Abstract
Faraday tomography allows us to study the distribution and properties of the magnetoionic medium of galaxies through the Faraday effect. However, this can be achieved only after the Faraday spectrum is interpreted. One approach is using galactic ISM/magnetism models to investigate how characteristic properties of the galaxies in the physical depth space are reflected to the Faraday spectrum. In this paper, I employ a realistic Galactic ISM/magnetism model and calculate the intrinsic Faraday spectrum of face-on galaxies, especially focusing on the galactic disk-halo structure and on the presence of the coherent, vertical magnetic field. I also calculate the Faraday depth cubes of the Milky Way from the model. I discuss the possibility of studying the disk and halo structures by means of Faraday tomography.
Highlights
Faraday tomography aims to determine the distribution and properties of magnetoionic medium along the line of sight (LOS) toward, and within, astronomical objects through the Faraday effect.This technique requires wide-band low frequency (.10 GHz) polarization data, and the SquareKilometre Array and its precursors/pathfinders make it possible to use the technique for studying cosmic magnetism
Cosmic magnetism studies using Faraday tomography require the interpretation of the Faraday spectrum, F (φ), which gives the intensity of synchrotron polarization as a function of the Faraday depth, φ
Faraday spectrum of galaxies using the realistic Galactic model constructed by Akahori et al [11]
Summary
Faraday tomography aims to determine the distribution and properties of magnetoionic medium along the line of sight (LOS) toward, and within, astronomical objects through the Faraday effect. (e.g., [4]), used optical photometric data showing a morphological correspondence (e.g., [5]), or used the information of Hα line which is a good tracer of warm ionized gas (e.g., [3,6]) Another complementary approach to interpret the properties of F (φ) can be to use simulation results. We have the information of the magnetic field as a function of physical depth and we can calculate the Faraday spectrum. In Ideguchi et al [10], they studied F (φ) of a small portion of the external face-on galaxies using the realistic Galactic model constructed by Akahori et al [11]. I study how the presence of the vertical magnetic field and the halo affect the polarization structures in the Faraday depth cubes.
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