AI 中文总结
该研究针对微引力透镜行星系统OGLE-2014-BLG-0676，将凯克AO高分辨率成像纳入光曲线建模，通过结合二者减轻系统效应和建模简并性，确定了该系统的主恒星质量、透镜距离、行星质量等物理性质，结果可被未来观测证实。
AI 中文摘要
我们提出了一种分析方法，将凯克自适应光学（AO）高分辨率成像纳入行星微引力透镜事件OGLE-2014-BLG-0676的微引力透镜光曲线建模中。利用事件发生6.3年后获得的凯克AO观测数据，我们直接分辨出了透镜和源。凯克图像显示出一种张力，即K波段源通量比先前报道的光曲线模型预测的亮0.52±0.22星等。通过将凯克成像约束纳入光曲线建模，我们得到了主恒星质量\(M_{\rm host}=0.60^{+0.17}_{-0.14}\,M_{\odot}\)，透镜距离\(D_{\rm L}=1.88^{+0.63}_{-0.35}\)千秒差距，行星质量\(m_{\rm p}=3.11^{+1.11}_{-0.63}\,M_{\rm J}\)，以及近距离和远距离解的投影间距分别为\(a_{\perp}=2.04^{+0.44}_{-0.35}\)天文单位和\(a_{\perp}=3.72^{+0.92}_{-0.72}\)天文单位。这些结果证明了将高角分辨率成像与微引力透镜光曲线建模相结合以减轻潜在系统效应和建模简并性的能力，从而能够可靠地确定微引力透镜行星系统的物理性质。这里给出的结果可以通过未来罗马太空望远镜的银道面调查观测得到证实。
英文摘要
We present an analysis that incorporates high-resolution Keck adaptive optics (AO) imaging into microlensing light-curve modeling for the planetary microlensing event OGLE-2014-BLG-0676. Using Keck AO observations obtained 6.3 years after the event, we directly resolved the lens and source. The Keck images reveal a tension, in that the $K$-band source flux is $0.52 \pm 0.22$ magnitudes brighter than predicted by previously reported light-curve models. By incorporating the Keck imaging constraints into the light-curve modeling, we find a host star mass of $M_{\rm host} = 0.60^{+0.17}_{-0.14}\,M_{\odot}$, a lens distance of $D_{\rm L} = 1.88^{+0.63}_{-0.35}$ kpc, a planet mass of $m_{\rm p} = 3.11^{+1.11}_{-0.63}\,M_{\rm J}$, and a projected separation of $a_{\perp} = 2.04^{+0.44}_{-0.35}$ au and $a_{\perp} = 3.72^{+0.92}_{-0.72}$ au for the close and wide solution, respectively. These results demonstrate the power of combining high-angular-resolution imaging with microlensing light-curve modeling to mitigate potential systematic effects and modeling degeneracies, enabling robust determinations of the physical properties of microlensing planetary systems. The results presented here can be confirmed by future observations from the \textit{Roman}'s Galactic Plane Survey.
CommentsAccepted for publication in AJ
