Speaker
Description
Diffuse radio emission in galaxy clusters has been established to be linked with the presence of (re-)accelerated particles (i.e. cosmic rays, CRs) and magnetic fields (B). In the last years, thanks to the advent of highly-sensitive radio telescopes such as LOFAR and MeerKAT, the detection of diffuse radio emission has become possible also in clusters at high redshift (z>0.6). This allowed a first investigation of evolution of magnetic fields in the largest virtualised structures in the Universe, at the time of their formation. However, a complete statistical analysis is still missing. I will present the current knowledge on the cosmic evolution of magnetic fields, and the future window that SKA and its precursors will open. These new observations will provide crucial insights on the properties of the non-thermal component in the high-z cluster population.
