Ogle-2017-blg-1049: another giant planet microlensing event

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Yun Hak Kim, Sun-Ju Chung, A. Udalski, Ian A. Bond, Youn Kil Jung, Andrew Gould, Michael D. Albrow, Cheongho Han, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Radek Poleski, Przemek Mroz, Jan Skowron, Michal K. Szymanski, Igor Soszynski, Pawel Pietrukowicz, Syzmon Kozlowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Martin Donachie, Hirosane Fujii, Akihiko Fukui, Yoshitaka Itow, Yuki Hirao, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Yasushi Muraki, Shota Miyazaki, Clement Ranc, Nicholas J. Rattenbury, Yuki Satoh, Hikaru Shoji, Takahiro Sumi, Daisuke Suzuki, Paul J. Tristram, Yuzuru Tanaka, Tsubasa Yamawaki, Atsunori Yonehara

We report a giant exoplanet discovery in the microlensing event OGLE-2017-BLG-1049, which is a planet-host star mass ratio of q=9.53±0.39×10−3 and has a caustic crossing feature in the 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 of the time scale of the event tE≃29 days, which is not long enough in this case to determine the microlens parallax. Thus, we perform a Bayesian analysis to estimate physical quantities of the lens system. From this, 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 in units of the Einstein radius (θE) corresponding to the total mass of the lens system 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. Then the flux of the host star can be measured by a 30m class telescope with high-resolution imaging in the future, and thus its mass can be determined.

https://arxiv.org/abs/2012.11080


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