发表机构
University of Maryland; NASA Goddard Space Flight Center; University of Tasmania; Universität Bern; Massey University; University of Warsaw（马里兰大学; 美国国家航空航天局戈达德太空飞行中心; 塔斯马尼亚大学; 伯尔尼大学; 梅西大学; 华沙大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用凯克和哈勃望远镜数据，首次直接探测到含行星的双星微透镜系统OGLE-2006-BLG-284，测得恒星质量与行星质量，并推动后续视向速度观测以确定行星轨道归属。
AI 中文摘要
自引力微透镜首次发现系外行星以来，已近25年。透镜与源系统之间的相对自行使它们能在数年内随着在天球上的分离而被分辨。这使得科学家能够研究直接来自透镜的光，并对这些行星系统的物理性质施加严格约束。本文中，我们利用凯克自适应光学和哈勃太空望远镜在事件发生15年多后获取的数据，对微透镜目标OGLE-2006-BLG-284进行了高角分辨率图像分析。我们清晰地探测到透镜系统，并测量了其在凯克和哈勃观测历元间的运动。我们测得透镜-源相对自行速度为$5.80 \pm 0.15$毫角秒/年。结合光变曲线参数和主星在$V$、$I$、$K$波段的亮度，我们得出主星和次星的质量分别为$M_{\rm 1} = 0.43 \pm 0.05\\,M_{\odot}$和$M_{\rm 2} = 0.12 \pm 0.02\\,M_{\odot}$，行星伴星质量为$m_p = 165^{+40}_{-33}\\,M_{\oplus}$。尽管我们无法确定该行星是绕双星中的一颗还是绕两颗运行，但我们的分析推动了下一代高精度视向速度测量，以区分这两种可能性。这是首次直接探测到来自含行星的双星微透镜系统的光通量。
英文摘要
Nearly 25 years have passed since gravitational microlensing delivered its first exoplanet discoveries. The relative proper motion between lens and source systems allows them to be resolved as they separate on the sky over many years. This enables scientists to study light coming directly from the lenses and place tight constraints on the physical properties of these planetary systems. In this paper we present an analysis of high angular resolution images of the microlensing target OGLE-2006-BLG-284 using Keck adaptive optics and HST data taken more than 15 years after the event. We clearly detect the lens system and measure its motion across the Keck and HST epochs. We measure a lens-source relative proper motion of $5.80 \pm 0.15$ mas yr$^{-1}$. A combination of the light curve parameters and the host star(s) brightnesses in $V,\, I$, and $K$ passbands gives primary and secondary host star masses of $M_{\rm 1} = 0.43 \pm 0.05\,M_{\odot}$ and $M_{\rm 2} = 0.12 \pm 0.02\,M_{\odot}$, and a planetary companion mass of $m_p = 165^{+40}_{-33}\,M_{\oplus}$. Although we are unable to determine if the planet orbits one or both stars in the system, our analysis motivates next-generation high-precision RV measurements that can distinguish these two possibilities. This is the first direct detection of flux coming from a two-star microlensing system which hosts a planet.
Comments15 pages, 8 figures, submitted to AJ
