  Dispersion measure (DM) of Fast Radio Bursts (FRBs) are commonly used as a
indicator of distance assuming that DM in excess of the expected amount within
the Milky Way in the direction of each FRB arise mostly from the inter-galactic
medium. However, the assumption might not be true if, for example, most FRB
progenitors are embedded in ionized circumstellar material (CSM, e.g. supernova
remnant). In this study, we jointly analyze distributions of DM, flux density,
and fluence of the FRB samples observed by the Parkes telescope and the
Australian Square Kilometre Array Pathfinder (ASKAP) using analytical models of
FRBs, to constrain fractions of various DM components that shape the overall DM
distribution and emission properties of FRBs. Comparing the model predictions
with the observations we find that the typical amount of DM in each FRB host
galaxy is $\sim 120$ cm$^{-3}$pc which is naturally explained as a combination
of interstellar medium (ISM) and halo of an ordinary galaxy, without additional
contribution from ionized CSM that is directly associated with an FRB
progenitor. Furthermore, we also find that observed flux densities of FRBs do
not statistically suffer strong $K$-correction, i.e. the typical luminosity
density of FRBs does not significantly change within the range of emitting
frequency $\nu_{\rm rest} \sim$ 1--4 GHz.
