Cosmic rays and the magnetic field in the nearby starburst galaxy NGC 253 III. Helical magnetic fields in the nuclear outflow

Context. Magnetic fields are good tracers of gas compression by shock w aves in the interstellar medium. These can be caused by the interaction of star-formation driven outflows from individ ual star formation sites as described in the chimney model. Integration along the line-of-sight and cosmic-ray diffusion may hamper detection of compressed magnetic fields in m any cases. Aims. We study the magnetic field structure in the central part of th e nuclear starburst galaxy NGC 253 with spatial resolutions between 40 and 150 pc to detect any filamentary emission assoc iated with the nuclear outflow. As the nuclear region is much b righter than the rest of the disc we can distinguish this emission fro m that of the disc. Methods. We used radio polarimetric observations with the VLA. New observations at �3 cm with 7. ′′ 5 resolution were combined with archive data at �� 20 and 6 cm. We created a map of the rotation measure distribution between �� 6 and 3 cm and compared it with a synthetic polarization map. Results. We find filamentary radio continuum emission in a geometrical distribution, which we interpret as the boundary of the NW nuclear outflow cone seen in projection. The scaleheight o f the continuum emission is 150± 20 pc, regardless of the observing frequency. The equipartition magnetic field strength is 46 ± 10µG for the total field and 21± 5µG for the regular field in the filaments. We find that the ordered magnetic field is aligned along the fila ments, in agreement with amplification due to compression. T he perpendicular diffusion coeffi cient across the filaments is �⊥ = 1.5× 10 28 cm 2 s −1 · E(GeV) 0.5±0.7 . In the SE part of the nuclear outflow cone the magnetic field is pointing away from the disc in form o f a helix, with an azimuthal component increasing up to at least 1200 pc height, where it is about equal to the total component. The ordered magnetic field in the disc is anisotropic within a radius of 2.2 kpc. At larger radii, the large-scale field is regular and of even parity. Conclusions. The magnetic filaments indicate an interaction of the nuclea r outflow with the interstellar medium. The magnetic field is able to collimate the outflow, which can explain the observ ed small opening angle of≈ 26 ◦ . Owing to the conservation of angular momentum by the plasma in the nuclear outflow, the field lines a re frozen into the plasma, and they wind up into a helix. Strong adiabatic losses of the cosmic-ray electrons in the acceler ated outflow can partly explain why the radio luminosity of th e nucleus lies below the radio-FIR correlation.