Mami Machida

Studies of the three-dimensional structures of galactic magnetic fields are now entering a new era, with broad-band, highly sensitive radio observations and new analysis methods. To reveal the magnetic field configuration from the observed intensities integrated along the line of sight, it is necessary to derive an appropriate model involving various combinations of parameters that can reproduce the same observational characteristics. We aim to clarify the relationship between the radiation field and the spatial distribution of physical quantities through pseudo-observations using global three-dimensional magnetohydrodynamics (MHD) simulation results. In particular, we focus here on using the depolarization effect, which is important in the meter-wave band, to verify the polarization model and to identify the emission region. First, we show that wavelength-independent depolarization, which takes into account anisotropic turbulence, does not work efficiently because the polarized emission is stronger in regions of ordered spiral fields than in regions dominated by isotropic turbulent fields. Beam depolarization, specifically internal depolarization, becomes more effective below 1 GHz. Although in and close to the equatorial plane there will be strong depolarization that increases with observing wavelength, this effect is less in the halo, making halo magnetic fields detectable through their polarized emission at meter-wavelength bands. Although polarized emission from the halo is below the detection limit of current facilities, it will be detectable within the Square Kilometer Array era. In addition, we find that the spiral polarization projected on a screen is produced by overlapping magnetic flux tubes extending to different heights from the equatorial plane. This suggests that the traditional classification of global magnetic fields has difficulty reproducing the global structure of the magnetic fields. Finally, we demonstrate the method to separate magnetic flux tubes at different heights by using peak frequencies that cause the decrease of polarized flux.