arXiv 2102.073382021-02-15astro-ph.EPastro-ph.GA

OGLE-2018-BLG-0567 Lb和OGLE-2018-BLG-0962 Lb：通过行星焦散通道的两颗微透镜行星

OGLE-2018-BLG-0567Lb and OGLE-2018-BLG-0962Lb: Two Microlensing Planets through Planetary-Caustic Channel

Youn Kil Jung, Cheongho Han, Andrzej Udalski, Andrew Gould, Jennifer C. Yee, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shv… 展开作者

Youn Kil Jung, Cheongho Han, Andrzej Udalski, Andrew Gould, Jennifer C. Yee, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Wei Zhu, Weicheng Zang, 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, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzystof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona

备注：: 25 pages, 8 figures, 4 tables, submitted to AAS journal
DOI：: 10.3847/1538-3881/abf8bd

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摘要：

我们介绍了对两个微透镜事件OGLE-2018-BLG-0567和OGLE-2018-BLG-0962的分析。在这两个事件中，短暂的异常密集和连续覆盖的两个高节奏的调查。光变曲线模拟表明，这些异常是由行星伴星与宿主星之间的源交叉引起的行星焦散线产生的。估计的行星/宿主分离（换算成爱因斯坦角半径$θ_{\rm E}$）和质量比分别为$(s, q) = (1.81, 1.24\times10^{-3})$和$(s, q) = (1.25, 2.38\times10^{-3})$。从贝叶斯分析，我们估计的主机和行星质量为$(M_{\rm h}, M_{\rm p}) = (0.24_{-0.13}^{+0.16}\,M_{\odot}, 0.32_{-0.16}^{+0.34}\,M_{\rm J})$和$(M_{\rm h}, M_{\rm p}) = (0.55_{-0.29}^{+0.32}\,M_{\odot}, 1.37_{-0.72}^{+0.80}\,M_{\rm J})$，分别。这些行星系位于OGLE-2018-BLG-0567的$7.07_{-1.15}^{+0.93}\,{\rm kpc}$和OGLE-2018-BLG-0962的$6.47_{-1.73}^{+1.04}\,{\rm kpc}$之间，这表明它们很可能靠近银河系凸起。这两个事件证明了当前高节奏调查通过行星焦散通道寻找行星的能力。我们发现，大多数已发表的行星式焦散行星都是在好莱坞事件中发现的，其中源大小对相对于焦散大小的异常截面有很大贡献。

英文摘要：

We present the analyses of two microlensing events, OGLE-2018-BLG-0567 and OGLE-2018-BLG-0962. In both events, the short-lasting anomalies were densely and continuously covered by two high-cadence surveys. The light-curve modeling indicates that the anomalies are generated by source crossings over the planetary caustics induced by planetary companions to the hosts. The estimated planet/host separation (scaled to the angular Einstein radius $θ_{\rm E}$) and mass ratio are $(s, q) = (1.81, 1.24\times10^{-3})$ and $(s, q) = (1.25, 2.38\times10^{-3})$, respectively. From Bayesian analyses, we estimate the host and planet masses as $(M_{\rm h}, M_{\rm p}) = (0.24_{-0.13}^{+0.16}\,M_{\odot}, 0.32_{-0.16}^{+0.34}\,M_{\rm J})$ and $(M_{\rm h}, M_{\rm p}) = (0.55_{-0.29}^{+0.32}\,M_{\odot}, 1.37_{-0.72}^{+0.80}\,M_{\rm J})$, respectively. These planetary systems are located at a distance of $7.07_{-1.15}^{+0.93}\,{\rm kpc}$ for OGLE-2018-BLG-0567 and $6.47_{-1.73}^{+1.04}\,{\rm kpc}$ for OGLE-2018-BLG-0962, suggesting that they are likely to be near the Galactic bulge. The two events prove the capability of current high-cadence surveys for finding planets through the planetary-caustic channel. We find that most published planetary-caustic planets are found in Hollywood events in which the source size strongly contributes to the anomaly cross section relative to the size of the caustic.

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