August
2020
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2020AJ....160...74H
Authors
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Hirao, Yuki
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Bennett, David P.
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Ryu, Yoon-Hyun
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Koshimoto, Naoki
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Udalski, Andrzej
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Yee, Jennifer C.
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Sumi, Takahiro
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Bond, Ian A.
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Shvartzvald, Yossi
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Abe, Fumio
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Barry, Richard K.
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Bhattacharya, Aparna
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Donachie, Martin
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Fukui, Akihiko
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Itow, Yoshitaka
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Kondo, Iona
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Li, Man Cheung Alex
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Matsubara, Yutaka
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Matsuo, Taro
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Miyazaki, Shota
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Muraki, Yasushi
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Nagakane, Masayuki
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Ranc, Clément
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Rattenbury, Nicholas J.
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Suematsu, Haruno
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Shibai, Hiroshi
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Suzuki, Daisuke
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Tristram, Paul J.
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Yonehara, Atsunori
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MOA Collaboration
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Skowron, J.
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Poleski, R.
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Mróz, P.
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Szymański, M. K.
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Soszyński, I.
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Kozłowski, S.
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Pietrukowicz, P.
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Ulaczyk, K.
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Rybicki, K.
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Iwanek, P.
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OGLE Collaboration
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Albrow, Michael D.
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Chung, Sun-Ju
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Gould, Andrew
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Han, Cheongho
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Hwang, Kyu-Ha
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Jung, Youn Kil
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Shin, In-Gu
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Zang, Weicheng
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Cha, Sang-Mok
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Kim, Dong-Jin
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Kim, Hyoun-Woo
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Kim, Seung-Lee
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Lee, Chung-Uk
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Lee, Dong-Joo
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Lee, Yongseok
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Park, Byeong-Gon
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Pogge, Richard W.
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KMTNet Collaboration
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Beichman, Charles A.
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Bryden, Geoffery
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Novati, Sebastiano Calchi
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Carey, Sean
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Gaudi, B. Scott
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Henderson, Calen B.
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Zhu, Wei
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Spitzer Team
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Bachelet, Etienne
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Bolt, Greg
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Christie, Grant
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Hundertmark, Markus
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Natusch, Tim
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Maoz, Dan
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McCormick, Jennie
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Street, Rachel A.
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Tan, Thiam-Guan
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Tsapras, Yiannis
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LCO and μFUN Follow-up Teams
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Jørgensen, U. G.
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Dominik, M.
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Bozza, V.
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Skottfelt, J.
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Snodgrass, C.
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Ciceri, S.
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Jaimes, R. Figuera
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Evans, D. F.
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Peixinho, N.
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Hinse, T. C.
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Burgdorf, M. J.
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Southworth, J.
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Rahvar, S.
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Sajadian, S.
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Rabus, M.
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von Essen, C.
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Fujii, Y. I.
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Campbell-White, J.
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Lowry, S.
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Helling, C.
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Mancini, L.
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Haikala, L.
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MindSTEp Collaboration
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Kandori, Ryo
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IRSF Team
Abstract
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We report the discovery and analysis of the planetary microlensing event OGLE-2017-BLG-0406, which was observed both from the ground and by the Spitzer satellite in a solar orbit. At high magnification, the anomaly in the light curve was densely observed by ground-based-survey and follow-up groups, and it was found to be explained by a planetary lens with a planet/host mass ratio of $q=7.0\times {10}^{-4}$ from the light-curve modeling. The ground-only and Spitzer-"only" data each provide very strong one-dimensional (1D) constraints on the 2D microlens parallax vector ${{\boldsymbol{\pi }}}_{{\rm{E}}}$ . When combined, these yield a precise measurement of ${{\boldsymbol{\pi }}}_{{\rm{E}}}$ and of the masses of the host ${M}_{\mathrm{host}}=0.56\pm 0.07\,{M}_{\odot }$ and planet Mplanet = 0.41 ± 0.05 MJup. The system lies at a distance DL = 5.2 ± 0.5 kpc from the Sun toward the Galactic bulge, and the host is more likely to be a disk population star according to the kinematics of the lens. The projected separation of the planet from the host is ${a}_{\perp }=3.5\pm 0.3\,\mathrm{au}$ (i.e., just over twice the snow line). The Galactic-disk kinematics are established in part from a precise measurement of the source proper motion based on OGLE-IV data. By contrast, the Gaia proper-motion measurement of the source suffers from a catastrophic 10σ error.
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