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Gravitational microlensing is currently the only technique that helps studythe Galactic distribution of planets as a function of distance from theGalactic center. The Galactic location of a lens system can be uniquelydetermined only when at least two of the three quantities that determine themass--distance relations are measured. However, even if only one mass--distancerelation can be obtained, a large sample of microlensing events can be used tostatistically discuss the Galactic distribution of the lenses. In this study,we extract the Galactic distribution of planetary systems from the distributionof the lens-source proper motion, $\mu_{\rm rel}$, for a given Einstein radiuscrossing time, $t_{\rm E}$, measured for the 28 planetary events in thestatistical sample by Suzuki et al. (2016). Because microlensing is randomlycaused by stars in our Galaxy, the observational distribution can be predictedusing a Galactic model. We incorporate the planet-hosting probability, $P_{\rmhost} \propto M_{\rm L}^m R_{\rm L}^r$, into a Galactic model forrandom-selected stars, where $M_{\rm L}$ is the lens mass ($\sim$ host mass),and $R_{\rm L}$ is the Galactocentric distance. By comparing the observeddistribution with the model-predicted $\mu_{\rm rel}$ distribution for a given$t_{\rm E}$ at various combinations of $(m ,r)$, we obtain an estimate $r = 0.2\pm 0.4$ under a plausible uniform prior for $m$ of $0<m<2$. This indicatesthat the dependence of the planet frequency on the Galactocentric distance isnot large, and suggests that the Galactic bulge does have planets.

No Large Dependence of Planet Frequency on Galactocentric Distance