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We report the discovery of a sub-Jupiter mass planet orbiting beyond the snowline of an M-dwarf most likely in the Galactic disk as part of the jointSpitzer and ground-based monitoring of microlensing planetary anomalies towardthe Galactic bulge. The microlensing parameters are strongly constrained by thelight curve modeling and in particular by the Spitzer-based measurement of themicrolens parallax, $\pi_\mathrm{E}$. However, in contrast to many planetarymicrolensing events, there are no caustic crossings, so the angular Einsteinradius, $\theta_\mathrm{E}$ has only an upper limit based on the light curvemodeling alone. Additionally, the analysis leads us to identify 8 degenerateconfigurations: the four-fold microlensing parallax degeneracy being doubled bya degeneracy in the caustic structure present at the level of the ground-basedsolutions. To pinpoint the physical parameters, and at the same time to breakthe parallax degeneracy, we make use of a series of arguments: the $\chi^2$hierarchy, the Rich argument, and a prior Galactic model. The preferredconfiguration is for a host at $D_L=3.73_{-0.67}^{+0.66}~\mathrm{kpc}$ withmass $M_\mathrm{L}=0.30_{-0.12}^{+0.15}~\mathrm{M_\odot}$, orbited by aSaturn-like planet with$M_\mathrm{planet}=0.43_{-0.17}^{+0.21}~\mathrm{M_\mathrm{Jup}}$ at projectedseparation $a_\perp = 1.70_{-0.39}^{+0.38}~\mathrm{au}$, about 2.1 times beyondthe system snow line. Therefore, it adds to the growing population ofsub-Jupiter planets orbiting near or beyond the snow line of M-dwarfsdiscovered by microlensing. Based on the rules of the real-time protocol forthe selection of events to be followed up with Spitzer, this planet will notenter the sample for measuring the Galactic distribution of planets.

Spitzer Microlensing Parallax for OGLE-2016-BLG-1067: a sub-Jupiter Orbiting an M-dwarf in the Disk