polarization increases towards the cluster periphery.

No difference in depolarization trends between clusters with and without radio halos.

Significant differences in polarization trends between cool core and non-cool core clusters.

Abstract

The aim of this work is to investigate the average properties of the intra-cluster medium (ICM) magnetic fields, and to search for possible correlations with the ICM thermal properties and cluster radio emission. We have selected a sample of 39 massive galaxy clusters from the HIghest X-ray FLUx Galaxy Cluster Sample, and used Northern VLA Sky Survey data to analyze the fractional polarization of radio sources out to 10 core radii from the cluster centers. Following Murgia et al (2004), we have investigated how different magnetic field strengths affect the observed polarized emission of sources lying at different projected distances from the cluster center. In addition, statistical tests are performed to investigate the fractional polarization trends in clusters with different thermal and non-thermal properties. We find a trend of the fractional polarization with the cluster impact parameter, with fractional polarization increasing at the cluster periphery and decreasing toward the cluster center. Such trend can be reproduced by a magnetic field model with central value of few $\mu$G. The logrank statistical test indicates that there are no differences in the depolarization trend observed in cluster with and without radio halo, while the same test indicates significant differences when the depolarization trend of sources in clusters with and without cool core are compared. The comparison between clusters with high and low temperatures does not yields significant differences. Although therole of the gas density should be better accounted for, these results give important indications for models that require a role of the ICM magnetic field to explain the presence of cool core and radio halos in galaxy clusters.