Cosmological MHD simulation of a cooling flow cluster

Context. Various observations of magnetic fields in the intra-cluster medium (ICM), most of the time restricted to cluster cores, point towards a field strength of a few (synchrotron radiation from radio relics and radio halos, inverse Compton radiation in X-rays and Faraday rotation measure of polarised background sources). Both the origin and the spatial structure of galaxy cluster magnetic fields are still under debate. In particular, the radial profile of the magnetic field, from the core of clusters to their outskirts, is important for cosmic ray propagation within the cosmic web.