Spitzer Microlensing Parallax for OGLE-2016-BLG-1067: a sub-Jupiter Orbiting an M-dwarf in the Disk
Creators: name: Novati, S. Calchi
name: Suzuki, D.
name: Udalski, A.
name: Gould, A.
name: Shvartzvald, Y.
name: Bozza, V.
name: Bennett, D. P.
name: Beichman, C.
name: Bryden, G.
name: Carey, S.
name: Gaudi, B. S.
name: Henderson, C. B.
name: Yee, J. C.
name: Zhu, W.
name: Abe, F.
name: Asakura, Y.
name: Barry, R.
name: Bhattacharya, A.
name: Bond, I. A.
name: Donachie, M.
name: Evans, P.
name: Fukui, A.
name: Hirao, Y.
name: Itow, Y.
name: Kawasaki, K.
name: Koshimoto, N.
name: Li, M. C. A.
name: Ling, C. H.
name: Matsubara, Y.
name: Miyazaki, S.
name: Muraki, Y.
name: Nagakane, M.
name: Ohnishi, K.
name: Ranc, C.
name: Rattenbury, N. J.
name: Saito, To.
name: Sharan, A.
name: Sullivan, D. J.
name: Sumi, T.
name: Tristram, P. J.
name: Yamada, T.
name: Yonehara, A.
name: Mróz, P.
name: Poleski, R.
name: Skowron, J.
name: Szymański, M. K.
name: Soszyński, I.
name: Kozłowski, S.
name: Pietrukowicz, P.
name: Ulaczyk, K.
name: Pawlak, M.
name: Albrow, M. D.
name: Chung, S. -J.
name: Han, C.
name: Hwang, K. -H.
name: Jung, Y. K.
name: Ryu, Y. -H.
name: Shin, I. -G.
name: Zang, W.
name: Cha, S. -M.
name: Kim, D. -J.
name: Kim, H. -W.
name: Kim, S. -L.
name: Lee, C. -U.
name: Lee, D. -J.
name: Lee, Y.
name: Park, B. -G.
name: Pogge, R. W.
Publisher: name: arXiv
Year: 2018
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: 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 microlensing planetary anomalies toward the Galactic bulge. The microlensing parameters are strongly constrained by the light curve modeling and in particular by the Spitzer-based measurement of the microlens parallax, $π_\mathrm{E}$. However, in contrast to many planetary microlensing events, there are no caustic crossings, so the angular Einstein radius, $θ_\mathrm{E}$ has only an upper limit based on the light curve modeling alone. Additionally, the analysis leads us to identify 8 degenerate configurations: the four-fold microlensing parallax degeneracy being doubled by a degeneracy in the caustic structure present at the level of the ground-based solutions. To pinpoint the physical parameters, and at the same time to break the parallax degeneracy, we make use of a series of arguments: the $χ^2$ hierarchy, the Rich argument, and a prior Galactic model. The preferred configuration is for a host at $D_L=3.73_{-0.67}^{+0.66}~\mathrm{kpc}$ with mass $M_\mathrm{L}=0.30_{-0.12}^{+0.15}~\mathrm{M_\odot}$, orbited by a Saturn-like planet with $M_\mathrm{planet}=0.43_{-0.17}^{+0.21}~\mathrm{M_\mathrm{Jup}}$ at projected separation $a_\perp = 1.70_{-0.39}^{+0.38}~\mathrm{au}$, about 2.1 times beyond the system snow line. Therefore, it adds to the growing population of sub-Jupiter planets orbiting near or 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.
description: Submitted to AAS Journals