arXiv 2109.022092021-09-06astro-ph.EPastro-ph.GAastro-ph.IMastro-ph.SR

OGLE-2019-BLG-0304：行星双星模型和双星源+双星透镜模型之间的竞争解释

OGLE-2019-BLG-0304: Competing Interpretations between a Planet-binary Model and a Binary-source + Binary-lens model

Cheongho Han, Andrzej Udalski, Chung-Uk Lee, Doeon Kim, Yoon-Hyun Ryu, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Hyoun-Woo Kim… 展开作者

Cheongho Han, Andrzej Udalski, Chung-Uk Lee, Doeon Kim, Yoon-Hyun Ryu, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Hyoun-Woo Kim, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki

备注：: 11 pages, 3 tables, 11 figures
DOI：: 10.3847/1538-3881/ac1c09

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摘要：

我们分析了微透镜事件OGLE-2019-BLG-0304，其光变曲线表现出两个独特的特征：峰值区域的偏差和主峰后$\sim 61$ ~天出现的第二个凸起。虽然二元透镜模型可以解释整体特征，但它在峰值区域留下了微妙但明显的残差。我们发现，残差可以解释的存在下，无论是位于接近的主要的双透镜（3L 1 S模型）或一个额外的近伴星的源（2L 2S模型）的行星伴侣。虽然3L 1 S模型优于2L 2S模型，但使用$Δχ^2\sim 8$，使用当前可用的光度数据很难安全地解决两个模型之间的简并性。根据3L 1 S的解释，透镜是一个行星系，其中一颗质量为$0.51^{+0.51}_{-0.23}~M_{\rm J}$的行星围绕一个由质量为$0.27^{+0.27}_{-0.12}~M_\odot$和$0.10^{+0.10}_{-0.04}~M_\odot$的恒星组成的双星运行。另一方面，根据2L 2S的解释，源由G-和K-型巨星组成，透镜由质量分别为$0.12^{+0.12}_{-0.05}~M_\odot$和$0.045^{+0.045}_{-.019}~M_\odot$的低质量M矮星和棕矮星组成。该事件说明了通过模型测试来解释具有复杂光变曲线特征的透镜事件的必要性。

英文摘要：

We analyze the microlensing event OGLE-2019-BLG-0304, whose light curve exhibits two distinctive features: a deviation in the peak region and a second bump appearing $\sim 61$~days after the main peak. Although a binary-lens model can explain the overall features, it leaves subtle but noticeable residuals in the peak region. We find that the residuals can be explained by the presence of either a planetary companion located close to the primary of the binary lens (3L1S model) or an additional close companion to the source (2L2S model). Although the 3L1S model is favored over the 2L2S model, with $Δχ^2\sim 8$, securely resolving the degeneracy between the two models is difficult with the currently available photometric data. According to the 3L1S interpretation, the lens is a planetary system, in which a planet with a mass $0.51^{+0.51}_{-0.23}~M_{\rm J}$ is in an S-type orbit around a binary composed of stars with masses $0.27^{+0.27}_{-0.12}~M_\odot$ and $0.10^{+0.10}_{-0.04}~M_\odot$. According to the 2L2S interpretation, on the other hand, the source is composed of G- and K-type giant stars, and the lens is composed of a low-mass M dwarf and a brown dwarf with masses $0.12^{+0.12}_{-0.05}~M_\odot$ and $0.045^{+0.045}_{-.019}~M_\odot$, respectively. The event illustrates the need for through model testing in the interpretation of lensing events with complex features in light curves.

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