  Dark matter halos of dwarf spheroidal galaxies (dSphs) play important roles
in dark matter detection. Generally we estimate the halo profile using a
kinematical equation of dSphs but the halo profile has a large uncertainty
because we have only a limited number of kinematical dataset. In this paper, we
utilize cosmological models of dark matter subhalos to obtain better
constraints on halo profile of dSphs. The constraints are realized as two
cosmological priors: satellite prior, based on a semi-analytic model of the
accretion history of subhalos and their tidal stripping effect, and
stellar-to-halo mass relation prior, which estimates halo mass of a galaxy from
its stellar mass using empirical correlations. In addition, we adopt a radial
dependent likelihood function by considering velocity dispersion profile, which
allows us to mitigate the parameter degeneracy in the previous analysis using a
radial independent likelihood function with averaged dispersion. Using these
priors, we estimate the squared dark matter density integrated over the
region-of-interest (so-called $J$-factor) of 8 classical and 27 ultra-faint
dSphs. Our method significantly decreases the uncertainty of $J$-factors (upto
about $20\%$) compared to the previous radial independent analysis. We confirm
the model dependence of $J$-factor estimates by evaluating Bayes factors of
different model setups and find that the estimates are still stable even when
assuming different cosmological models.
