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http://dx.doi.org/10.5303/JKAS.2020.53.6.161

OGLE-2017-BLG-1049: ANOTHER GIANT PLANET MICROLENSING EVENT  

Kim, Yun Hak (Korea Astronomy and Space Science Institute)
Chung, Sun-Ju (Korea Astronomy and Space Science Institute)
Udalski, A. (Warsaw University Observatory)
Bond, Ian A. (Institute of Natural and Mathematical Science, Massey University)
Jung, Youn Kil (Korea Astronomy and Space Science Institute)
Gould, Andrew (Korea Astronomy and Space Science Institute)
Albrow, Michael D. (Department of Physics and Astronomy, University of Canterbury)
Han, Cheongho (Department of Physics, Chungbuk National University)
Hwang, Kyu-Ha (Korea Astronomy and Space Science Institute)
Ryu, Yoon-Hyun (Korea Astronomy and Space Science Institute)
Shin, In-Gu (Korea Astronomy and Space Science Institute)
Shvartzvald, Yossi (Department of Particle Physics and Astrophysics, Weizmann Institute of Science)
Yee, Jennifer C. (Center for Astrophysics - Harvard & Smithsonian)
Zang, Weicheng (Department of Astronomy and Tsinghua Centre for Astrophysics, Tsinghua University)
Cha, Sang-Mok (Korea Astronomy and Space Science Institute)
Kim, Dong-Jin (Korea Astronomy and Space Science Institute)
Kim, Hyoun-Woo (Korea Astronomy and Space Science Institute)
Kim, Seung-Lee (Korea Astronomy and Space Science Institute)
Lee, Chung-Uk (Korea Astronomy and Space Science Institute)
Lee, Dong-Joo (Korea Astronomy and Space Science Institute)
Publication Information
Journal of The Korean Astronomical Society / v.53, no.6, 2020 , pp. 161-168 More about this Journal
Abstract
We report the discovery of a giant exoplanet in the microlensing event OGLE-2017-BLG-1049, with a planet-host star mass ratio of q = 9.53 ± 0.39 × 10-3 and a caustic crossing feature in Korea Microlensing Telescope Network (KMTNet) observations. The caustic crossing feature yields an angular Einstein radius of θE = 0.52 ± 0.11 mas. However, the microlens parallax is not measured because the time scale of the event, tE ≃ 29 days, is too short. Thus, we perform a Bayesian analysis to estimate physical quantities of the lens system. We find that the lens system has a star with mass Mh = 0.55+0.36-0.29 M⊙ hosting a giant planet with Mp = 5.53+3.62-2.87 MJup, at a distance of DL = 5.67+1.11-1.52 kpc. The projected star-planet separation is a⊥ = 3.92+1.10-1.32 au. This means that the planet is located beyond the snow line of the host. The relative lens-source proper motion is μrel ~ 7 mas yr-1, thus the lens and source will be separated from each other within 10 years. After this, it will be possible to measure the flux of the host star with 30 meter class telescopes and to determine its mass.
Keywords
gravitational lensing: micro;
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