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We use the TNG50 cosmological magnetohydrodynamical simulation of theIllustrisTNG project to show that magnetic fields in the circumgalactic medium(CGM) have significant angular structure. This azimuthal anisotropy at fixeddistance is driven by galactic feedback processes that launch strong outflowsinto the halo, preferentially along the minor axes of galaxies. Thesefeedback-driven outflows entrain strong magnetic fields from the interstellarmedium, dragging fields originally amplified by small-scale dynamos into theCGM. At the virial radius, $z=0$ galaxies with M$_\star \sim10^{10}\,\rm{M_\odot}$ show the strongest anisotropy ($\sim 0.35$ dex). Thissignal weakens with decreasing impact parameter, and is also present but weakerfor lower mass as well as higher mass galaxies. Creating mock Faraday rotationmeasure (RM) sightlines through the simulated volume, we find that the angularRM trend is qualitatively consistent with recent observational measurements. Weshow that rich structure is present in the circumgalactic magnetic fields ofgalaxies. However, TNG50 predicts small RM amplitudes in the CGM that makedetection difficult as a result of other contributions along the line of sight.

Azimuthal Anisotropy of Magnetic Fields in the Circumgalactic Medium Driven by Galactic Feedback Processes