Magnetic fields in the intracluster medium (ICM) affect the structure and the evolution of galaxy

clusters. However, their properties are largely unknown, and measuring magnetic fields in galaxy

clusters is challenging, especially on large-scales outside of individual radio sources. Here we

probe the plane-of-the-sky orientation of magnetic fields in clusters using the intensity gradients.

The technique is a branch of the Gradient Technique (GT) that employs emission intensity maps

from turbulent gas. We utilize the Chandra X-ray images of the Perseus, M 87, Coma, and

A2597 galaxy clusters, and the VLA radio observations of the synchrotron emission from

Perseus. We find that the fields predominantly follow the sloshing arms in Perseus, which is in

agreement with numerical simulations. The GT-predicted magnetic field shows signatures of

magnetic draping around rising bubbles driven by supermassive black hole (SMBH) feedback in

the centers of cool-core clusters, as well as draping around substructures merging with the Coma

cluster.

Zoom Recording: https://uky.zoom.us/rec/share/mkGB72TcxVuohGMJ5EVwN282koaKcMinbki7FuSKX3UvAwcl4j22df-zG5VZJnS_.gnvslk37Wx91DbZZ