indicate the existence of turbulent magnetic fields [@sun08; @wae09; @gae11; @bur12]. These would result in complicated shape of FDF. So far, there are a number of theoretical works which investigated the capability of Faraday RM synthesis [see @sun14 references therein]. But most of them have considered a simple form of FDF such as the delta function, top hat, and gaussian function for simplicity.

There are some attempts which considered turbulence on the FDF of galaxies using simple models [e.g., @bel11; @fri11; @bec12]. For instance, [@bel11] took into account a simple magnetic field reversals, more or less realistic galactic model, and simple Gaussian random magnetic fields, and then discussed Faraday caustics – sharply peaked and asymmetric profiles are shown in the FDF because of LOS magnetic-field reversals. They examined observed FDFs assuming observations by radio telescopes such as the LOw-Frequency ARray (LOFAR) and Australian SKA Pathfinder (ASKAP) POSSUM survey.

Although previous studies have indicated an importance of simulating observed FDFs, it is complementary to focus on intrinsic FDFs in detail. Since real FDFs of galaxies would be complicated, it is meaningless to study observed FDFs without confirming by simulations that intrinsic FDFs of galaxies can possess meaningful information of galaxies and 