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OGLE-2018-BLG-1269Lb: A Jovian Planet with a Bright I = 16 Host

Jung, Youn Kil and Gould, Andrew and Udalski, Andrzej and Sumi, Takahiro and Yee, Jennifer C. and Han, Cheongho and Albrow, Michael D. and Chung, Sun-Ju and Hwang, Kyu-Ha and Ryu, Yoon-Hyun and Shin, In-Gu and Shvartzvald, Yossi and Zhu, Wei 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 Mróz, Przemek and Szymański, Michał K. and Skowron, Jan and Poleski, Radek and Soszyński, Igor and Pietrukowicz, Paweł and Kozłowski, Szymon and Ulaczyk, Krzystof and Rybicki, Krzysztof A. and Iwanek, Patryk and Wrona, Marcin and Abe, Fumio and Barry, Richard and Bennett, David P. and Bond, Ian A. and Bhattacharya, Aparna and Donachie, Martin and Fukui, Akihiko and Hirao, Yuki and Itow, Yoshitaka and Kondo, Iona and Koshimoto, Naoki and Li, Man Cheung Alex and Matsubara, Yutaka and Miyazaki, Shota and Muraki, Yasushi and Nagakane, Masayuki and Ranc, Clément and Rattenbury, Nicholas J. and Suematsu, Haruno and Sullivan, Denis J. and Suzuki, Daisuke and Tristram, Paul J. and Yonehara, Atsunori (2020) OGLE-2018-BLG-1269Lb: A Jovian Planet with a Bright I = 16 Host. Astronomical Journal, 160 (3). Art. No. 148. ISSN 1538-3881.

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We report the discovery of a planet in the microlensing event OGLE-2018-BLG-1269 with a planet–host mass ratio q ~ 6 × 10⁻⁴, i.e., 0.6 times smaller than the Jupiter/Sun mass ratio. Combined with the Gaia parallax and proper motion, a strong one-dimensional constraint on the microlens parallax vector allows us to significantly reduce the uncertainties of lens physical parameters. A Bayesian analysis that ignores any information about light from the host yields that the planet is a cold giant M₂ = (0.69)_(-0.22)^(+0.44) M_J orbiting a Sun-like star M₁ = 1.13_(-0.35)^(+0.72) M_⊙ at a distance of D_L = 2.56_(-0.62)^(+0.92) kpc. The projected planet–host separation is a_⟂ = 4.61_(-1.17)^(+1.70) au. Using Gaia astrometry, we show that the blended light lies ≾ 12 mas from the host and therefore must be either the host star or a stellar companion to the host. An isochrone analysis favors the former possibility at >99.6%. The host is therefore a subgiant. For host metallicities in the range of 0.0 ⩽ [Fe/H] ⩽ +0.3, the host and planet masses are then in the range of 1.16 ⩽ M_₁/M_⊙ ⩽ 1.38 and 0.74 ⩽ M_₂/M_J⩽ 0.89, respectively. Low host metallicities are excluded. The brightness and proximity of the lens make the event a strong candidate for spectroscopic follow-up both to test the microlensing solution and to further characterize the system.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Jung, Youn Kil0000-0002-0314-6000
Udalski, Andrzej0000-0001-5207-5619
Yee, Jennifer C.0000-0001-9481-7123
Han, Cheongho0000-0002-2641-9964
Chung, Sun-Ju0000-0001-6285-4528
Hwang, Kyu-Ha0000-0002-9241-4117
Ryu, Yoon-Hyun0000-0001-9823-2907
Shin, In-Gu0000-0002-4355-9838
Shvartzvald, Yossi0000-0003-1525-5041
Zhu, Wei0000-0003-4027-4711
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
Mróz, Przemek0000-0001-7016-1692
Szymański, Michał K.0000-0002-0548-8995
Skowron, Jan0000-0002-2335-1730
Poleski, Radek0000-0002-9245-6368
Soszyński, Igor0000-0002-7777-0842
Pietrukowicz, Paweł0000-0002-2339-5899
Kozłowski, Szymon0000-0003-4084-880X
Ulaczyk, Krzystof0000-0001-6364-408X
Rybicki, Krzysztof A.0000-0002-9326-9329
Iwanek, Patryk0000-0002-6212-7221
Wrona, Marcin0000-0002-3051-274X
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
Additional Information:© 2020. The American Astronomical Society. Received 2020 June 28; revised 2020 July 26; accepted 2020 August 1; published 2020 September 2. This research has made use of the KMTNet system operated by the Korea Astronomy and Space Science Institute (KASI), and the data were obtained at the three host sites of CTIO in Chile, SAAO in South Africa, and SSO in Australia. A.G. was supported by JPL grant 1500811. Work by C.H. was supported by grants of the National Research Foundation of Korea (2017R1A4A1015178 and 2019R1A2C2085965). The OGLE has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. The MOA project is supported by JSPS KAKENHI grant Nos. JSPS24253004, JSPS26247023, JSPS23340064, JSPS15H00781, JP16H06287, and 19KK0082.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Korea Astronomy and Space Science Institute (KASI)UNSPECIFIED
National Research Foundation of Korea2017R1A4A1015178
National Research Foundation of Korea2019R1A2C2085965
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)JP16H06287
Japan Society for the Promotion of Science (JSPS)JP19KK0082
Subject Keywords:Gravitational microlensing ; Gravitational microlensing exoplanet detection
Issue or Number:3
Classification Code:Unified Astronomy Thesaurus concepts: Gravitational microlensing (672); Gravitational microlensing exoplanet detection (2147)
Record Number:CaltechAUTHORS:20200911-133134585
Persistent URL:
Official Citation:Youn Kil Jung et al 2020 AJ 160 148
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:105335
Deposited By: George Porter
Deposited On:15 Sep 2020 14:26
Last Modified:15 Sep 2020 14:26

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