AGN Feedback in the Survey era: Insights into large samples of Clusters and Groups through LOFAR, MeerKAT and eROSITA

In the last two decades, significant improvements have been made in the understanding of how AGN feedback operates in galaxy clusters. However, the vast majority of these studies involved observations of small samples, mostly lying in the high mass (M> 5 x 10^14 Msun) regime. We will present recent works in which we make use of survey observations performed by VLA, LOFAR and MeerKAT in the radio band, as well as eROSITA, Chandra and XMM-Newton in the X-rays, to investigate AGN feedback on the macro scale in large (N>200) samples of galaxy clusters and groups, down to masses of 2 x 10^13 Msun. We find a close relation between the X-ray emission -estimated within the whole cluster/group extent- and the radio emission produced by the central AGN. Statistical tests show that this correlation is not dominated by biases or selection effects. After converting the radio power into kinetic luminosity, we find an even tighter relation which seemingly exists for both disturbed and relaxed objects. Exploiting a subsample composed by COSMOS spectroscopic galaxy members, we find that Brightest Cluster Galaxies hosting strong AGN radio emission always lie within 0.2 virial radii from the cluster centre, and that there is an higher probability of stronger AGN being hosted in more massive systems. All these observations support the picture of a strong connection between the ICM and radio galaxies hosted in BCGs, which is also predicted by Chaotic Cold Accretion (CCA) models.