Synchrotron intensity gradient revealing magnetic fields in galaxy clusters

Yue Hu (), C. Stuardi, A. Lazarian (), G. Brunetti, A. Bonafede and Ka Wai Ho
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Yue Hu: University of Wisconsin-Madison
C. Stuardi: Universitá di Bologna
A. Lazarian: University of Wisconsin-Madison
G. Brunetti: INAF—Istituto di Radioastronomia di Bologna
A. Bonafede: Universitá di Bologna
Ka Wai Ho: University of Wisconsin-Madison

Nature Communications, 2024, vol. 15, issue 1, 1-12

Abstract: Abstract Magnetic fields and their dynamical interplay with matter in galaxy clusters contribute to the physical properties and evolution of the intracluster medium. However, the current understanding of the origin and properties of cluster magnetic fields is still limited by observational challenges. In this article, we map the magnetic fields at hundreds-kpc scales of five clusters RXC J1314.4-2515, Abell 2345, Abell 3376, MCXC J0352.4-7401, and El Gordo using the synchrotron intensity gradient technique in conjunction with high-resolution radio observations from the Jansky Very Large Array (JVLA) and the Karoo Array Telescope (MeerKAT). We demonstrate that the magnetic field orientation of radio relics derived from synchrotron intensity gradient is in agreement with that obtained with synchrotron polarization. Most importantly, the synchrotron intensity gradient is not limited by Faraday depolarization in the cluster central regions and allows us to map magnetic fields in the radio halos of RXC J1314.4-2515 and El Gordo. We find that magnetic fields in radio halos exhibit a preferential direction along the major merger axis and show turbulent structures at higher angular resolution. The results are consistent with expectations from numerical simulations, which predict turbulent magnetic fields in cluster mergers that are stirred and amplified by matter motions.

Date: 2024
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DOI: 10.1038/s41467-024-45164-8

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