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The interstellar medium (ISM) in galaxies is directly affected by the massand energy outflows originating in regions of star formation. Magnetic fieldsare an essential ingredient of the ISM, but their connection to the gaseousmedium and its evolution remains poorly understood. Here we present thedetection of a gradient in Faraday rotation measure (RM), co-located with ahole in the neutral hydrogen (HI) distribution in the disk of the nearby spiralgalaxy NGC 6946. The gas kinematics in the same location show evidence forinfall of cold gas. The combined characteristics of this feature point to asubstantial vertical displacement of the initially plane-parallel orderedmagnetic field, driven by a localized star formation event. This reveals howthe large-scale magnetic field pattern in galaxy disks is directly influencedby internal energetic phenomena. Conversely, magnetic fields are observed to bean important ingredient in disk-halo interactions, as predicted in MHDsimulations. Turbulent magnetic fields at smaller spatial scales than theobserved RM gradient will also be carried from the disk and provide a mechanismfor the dynamo process to amplify the ordered magnetic field without quenching.We discuss the observational biases, and suggest that this is a common featureof star forming galaxies with active disk-halo flows.

Magnetic field transport from disk to halo via the galactic chimney process in NGC 6946