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OGLE-2016-BLG-0523: A Low-mass Brown Dwarf or Super-Jupiter in a >100 au Orbit

  • Authors: Hongjing Yang, 弘靖 杨, Weicheng Zang, 伟呈 臧, Yoon-Hyun Ryu, Andrzej Udalski, Yuchen Tang, 雨辰 唐, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, 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, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radoslaw Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Mateusz J. Mróz, Jiyuan Zhang, 纪元 张, Shude Mao, 淑德 毛, Hongyu Li, 弘禹 李, Qiyue Qian, 奇玥 钱

Hongjing Yang et al 2026 The Astrophysical Journal Letters 1011 .

  • Provider: AAS Journals

Caption: Figure D1.

The proper motions of the source star and field stars within a ﹩1\mathop{.}\limits^{{\rm{^{\prime} }}}5﹩ radius are shown. The proper motions of the field stars are measured using Gaia DR3. The source star, indicated by the orange dot, has no proper-motion measurement in Gaia DR3, and its value is derived from the OGLE-URANUS astrometry database (Udalski et al. 2026, in preparation). Red-clump (RC) stars are shown as black dots, and their mean proper motion is indicated by the red dot. The RC mean proper motion is (μα, μδ) = (−2.91 ± 0.12, −5.34 ± 0.12) mas yr−1, and the source proper motion is (μα, μδ) = (−4.91 ± 0.24, −7.21 ± 0.17) mas yr−1.

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