Intracluster Magnetic Filaments and an Encounter with a Radio Jet

• Published in: The Astrophysical journal 2022-08, Vol.935 (2), p.168
• Main Authors: Rudnick, L., Brüggen, M., Brunetti, G., Cotton, W. D., Forman, W., Jones, T. W., Nolting, C., Schellenberger, G., van Weeren, R.
• Format: Article
• Language: English
• Subjects: Astrophysics; Clusters; Cosmic ray electrons; Cosmic ray showers; Cosmic rays; Depth measurement; Electrons; Extragalactic magnetic fields; Extragalactic radio sources; Filaments; Galaxies; Galaxy clusters; Intracluster medium; LOFAR; Magnetic fields; Plasma physics; Poor galaxy clusters; Radio galaxies; Radio jets; Radio jets (astronomy); Relativistic effects; Relativistic particles; Sky surveys (astronomy); Surface brightness; Synchrotrons; Thermal plasmas
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ac7c76

Thin synchrotron-emitting filaments are increasingly seen in the intracluster medium (ICM). We present the first example of a direct interaction between a magnetic filament, a radio jet, and a dense ICM clump in the poor cluster A194. This enables the first exploration of the dynamics and possible histories of magnetic fields and cosmic rays in such filaments. Our observations are from the MeerKAT Galaxy Cluster Legacy Survey and the LOFAR Two-Meter Sky Survey. Prominent 220 kpc long filaments extend east of radio galaxy 3C40B, with very faint extensions to 300 kpc, and show signs of interaction with its northern jet. They curve around a bend in the jet and intersect the jet in Faraday depth space. The X-ray surface brightness drops across the filaments; this suggests that the relativistic particles and fields contribute significantly to the pressure balance and evacuate the thermal plasma in a ∼35 kpc cylinder. We explore whether the relativistic electrons could have streamed along the filaments from 3C40B, and present a plausible alternative whereby magnetized filaments are (a) generated by shear motions in the large-scale, post-merger ICM flow, (b) stretched by interactions with the jet and flows in the ICM, amplifying the embedded magnetic fields, and (c) perfused by re-energized relativistic electrons through betatron-type acceleration or diffusion of turbulently accelerated ICM cosmic-ray electrons. We use the Faraday depth measurements to reconstruct some of the 3D structures of the filameGnts and of 3C40A and B.