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By observing the interacting galaxy NGC 3627 in radio polarization we try toanswer the question to which degree the magnetic field follows the galactic gasflows. We obtained total power and polarized intensity maps at 8.46 GHz and4.85 GHz using the VLA in its compact D-configuration. In order to overcome thezero-spacing problems, the interferometric data were combined with single-dishmeasurements obtained with the Effelsberg 100-m radio telescope. The observedmagnetic field structure in NGC 3627 suggests that two field components aresuperposed. One component smoothly fills the interarm space and shows up alsoin the outermost disk regions, the other component follows a symmetric S-shapedstructure. In the western disk the latter component is well aligned with anoptical dust lane, following a bend which is possibly caused by externalinteractions. However, in the SE disk the magnetic field crosses a heavy dustlane segment, apparently being insensitive to strong density-wave effects. Wesuggest that the magnetic field is decoupled from the gas by high turbulentdiffusion, in agreement with the large \ion{H}{i} line width in this region. Wediscuss in detail the possible influence of compression effects andnon-axisymmetric gas flows on the general magnetic field asymmetries in NGC3627. On the basis of the Faraday rotation distribution we also suggest theexistence of a large ionized halo around this galaxy.Comment: 11 pages, 11 figure

Unusual magnetic fields in the interacting spiral NGC 3627