Ram pressure statistics for bent tail radio galaxies

TL;DR

This study uses hydrodynamic simulations and abundance matching to analyze the distribution and characteristics of bent tail radio galaxies, revealing their association with cluster mass and location.

Contribution

It introduces a method combining simulations and abundance matching to statistically analyze ram pressure effects on bent radio sources.

Findings

50% of ram pressure exceeding galaxies are in clusters >10^{14.5}MSol

RPEX galaxies in low mass clusters are within 500 kpc of center

Clusters >10^{15}MSol can host multiple BRSs

Abstract

In this paper we use the MareNostrum Universe Simulation, a large scale, hydrodynamic, non-radiative simulation in combination with a simple abundance matching approach to determine the ram pressure statistics for bent radio sources (BRSs). The abundance matching approach allows us to determine the locations of all galaxies with stellar masses $> 10^{11} MSol$ in the simulation volume. Assuming ram pressure exceeding a critical value causes bent morphology, we compute the ratio of all galaxies exceeding the ram pressure limit (RPEX galaxies) relative to all galaxies in our sample. According to our model 50% of the RPEX galaxies at $z = 0$ are found in clusters with masses larger than $10^{14.5}MSol$ the other half resides in lower mass clusters. Therefore, the appearance of bent tail morphology alone does not put tight constraints on the host cluster mass. In low mass clusters, $M < 10^{14}MSol$, RPEX galaxies are confined to the central 500 kpc whereas in clusters of $> 10^{15}Msol$ they can be found at distances up to 1.5Mpc. Only clusters with masses $> 10^{15}MSol $ are likely to host more than one BRS. Both criteria may prove useful in the search for distant, high mass clusters.