发表机构
The University of Osaka; Massey University; Ohio State University; Westlake University; NASA Goddard Space Flight Center; University of Maryland, College Park（大阪大学; 梅西大学; 俄亥俄州立大学; 西湖大学; 美国宇航局戈达德太空飞行中心; 马里兰大学帕克分校）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文分析两个微引力透镜事件，利用KMTNet光学与PRIME近红外颜色约束源半径，发现颜色估计影响物理参数，偏差需更大样本和自适应光学验证。
AI 中文摘要
我们呈现了对两个2024年微引力透镜事件KMT-2024-BLG-0211和KMT-2024-BLG-1522的分析，这两个事件由KMTNet在光学波段和PRIME在近红外波段联合观测。对于KMT-2024-BLG-0211，KMTNet--PRIME的$I-H$颜色为具有巨星源的短时标有限源事件提供了对源角半径的有用约束。该事件与低质量恒星透镜一致，尽管较弱的视差约束使得透镜质量和距离不确定。对于KMT-2024-BLG-1522，我们比较了从$V-I$、$I-H$、$V-H$和$J-H$颜色约束获得的结果。四次分析得到的微引力透镜参数几乎相同，产生了一个质量近乎相等的稳健双透镜解。然而，推断的源属性和透镜物理参数取决于所采用的源颜色，因为不同的颜色估计意味着不同的源角半径。比较$(V-I)_{\ m KMT}$与$(I-H)_{\ m KMT,PRIME}$平面显示，推断的源颜色偏离经验颜色-颜色关系，但落在观测恒星散布范围内。这种偏差的普遍性应通过更大的KMTNet--PRIME事件样本来测试，而这个特定案例可以通过未来的自适应光学后续观测进一步测试，该观测可以直接测量透镜-源相对自行和透镜通量。
英文摘要
We present analyses of two 2024 microlensing events, KMT-2024-BLG-0211 and KMT-2024-BLG-1522, jointly observed by KMTNet in the optical and PRIME in the near-infrared. For KMT-2024-BLG-0211, the KMTNet--PRIME $I-H$ color provides a useful constraint on the angular source radius for a short-timescale finite-source event with a giant source. The event is consistent with a low-mass stellar lens, although the weak parallax constraint leaves the lens mass and distance uncertain. For KMT-2024-BLG-1522, we compare the results obtained from $V-I$, $I-H$, $V-H$, and $J-H$ color constraints. The microlensing parameters are nearly identical among the four analyses, yielding a robust binary-lens solution with nearly equal masses. However, the inferred source properties and lens physical parameters depend on the adopted source color because the different color estimates imply different angular source radii. Comparing the $(V-I)_{\rm KMT}$ versus $(I-H)_{\rm KMT,PRIME}$ plane shows that the inferred source colors lie off empirical color--color relations but within the scatter of observed stars. The prevalence of such deviations should be tested with a larger sample of KMTNet--PRIME events and this specific case can be further tested with future adaptive-optics follow-up, which can directly measure the lens--source relative proper motion and lens flux.
Comments26 pages, 10 figures, 4 tables
