the Hubble Space Telescope images, to constrain the parameters of OGLE-2005-BLG-071Lb, which was discovered by @udalski05. @dong09a concluded that the $3.8 \pm 0.4~M_{\rm Jup}$ mass planet orbits an $M = 0.46\pm0.04~M_{\odot}$ star and lies at projected separation of $3.6\pm0.2~{\rm AU}$. @batista11 analyzed the MOA-2009-BLG-387 event. The projected separation of the planet and the star was comparable to the size of the Einstein ring, which resulted in a very large resonant caustic. This allowed a very precise measurement of the mass ratio $q = 0.0132 \pm 0.003$ with most probable planet and host masses of $2.6~M_{\rm Jup}$ and $0.19~M_{\odot}$, respectively. The estimated projected separation is $1.8~{\rm AU}$. There are two more microlensing planets that were claimed to be super-Jupiters orbiting low-mass stars beyond the snow-line based on Bayesian analysis, not the direct measurement of lens mass from microlensing model: OGLE-2003-BLG-235Lb [@bond04; @bennett06] and MOA-2011-BLG-293Lb [@yee12]. Both events were observed with high spatial resolution, and these observations neglected the results of Bayesian analysis in the latter case [@batista13]. We note that @street12 found a planetary mass object MOA-2010-BLG-073Lb ($11~M_{\rm Jup}$) orbiting an M-dwarf beyond the snow line, but they concluded that it is most likely extremely low-mass product of star formation.

The 