Speaker
Description
Observations of Faraday rotation and synchrotron emission in galaxy clusters suggest the presence of large-scale magnetic fields with $\mu$G strengths, possibly extending back to $z=4$. We investigate how galaxy formation physics and feedback processes drive the rapid growth of these magnetic fields at high redshift. In the early stages, the central dominant galaxy plays a key role in magnetizing not only its surroundings but also the forming proto-cluster. This occurs through a combination of gravitationally driven, compressive turbulence that fuels a small-scale dynamo, and stellar and active galactic nucleus (AGN) feedback, which distributes magnetic fields via outflows. As the cluster evolves, additional galaxies contribute by merging into the proto-cluster, bringing their already amplified magnetic fields, which are then redistributed into the intracluster medium (ICM) through ram pressure stripping and galactic winds.
