Spitzer Parallax of OGLE-2018-BLG-0596: A Low-mass-ratio Planet around an M Dwarf

We report the discovery of a Spitzer microlensing planetOGLE-2018-BLG-0596Lb, with preferred planet-host mass ratio q ~ 2 × 10^(−4). The planetary signal, which is characterized by a short (~1 day) "bump" on the rising side of the lensing light curve, was densely covered by ground-based surveys. We find that the signal can be explained by a bright source that fully envelops the planetary caustic, i.e., a "Hollywood" geometry. Combined with the source proper motionmeasured from Gaia, the Spitzer satellite parallaxmeasurement makes it possible to precisely constrain the lens physical parameters. The preferred solution, in which the planetperturbs the minor image due to lensing by the host, yields a Uranus-mass planetwith a mass of M_p = 13.9 ± 1.6 M⊕ orbiting a mid M-dwarf with a mass of M_h = 0.23 ± 0.03 M⊙. There is also a second possible solution that is substantially disfavored but cannot be ruled out, for which the planetperturbs the major image. The latter solution yields M_p = 1.2 ± 0.2 M⊕ and M_h = 0.15 ± 0.02 M⊙. By combining the microlensing and Gaia data together with a Galactic model, we find in either case that the lens lies on the near side of the Galactic bulge at a distance D_L ~ 6 ± 1 kpc. Future adaptive optics observations may decisively resolve the major image/minor image degeneracy.