OGLE-2014-BLG-0962 and a Comparison of Galactic Model Priors to Microlensing Data
OGLE-2014-BLG-0962 and a Comparison of Galactic Model Priors to Microlensing Data
复制标题
DOI：
10.3847/1538-4357/ab0021
复制
发表时间：
2019-02
期刊：
影响因子：
--
通讯作者：
Y. Shan;J. Yee;A. Udalski;I. Bond;Y. Shvartzvald;I. Shin;Y. Jung;S. Novati;C. Beichman;S. Carey;B. Gaudi;A. Gould;R. Pogge;aw Poleski;J. Skowron;aw J. Mróz;Pawe;Pietrukowicz;K. Szyma;ski;I. Soszy;K. Ulaczyk;ukasz Wyrzykowski;F. Abe;R. Barry;D. Bennett;A. Bhattacharya;M. Donachie;A. Fukui;Y. Hirao;Y. Itow;K. Kawasaki;I. Kondo;N. Koshimoto;M. Li;Y. Matsubara;Y. Muraki;S. Miyazaki;M. Nagakane;C. Ranc;N. Rattenbury;H. Suematsu;D. Sullivan;T. Sumi;D. Suzuki;P. Tristram;A. Yonehara;D. Maoz;S. Kaspi;M. Friedmann
中科院分区：
文献类型：
--
作者：
Y. Shan;J. Yee;A. Udalski;I. Bond;Y. Shvartzvald;I. Shin;Y. Jung;S. Novati;C. Beichman;S. Carey;B. Gaudi;A. Gould;R. Pogge;aw Poleski;J. Skowron;aw J. Mróz;Pawe;Pietrukowicz;K. Szyma;ski;I. Soszy;K. Ulaczyk;ukasz Wyrzykowski;F. Abe;R. Barry;D. Bennett;A. Bhattacharya;M. Donachie;A. Fukui;Y. Hirao;Y. Itow;K. Kawasaki;I. Kondo;N. Koshimoto;M. Li;Y. Matsubara;Y. Muraki;S. Miyazaki;M. Nagakane;C. Ranc;N. Rattenbury;H. Suematsu;D. Sullivan;T. Sumi;D. Suzuki;P. Tristram;A. Yonehara;D. Maoz;S. Kaspi;M. Friedmann
OGLE-2014-BLG-0962（OB 140962）是一个恒星双星微透镜事件，它被斯皮策卫星的观测以及地面调查很好地覆盖。模拟结果给出了一个独特的物理解：一个中M + M矮星双星，其M轨道为0.20 ± 0.01 M，M秒为0.16 ± 0.01 M，预计距离为2.0 ± 0.3 Au。透镜在光源前的DLS仅为0.41 ± 0.06 kpc，使OB 140962成为一个凸出的透镜，也是迄今为止距离最远的斯皮策双星透镜。相比之下，由于爱因斯坦半径（θE = 0.143 ± 0.007 mas）非常小，在没有视差信息的情况下进行的标准贝叶斯分析将预测棕矮星双星。我们比较贝叶斯分析的结果，使用两种常用的银河系模型先验的一组斯皮策镜头的测量值。我们发现所有的模型测试预测透镜属性与斯皮策数据一致。此外，我们通过比较斯皮策两体透镜与斯皮策单透镜的累积距离分布，说明了探测银河系行星分布的方法。
OGLE-2014-BLG-0962 (OB140962) is a stellar binary microlensing event that was well covered by observations from the Spitzer satellite as well as ground-based surveys. Modeling yields a unique physical solution: a mid-M+M-dwarf binary with Mprim = 0.20 ± 0.01 M☉ and Msec = 0.16 ± 0.01 M☉, with projected separation of 2.0 ± 0.3 au. The lens is only DLS = 0.41 ± 0.06 kpc in front of the source, making OB140962 a bulge lens and the most distant Spitzer binary lens to date. In contrast, because the Einstein radius (θE = 0.143 ± 0.007 mas) is unusually small, a standard Bayesian analysis, conducted in the absence of parallax information, would predict a brown dwarf binary. We compare the results of Bayesian analysis using two commonly used Galactic model priors to the measured values for a set of Spitzer lenses. We find all models tested predict lens properties consistent with the Spitzer data. Furthermore, we illustrate the methodology for probing the Galactic distribution of planets by comparing the cumulative distance distribution of the Spitzer two-body lenses to that of the Spitzer single lenses.