arXiv 2003.011262020-03astro-ph.EPastro-ph.GAastro-ph.IMastro-ph.SR

微透镜事件OGLE-2019-BLG-0551中的自由漂浮或宽轨道行星

A free-floating or wide-orbit planet in the microlensing event OGLE-2019-BLG-0551

P. Mroz, R. Poleski, C. Han, A. Udalski, A. Gould, M. K. Szymanski, I. Soszynski, P. Pietrukowicz, S. Kozlowski, J. Skowron, K. Ulaczyk, M. Gromadzki, K. Rybick… 展开作者

P. Mroz, R. Poleski, C. Han, A. Udalski, A. Gould, M. K. Szymanski, I. Soszynski, P. Pietrukowicz, S. Kozlowski, J. Skowron, K. Ulaczyk, M. Gromadzki, K. Rybicki, P. Iwanek, M. Wrona, M. D. Albrow, S. Chung, K. Hwang, Y. Ryu, Y. K. Jung, I. Shin, Y. Shvartzvald, J. C. Yee, W. Zang, S. Cha, D. Kim, H. Kim, S. Kim, C. Lee, D. Lee, Y. Lee, B. Park, R. W. Pogge

备注：: accepted for publication in AJ, minor changes
发表信息：: AJ 159, 6 (2020)
DOI：: 10.3847/1538-3881/ab8aeb

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摘要：

微透镜巡天对银河系隆起的高节奏观测导致了少数极短时间尺度的微透镜事件的发现，这些事件可以归因于自由浮动或宽轨道行星。在这里，我们报告了另一个强大的自由浮动行星候选者的发现，这是从引力微透镜事件OGLE-2019-BLG-0551的分析中发现的。该事件的光变曲线的特征是持续时间很短（<3天），振幅很小（< 0.1等）。通过对光变曲线的模拟，我们发现爱因斯坦时标tE = 0.381 +/- 0.017 d，比恒星质量透镜产生的典型透镜事件的爱因斯坦时标tE = 0.381 +/- 0.017 d要短得多，爱因斯坦角半径θ E = 4.35 +/- 0.34 uas也要小得多（tE ~ 20 d，θ E ~ 0.3 mas），表明透镜很可能是一个行星质量的物体。我们进行了广泛的搜索，在事件的光变曲线中寻找伴星的可能签名，没有发现推定的宿主星的重要证据。我们还首次证明了在具有强有限源效应的低放大率事件中，透镜的爱因斯坦角半径不依赖于混合。

英文摘要：

High-cadence observations of the Galactic bulge by the microlensing surveys led to the discovery of a handful of extremely short-timescale microlensing events that can be attributed to free-floating or wide-orbit planets. Here, we report the discovery of another strong free-floating planet candidate, which was found from the analysis of the gravitational microlensing event OGLE-2019-BLG-0551. The light curve of the event is characterized by a very short duration (<3 d) and a very small amplitude (< 0.1 mag). From modeling of the light curve, we find that the Einstein timescale, tE = 0.381 +/- 0.017 d, is much shorter, and the angular Einstein radius, thetaE = 4.35 +/- 0.34 uas, is much smaller than those of typical lensing events produced by stellar-mass lenses (tE ~ 20 d, thetaE ~ 0.3 mas), indicating that the lens is very likely to be a planetary-mass object. We conduct an extensive search for possible signatures of a companion star in the light curve of the event, finding no significant evidence for the putative host star. For the first time, we also demonstrate that the angular Einstein radius of the lens does not depend on blending in the low-magnification events with strong finite source effects.

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