OGLE-2016-BLG-1093Lb: A Sub-Jupiter-mass Spitzer Planet Located in the Galactic Bulge

Creators: Shin, In-Gu; Yee, Jennifer C.; Hwang, Kyu-Ha; Gould, Andrew; Udalski, Andrzej; Bond, Ian A.; Albrow, Michael D.; Chung, Sun-Ju; Han, Cheongho; Kil Jung, Youn; Woo Kim, Hyoun; Ryu, Yoon-Hyun; Shvartzvald, Yossi; Zang, Weicheng; Cha, Sang-Mok; Kim, Dong-Jin; Kim, Seung-Lee; Lee, Chung-Uk; Lee, Dong-Joo; Lee, Yongseok; Park, Byeong-Gon; Pogge, Richard W.; Mróz, Przemek; Szymański, Michał K.; Skowron, Jan; Poleski, Radek; Soszyński, Igor; Pietrukowicz, Paweł; Kozłowski, Szymon; Ulaczyk, Krzysztof; Beichman, Charles A.; Bryden, Geoffery; Calchi Novati, Sebastiano; Carey, Sean; Gaudi, B. Scott; Henderson, Calen B.; Zhu, Wei; Abe, Fumio; Barry, Richard K.; Bennett, David P.; Bhattacharya, Aparna; Fujii, Hirosane; Fukui, Akihiko; Hirao, Yuki; Itow, Yoshitaka; Kirikawa, Rintaro; Koshimoto, Naoki; Kondo, Iona; Matsubara, Yutaka; Matsumoto, Sho; Miyazaki, Shota; Muraki, Yasushi; Olmschenk, Greg; Okamura, Arisa; Ranc, Clément; Rattenbury, Nicholas J.; Satoh, Yuki; Silva, Stela Ishitani; Sumi, Takahiro; Suzuki, Daisuke; Toda, Taiga; Tristram, Paul J.; Vandorou, Aikaterini; Yama, Hibiki; MOA Collaboration; KMTNet Collaboration; OGLE Collaboration; Spitzer Team

Abstract

OGLE-2016-BLG-1093 is a planetary microlensing event that is part of the statistical Spitzer microlens parallax sample. The precise measurement of the microlens parallax effect for this event, combined with the measurement of finite-source effects, leads to a direct measurement of the lens masses and system distance, M_(host) =0.38–0.57 M_⊙ and m_p = 0.59–0.87 M_(Jup), and the system is located at the Galactic bulge (D_L ∼ 8.1 kpc). Because this was a high-magnification event, we are also able to empirically show that the "cheap-space parallax" concept produces well-constrained (and consistent) results for ∣π_E∣. This demonstrates that this concept can be extended to many two-body lenses. Finally, we briefly explore systematics in the Spitzer light curve in this event and show that their potential impact is strongly mitigated by the color constraint.

Additional Information

© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2022 January 6; revised 2022 March 10; accepted 2022 April 6; published 2022 May 10. 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 three host sites of CTIO in Chile, SAAO in South Africa, and SSO in Australia. Work by C.H. was supported by grants of the National Research Foundation of Korea (2017R1A4A1015178 and 2019R1A2C2085965). J.C.Y. acknowledges support from N.S.F grant No. AST–2108414 and JPL grant 1571564. The MOA project is supported by JSPS KAKENHI grant Nos. JSPS24253004, JSPS26247023, JSPS23340064, JSPS15H00781, JP16H06287, 17H02871, and 19KK0082.

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