The large scale magnetic field structure of the spiral galaxy NGC 5775

TL;DR

This study reveals the 3D magnetic field structure of NGC 5775, showing an X-shaped halo and an axisymmetric disk field, using multi-frequency radio polarization data and Faraday rotation analysis.

Contribution

It provides the first detailed 3D magnetic field model of NGC 5775, combining new observations with archival data to analyze the galaxy's magnetic topology.

Findings

Detected a large-scale X-shaped halo magnetic field.

Identified an even axisymmetric magnetic field in the disk.

Suggested galactic wind influences the halo magnetic structure.

Abstract

In order to better determine the large-scale 3D-structure of magnetic fields in spiral galaxies we present a Faraday rotation analysis of the edge-on spiral galaxy NGC 5775. Deep radio-continuum observations in total power and linear polarization were performed at 8.46 GHz with the VLA and the 100-m Effelsberg telescope. They were analyzed together with archival 4.86 and 1.49 GHz VLA-data. We thus can derive rotation measures from a comparison of three frequencies and determine the intrinsic magnetic field structure. A very extended halo is detected in NGC 5775, with magnetic field lines forming an X-shaped structure. Close to the galactic disk the magnetic field is plane-parallel. The scaleheights of the radio emission esimated for NGC 5775 are comaprable with other galaxies. The rotation measure distribution varies smoothly on both sides along the major axis from positive to negative values. From the derived distribution of rotation measures and the plane-parallel intrinsic magnetic field orientation along the galactic midplane we conclude that NGC 5775 has an 'even axisymmetric' large-scale magnetic field configuration in the disk as generated by an \alpha \Omega -dynamo which is accompanied by a quadrupolar poloidal field. The magnetic field lines of the plane-parallel component are pointing 'outwards'. The observed X-shaped halo magnetic field, however, cannot be explained by the action of the disk's mean-field dynamo alone. It is probably due to the influence of the galactic wind together with the dynamo action.