On the other hand, although 68% confidence intervals are mostly overlapped with each other in the probability distribution of skewness and kurtosis, for Model 2, these quantities are limited to relatively narrow ranges. The skewness for Model 2 tends to be negative and this is due to the orientation of coherent vertical magnetic fields.

Summary and Discussion {#section:4}
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In this paper, we calculated the Faraday dispersion function (FDF) of face-on spiral galaxies, which represents the distribution of the polarized intensity as a function of Faraday depth, using realistic galactic models [@arkg13] which are based on observational data and numerical simulations of turbulence. FDFs reflect the distribution of magnetic fields and thermal and cosmic-ray electrons and can be a useful tool to probe galaxies. However, in general, FDFs do not have one-to-one correspondence with the distribution of the polarized intensity in physical space and are not easy to give a direct interpretation. Further, the shape of FDFs varies significantly for different configurations of turbulence, even if we fix the global parameters of the galactic model such as the mean amplitude and correlation length of magnetic fields and the scale heights of thermal and cosmic-ray electron number densities. We, especially, focused 