Radio relics in PSZ2 G096.88+24.18: A connection with pre-existing plasma

TL;DR

This study investigates how pre-existing relativistic electrons, possibly supplied by AGN, influence the formation and brightness of radio relics in merging galaxy clusters, using multi-wavelength observations of PSZ2 G096.88+24.18.

Contribution

It provides observational evidence linking AGN-related seed electrons to the enhanced brightness of radio relics in a merging galaxy cluster.

Findings

A diffuse emission connects a radio galaxy with a relic, indicating a possible seed electron source.

The shock wave likely re-accelerates electrons from an AGN lobe, increasing relic brightness.

The connection suggests pre-existing relativistic electrons are important for relic formation.

Abstract

Giant radio relics are arc-like structures of diffuse, non-thermal synchrotron radiation that trace shock waves induced by galaxy cluster mergers. The particle (re-)acceleration mechanism producing such radio relics is unclear. One major open question is whether relics can be formed directly from a population of thermal seed electrons, or if pre-existing relativistic seed electrons are required. In some cases AGN can provide such a population of sub-GeV electrons. However, it is unclear how common this connection is. In this paper we present LOFAR 140 MHz and VLA L-band radio observations, as well as Chandra data of PSZ2 G096.88+24.18, a merging galaxy cluster system hosting a pair of radio relics. A large patch of diffuse emission connects a bright radio galaxy with one of the relics, likely affecting the properties of the relic. We find that the most plausible explanation for the connection is that the merger shock wave has passed over an AGN lobe. The shock passing over this seed population of electrons has led to an increased brightness in the relic only in the region filled with seed electrons.