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OGLE-2017-BLG-1049: Another Giant Planet Microlensing Event

Kim, Yun Hak and Chung, Sun-Ju and Udalski, A. and Bond, Ian A. and Jung, Youn Kil and Gould, Andrew and Albrow, Michael D. and Han, Cheongho and Hwang, Kyu-Ha and Ryu, Yoon-Hyun and Shin, In-Gu and Shvartzvald, Yossi and Yee, Jennifer C. and Zang, Weicheng and Cha, Sang-Mok and Kim, Dong-Jin and Kim, Hyoun-Woo and Kim, Seung-Lee and Lee, Chung-Uk and Lee, Dong-Joo and Lee, Yongseok and Park, Byeong-Gon and Pogge, Richard W. and Poleski, Radek and Mróz, Przemek and Skowron, Jan and Szymanski, Michal K. and Soszyński, Igor and Pietrukowicz, Pawel and Kozlowski, Syzmon and Ulaczyk, Krzysztof and Rybicki, Krzysztof A. and Iwanek, Patryk and Abe, Fumio and Barry, Richard and Bennett, David P. and Bhattacharya, Aparna and Donachie, Martin and Fujii, Hirosane and Fukui, Akihiko and Itow, Yoshitaka and Hirao, Yuki and Kirikawa, Rintaro and Kondo, Iona and Koshimoto, Naoki and Matsubara, Yutaka and Muraki, Yasushi and Miyazaki, Shota and Ranc, Clément and Rattenbury, Nicholas J. and Satoh, Yuki and Shoji, Hikaru and Sumi, Takahiro and Suzuki, Daisuke and Tristram, Paul J. and Tanaka, Yuzuru and Yamawaki, Tsubasa and Yonehara, Atsunori (2020) OGLE-2017-BLG-1049: Another Giant Planet Microlensing Event. Journal of the Korean Astronomical Society, 53 (6). pp. 161-168. ISSN 1225-4614.

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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 θ_E = 0.52±0.11 mas. However, the microlens parallax is not measured because the time scale of the event, t_E ≃ 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 M_h = 0.55_(−0.29)^(+0.36) M⊙ hosting a giant planet with M_p = 5.53_(−2.87)^(+3.62) M_(Jup), at a distance of D_L = 5.67_(−1.52)^(+1.11) kpc. The projected star-planet separation is a ⊥ = 3.92_(−1.32)^(+1.10) au. This means that the planet is located beyond the snow line of the host. The relative lens-source proper motion is μ_(rel) ∼ 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.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Chung, Sun-Ju0000-0001-6285-4528
Udalski, A.0000-0001-5207-5619
Jung, Youn Kil0000-0002-0314-6000
Albrow, Michael D.0000-0003-3316-4012
Han, Cheongho0000-0002-2641-9964
Hwang, Kyu-Ha0000-0002-9241-4117
Ryu, Yoon-Hyun0000-0001-9823-2907
Shin, In-Gu0000-0002-4355-9838
Shvartzvald, Yossi0000-0003-1525-5041
Yee, Jennifer C.0000-0001-9481-7123
Zang, Weicheng0000-0001-6000-3463
Cha, Sang-Mok0000-0002-7511-2950
Kim, Hyoun-Woo0000-0001-8263-1006
Kim, Seung-Lee0000-0003-0562-5643
Lee, Chung-Uk0000-0003-0043-3925
Lee, Yongseok0000-0001-7594-8072
Park, Byeong-Gon0000-0002-6982-7722
Pogge, Richard W.0000-0003-1435-3053
Poleski, Radek0000-0002-9245-6368
Mróz, Przemek0000-0001-7016-1692
Skowron, Jan0000-0002-2335-1730
Szymanski, Michal K.0000-0002-0548-8995
Soszyński, Igor0000-0002-7777-0842
Pietrukowicz, Pawel0000-0002-2339-5899
Ulaczyk, Krzysztof0000-0001-6364-408X
Rybicki, Krzysztof A.0000-0002-9326-9329
Iwanek, Patryk0000-0002-6212-7221
Barry, Richard0000-0003-4916-0892
Bennett, David P.0000-0001-8043-8413
Fukui, Akihiko0000-0002-4909-5763
Itow, Yoshitaka0000-0002-8198-1968
Kondo, Iona0000-0002-3401-1029
Koshimoto, Naoki0000-0003-2302-9562
Miyazaki, Shota0000-0001-9818-1513
Ranc, Clément0000-0003-2388-4534
Rattenbury, Nicholas J.0000-0001-5069-319X
Suzuki, Daisuke0000-0002-5843-9433
Yonehara, Atsunori0000-0003-3480-0973
Additional Information:© 2020 Korean Astronomical Society. Published under Creative Commons license CC BY-SA 4.0. Received September 1, 2020; accepted December 1, 2020. 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).
Funding AgencyGrant Number
Korea Astronomy and Space Science Institute (KASI)2020-1-830-08
National Science Centre (Poland)MAESTRO 2014/14/A/ST9/00121
Japan Society for the Promotion of Science (JSPS)JSPS24253004
Japan Society for the Promotion of Science (JSPS)JSPS26247023
Japan Society for the Promotion of Science (JSPS)JSPS23340064
Japan Society for the Promotion of Science (JSPS)JSPS15H00781
Japan Society for the Promotion of Science (JSPS)JP17H02871
Japan Society for the Promotion of Science (JSPS)JP16H06287
National Research Foundation of Korea2017R1A4A1015178
National Research Foundation of Korea2019R1A2C2085965
Subject Keywords:gravitational lensing: micro
Issue or Number:6
Record Number:10.5303/JKAS.2020.53.6.161
Persistent URL:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:107716
Deposited By: Tony Diaz
Deposited On:26 Jan 2021 19:16
Last Modified:26 Jan 2021 19:16

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