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We employ an analytical model that incorporates both wavelength-dependent andwavelength-independent depolarization to describe radio polarimetricobservations of polarization at $\lambda \lambda \lambda \, 3.5, 6.2, 20.5$ cmin M51 (NGC 5194). The aim is to constrain both the regular and turbulentmagnetic field strengths in the disk and halo, modeled as a two- or three-layermagneto-ionic medium, via differential Faraday rotation and internal Faradaydispersion, along with wavelength-independent depolarization arising fromturbulent magnetic fields. A reduced chi-squared analysis is used for thestatistical comparison of predicted to observed polarization maps to determinethe best-fit magnetic field configuration at each of four radial rings spanning$2.4 - 7.2$ kpc in $1.2$ kpc increments. We find that a two-layer modelingapproach 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, althoughthe resulting best-fit magnetic field strengths are comparable. This impliesthat all of the signal from the far halo is depolarized at these wavelengths.We find a total magnetic field in the disk of approximately $18~\mu$G and atotal magnetic field strength in the halo of $\sim 4-6~\mu$G. Both turbulentand regular magnetic field strengths in the disk exceed those in the halo by afactor of a few. About half of the turbulent magnetic field in the disk isanisotropic, but in the halo all turbulence is only isotropic.

Constraining regular and turbulent magnetic field strengths in M51 via Faraday depolarization