Magnetism in the spiral galaxy NGC 6946: magnetic arms, depolarization rings, dynamo modes and helical fields

TL;DR

This study investigates the magnetic field structures, dynamo modes, and depolarization phenomena in the spiral galaxy NGC 6946 through multi-band radio polarization observations, revealing complex magnetic arm configurations and large-scale helical fields.

Contribution

It provides new insights into the magnetic field topology, including the discovery of additional magnetic arms and depolarization rings, and links these features to dynamo modes and helical fields.

Findings

Magnetic arms are aligned with gas arms and are visible in polarized intensity.

Three new magnetic arms are discovered between HI arms in the outer galaxy.

Depolarization rings are likely caused by differential Faraday rotation in HII complexes.

Abstract

The spiral galaxy NGC 6946 was observed in total intensity and linear polarization in five radio bands between 3cm and 21cm. At the inner edge of the inner gas spiral arm the ordered magnetic field is only mildly compressed and turns smoothly, to become aligned along the gas arm. Hence the field is not shocked and is probably connected to the warm, diffuse gas. At larger radii, two bright magnetic arms between the optical arms are visible in polarized intensity. The field in the northern magnetic arm is almost totally aligned. Faraday rotation measures (RM) in these arms are consistent with the superposition of two low azimuthal dynamo modes. Three more magnetic arms are discovered in the outer galaxy, located between HI arms. Due to strong Faraday depolarization the galaxy is not transparent to polarized waves at 18cm and 20cm. The large-scale asymmetry in depolarization with respect to the major axis may be another indication of large-scale helical fields. Three depolarization rings of almost zero polarization seen at 20cm are probably generated by differential Faraday rotation in HII complexes in NGC 6946 of 300-500 pc size. - In the gas/optical spiral arms, the total (mostly turbulent) magnetic field is amplified to \simeq 20\muG. Its energy density is \simeq 10 times larger than that of the ionized gas and is similar to that of the turbulent gas motions in the inner galaxy. The magnetic energy exceeds that of the turbulent energy in the outer galaxy.