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Magnetic fields in the intracluster medium (ICM) affect the structure and theevolution of galaxy clusters. However, their properties are largely unknown,and measuring magnetic fields in galaxy clusters is challenging, especially onlarge-scales outside of individual radio sources. In this work, we probe theplane-of-the-sky orientation of magnetic fields in clusters using the intensitygradients. The technique is a branch of the Gradient Technique (GT) thatemploys emission intensity maps from turbulent gas. We utilize the ChandraX-ray images of the Perseus, M 87, Coma, and A2597 galaxy clusters, and the VLAradio observations of the synchrotron emission from Perseus. We find that thefields predominantly follow the sloshing arms in Perseus, which is in agreementwith numerical simulations. The GT-predicted magnetic field shows signatures ofmagnetic draping around rising bubbles driven by supermassive black hole (SMBH)feedback in the centers of cool-core clusters, as well as draping aroundsubstructures merging with the Coma cluster. We calculate the mean-fieldorientation with respect to the radial direction in these clusters. In thecentral regions of cool-core clusters, the mean orientation of the magneticfields is preferentially azimuthal. There is a broad agreement between themagnetic field of Perseus predicted using the X-ray and radio data. Furthernumerical studies and better future observations with higher resolution and thelarger effective area will help reduce the uncertainties of this method.

Probing Magnetic Field Morphology in Galaxy Clusters with the Gradient Technique