Astronomy and Astrophysics, volume 568A, 83-83 (2014/8-1)
Constraining regular and turbulent magnetic field strengths in M 51 via Faraday depolarization.
SHNEIDER C., HAVERKORN M., FLETCHER A. and SHUKUROV A.
Abstract (from CDS):
We employ an analytical model that incorporates both wavelength-dependent and wavelength-independent depolarization to describe radio polarimetric observations of polarization at λλλ 3.5, 6.2, 20.5cm in M51 (NGC 5194). The aim is to constrain both the regular and turbulent magnetic field strengths in the disk and halo, modeled as a two- or three-layer magneto-ionic medium, via differential Faraday rotation and internal Faraday dispersion, along with wavelength-independent depolarization arising from turbulent magnetic fields. A reduced chi-squared analysis is used for the statistical comparison of predicted to observed polarization maps to determine the best-fit magnetic field configuration at each of four radial rings spanning 2.4-7.2kpc in 1.2kpc increments. We find that a two-layer modeling approach provides a better fit to the observations than a three-layer model, where the near and far sides of the halo are taken to be identical, although the resulting best-fit magnetic field strengths are comparable. This implies that all of the signal from the far halo is depolarized at these wavelengths. We find a total magnetic field in the disk of approximately 18 µG and a total magnetic field strength in the halo of ∼4-6 µG. Both turbulent and regular magnetic field strengths in the disk exceed those in the halo by a factor of a few. About half of the turbulent magnetic field in the disk is anisotropic, but in the halo all turbulence is only isotropic.
galaxies: magnetic fields - polarization - galaxies: spiral - ISM: magnetic fields - radio continuum: galaxies