  We measure the dependence of planet frequency on host star mass, $M_{\rm L}$,
and distance from the Galactic center, $R_{\rm L}$, using a sample of planets
discovered by gravitational microlensing. We compare the two-dimensional
distribution of the lens-source proper motion, $\mu_{\rm rel}$, and the
Einstein radius crossing time, $t_{\rm E}$, measured for 22 planetary events
from Suzuki et al. (2016) with the distribution expected from Galactic model.
Assuming that the planet-hosting probability of a star is proportional to
$M_{\rm L}^m R_{\rm L}^r$, we calculate the likelihood distribution of $(m,r)$.
We estimate that $r = 0.10^{+0.51}_{-0.37}$ and $m = 0.50^{+0.90}_{-0.70}$
under the assumption that the planet-hosting probability is independent of the
mass ratio. We also divide the planet sample into subsamples based on their
mass ratio, $q$, and estimate that $m=-0.08^{+0.95}_{-0.65}$ for $q < 10^{-3}$
and $1.25^{+1.07}_{-1.14}$ for $q > 10^{-3}$. Although uncertainties are still
large, this result implies a possibility that in orbits beyond the snowline,
massive planets are more likely to exist around more massive stars whereas
low-mass planets exist regardless of their host star mass.
