Journal of The Korean Astronomical Society (천문학회지)

The Korean Astronomical Society (한국천문학회)
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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)
  • Received : 2020.09.01
  • Accepted : 2020.12.01
  • Published : 2020.12.31
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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

Acknowledgement

Work by Y. H. Kim was supported by the Korea Astronomy and Space Science Institute (KASI) grant 2020-1-830-08. This research has made use of the KMTNet system operated by KASI and the data were obtained at the three host sites CTIO in Chile, SAAO in South Africa, and SSO in Australia. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to AU. The MOA project was supported by JSPS KAKENHI grant No. JSPS24253004, JSPS26247023, JSPS23340064, JSPS15H00781, JP17H02871, and JP16H06287. This work has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Work by CH was supported by the National Research Foundation of Korea (grants 2017R1A4A1015178 and 2019R1A2C2085965).

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