Speaker
Description
Magnetic fields are a fundamental component of galaxy clusters, regulating cosmic-ray transport, plasma thermodynamics, and the dynamics of the intracluster medium. Yet their origin, amplification, and three-dimensional structure remain poorly understood, in large part because traditional probes such as synchrotron polarization and Faraday rotation provide only limited, 2D information. A central open question is how cluster mergers and turbulence shape magnetic-field topology and strength, and what role these processes play in cosmic magnetogenesis.
In this talk, I will present new observational evidence linking cluster turbulence and mergers to the amplification of magnetic fields. By exploiting morphological signatures in radio and X-ray data, and guided by advances in turbulence theory, we have developed new diagnostic approaches—including the synchrotron intensity gradient method and machine learning—that allow us to trace the 3D structure of cluster magnetic fields. Applying these tools to high-resolution MeerKAT observations, we have mapped the magnetic fields of several massive clusters, including the extreme merger El Gordo, providing direct evidence of turbulence-driven field amplification on mega-kiloparsec scales.
Looking ahead, the synergy of these techniques with upcoming facilities such as LOFAR and the Square Kilometre Array (SKA) will enable systematic surveys of cluster magnetic fields, opening a new observational window on their role in large-scale structure formation and the cosmic origin of magnetism.
| Session Selection | Astronomy and Astrophysics |
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