Radio relics in the MareNostrum Universe

TL;DR

This paper investigates radio relics in galaxy clusters using simulations, modeling shock-accelerated electrons to predict radio emissions at 1.4 GHz and 120 MHz, aiding future radio telescope observations.

Contribution

It introduces a simulation-based analysis of radio relics, linking shock waves in galaxy clusters to non-thermal radio emissions at multiple frequencies.

Findings

Predicted radio relic counts at 1.4 GHz and 120 MHz

Constraints for LOFAR and future radio telescopes

Correlation between shock regions and radio emissions

Abstract

We identify shocked gas in simulated galaxy clusters extracted from the MareNostrum Universe simulation (Gottloeber et al. 2006) assuming that shock waves are regions of electron acceleration. We perform flux number counts within the framework of the non-thermal emission model developed by Hoeft et al. (2008). Results are presented at two different observing frequencies, i.e. 1.4 GHz and 120 MHz, posing interesting constraints for LOFAR and upcoming radio telescopes.