Spitzer Microlensing Parallax for OGLE-2016-BLG-1067: A Sub-Jupiter Orbiting an M Dwarf in the Disk

We report the discovery of a sub-Jupiter-mass planet orbiting beyond the snow line of an M dwarf most likely in the Galactic disk as part of the joint Spitzer and ground-based monitoring of planetary microlensing anomalies toward the Galactic bulge. Most of the microlensing parameters are strongly constrained by the light-curve modeling, and in particular there is a Spitzer-based measurement of the microlens parallax, π <SUB>E</SUB>. However, there are no caustic crossings, so the angular Einstein radius has only an upper limit based on the light-curve modeling alone. Additionally, the analysis leads us to identify eight degenerate configurations: the fourfold microlensing parallax degeneracy being doubled by a degeneracy in the caustic structure present at the level of the ground-based solutions. To calculate the physical parameters, and at the same time to break the parallax degeneracy, we make use of a series of arguments: the χ <SUP>2</SUP> hierarchy, the Rich argument (stating that the small-parallax solution is more likely), and a prior Galactic model. The preferred configuration, favored by a likelihood ratio of at least 4000, is for a host at {D}<SUB>L</SUB>={3.73}<SUB>-0.67</SUB><SUP>+0.66</SUP> {kpc} with mass {M}<SUB>{{L</SUB>}}={0.30}<SUB>-0.12</SUB><SUP>+0.15</SUP> {M}<SUB>⊙ </SUB>, orbited by a Saturn-like planet with {M}<SUB>planet</SUB>} ={0.43}<SUB>-0.17</SUB><SUP>+0.21</SUP> {M}<SUB>Jup</SUB>} at projected separation {a}<SUB>\perp </SUB>={1.70}<SUB>-0.39</SUB><SUP>+0.38</SUP> {au}, about 2.1 times beyond the system snow line. Therefore, it adds to the growing population of sub-Jupiter planets orbiting beyond the snow line of M dwarfs discovered by microlensing. Based on the rules of the real-time protocol for the selection of events to be followed up with Spitzer, this planet will not enter the sample for measuring the Galactic distribution of planets.