arXiv 1801.050842018-01-16astro-ph.SR

OGLE-2014-BLG-0289：五峰引力微透镜事件的精确表征

OGLE-2014-BLG-0289: Precise Characterization of a Quintuple-Peak Gravitational Microlensing Event

A. Udalski, C. Han, V. Bozza, A. Gould, I. A. Bond, P. Mróz, J. Skowron, Ł. Wyrzykowski, M. K. Szymański, I. Soszyński, K. Ulaczyk, R. Poleski, P. Pietrukowicz,… 展开作者

A. Udalski, C. Han, V. Bozza, A. Gould, I. A. Bond, P. Mróz, J. Skowron, Ł. Wyrzykowski, M. K. Szymański, I. Soszyński, K. Ulaczyk, R. Poleski, P. Pietrukowicz, S. Kozłowski, F. Abe, R. Barry, D. P. Bennett, A. Bhattacharya, M. Donachie, P. Evans, A. Fukui, Y. Hirao, Y. Itow, K. Kawasaki, N. Koshimoto, M. C. A. Li, C. H. Ling, K. Masuda, Y. Matsubara, S. Miyazaki, H. Munakata, Y. Muraki, M. Nagakane, K. Ohnishi, C. Ranc, N. Rattenbury, T. Saito, A. Sharan, D. J. Sullivan, T. Sumi, D. Suzuki, P. J. Tristram, T. Yamada, A. Yonehara, E. Bachelet, D. M. Bramich, G. DÁgo, M. Dominik, R. Figuera Jaimes, K. Horne, M. Hundertmark, N. Kains, J. Menzies, R. Schmidt, C. Snodgrass, I. A. Steele, J. Wambsganss, R. W. Pogge, Y. K. Jung, I. -G. Shin, J. C. Yee, W. -T. Kim, C. Beichman, S. Carey, S. Calchi Novati, W. Zhu

备注：: 10 pages, 7 figures
DOI：: 10.3847/1538-4357/aaa295

阅读 PDF

arXiv 页面 ↗HTML 原文 ↗

摘要：

我们提出了对二元微透镜事件OGLE-2014-BLG-0289的分析。事件光变曲线呈现出非常不寻常的五个峰，其中四个峰由焦散交叉产生，另一个峰由尖点方法产生。结果发现，光变曲线的五峰功能提供了严格的约束源的轨迹，使我们能够精确和准确地测量微透镜视差$π_{\rm E}$。此外，三个分解焦散线允许我们测量爱因斯坦角半径$\thetae$。根据$π_{\rm E}$和$\thetae$的组合，唯一地确定物理镜片参数。发现该透镜是由质量分别为$M_1 = 0.52 \pm 0.04\ M_\odot$和$M_2=0.42 \pm 0.03\ M_\odot$的两颗M矮星组成的双星，它们在投影上相隔$a_\perp = 6.4 \pm 0.5$ au。透镜位于光盘中，距离为$D_{\rm L} = 3.3 \pm 0.3$ ~kpc。事实证明，在{ \it Spitzer}数据中没有透镜信号的原因是观察时间对应于光变曲线的平坦区域。

英文摘要：

We present the analysis of the binary-microlensing event OGLE-2014-BLG-0289. The event light curve exhibits very unusual five peaks where four peaks were produced by caustic crossings and the other peak was produced by a cusp approach. It is found that the quintuple-peak features of the light curve provide tight constraints on the source trajectory, enabling us to precisely and accurately measure the microlensing parallax $π_{\rm E}$. Furthermore, the three resolved caustics allow us to measure the angular Einstein radius $\thetae$. From the combination of $π_{\rm E}$ and $\thetae$, the physical lens parameters are uniquely determined. It is found that the lens is a binary composed of two M dwarfs with masses $M_1 = 0.52 \pm 0.04\ M_\odot$ and $M_2=0.42 \pm 0.03\ M_\odot$ separated in projection by $a_\perp = 6.4 \pm 0.5$ au. The lens is located in the disk with a distance of $D_{\rm L} = 3.3 \pm 0.3$~kpc. It turns out that the reason for the absence of a lensing signal in the {\it Spitzer} data is that the time of observation corresponds to the flat region of the light curve.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

摘要：

英文摘要：

相关论文