Spitzer Microlensing Parallax for OGLE-2016-BLG-1067: A Sub-Jupiter Orbiting an M Dwarf in the Disk
Spitzer Microlensing Parallax for OGLE-2016-BLG-1067: A Sub-Jupiter Orbiting an M Dwarf in the Disk
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DOI：
10.3847/1538-3881/ab0106
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发表时间：
2018-01
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通讯作者：
S. Calchi Novati;D. Suzuki;A. Udalski;A. Gould;Y. Shvartzvald;V. Bozza;D. Bennett;C. Beichman;G. Bryden;S. Carey;B. Gaudi;C. Henderson;J. Yee;W. Zhu;F. Abe;Y. Asakura;R. Barry;A. Bhattacharya;I. Bond;M. Donachie;P. Evans;A. Fukui;Y. Hirao;Y. Itow;K. Kawasaki;N. Koshimoto;M. Li;C. Ling;Y. Matsubara;S. Miyazaki;Y. Muraki;M. Nagakane;K. Ohnishi;C. Ranc;N. Rattenbury;T. Saito;A. Sharan;D. Sullivan;T. Sumi;P. Tristram;T. Yamada;A. Yonehara;P. Mróz;R. Poleski;J. Skowron;M. Szyma'nski;I. Soszy'nski;S. Kozłowski;P. Pietrukowicz;K. Ulaczyk;M. Pawlak;M. Albrow;S. Chung;C. Han;K. Hwang;Y. Jung;Y. Ryu;I. Shin;W. Zang;S. Cha;D.-J. Kim;H.-W. Kim;S.-L. Kim;C.‐U. Lee;D.-J. Lee;Y. Lee;B.-G. Park;R. Pogge
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作者：
S. Calchi Novati;D. Suzuki;A. Udalski;A. Gould;Y. Shvartzvald;V. Bozza;D. Bennett;C. Beichman;G. Bryden;S. Carey;B. Gaudi;C. Henderson;J. Yee;W. Zhu;F. Abe;Y. Asakura;R. Barry;A. Bhattacharya;I. Bond;M. Donachie;P. Evans;A. Fukui;Y. Hirao;Y. Itow;K. Kawasaki;N. Koshimoto;M. Li;C. Ling;Y. Matsubara;S. Miyazaki;Y. Muraki;M. Nagakane;K. Ohnishi;C. Ranc;N. Rattenbury;T. Saito;A. Sharan;D. Sullivan;T. Sumi;P. Tristram;T. Yamada;A. Yonehara;P. Mróz;R. Poleski;J. Skowron;M. Szyma'nski;I. Soszy'nski;S. Kozłowski;P. Pietrukowicz;K. Ulaczyk;M. Pawlak;M. Albrow;S. Chung;C. Han;K. Hwang;Y. Jung;Y. Ryu;I. Shin;W. Zang;S. Cha;D.-J. Kim;H.-W. Kim;S.-L. Kim;C.‐U. Lee;D.-J. Lee;Y. Lee;B.-G. Park;R. Pogge
我们报告了一颗质量低于木星的行星的发现，它的轨道超出了M矮星的雪线，最有可能在银盘中，这是斯皮策和地面联合监测行星微透镜异常朝向银河凸起的一部分。大多数微透镜参数受到光曲线建模的强烈限制，特别是基于斯皮策的微透镜视差πE的测量。然而，由于没有焦散交叉，因此仅基于光曲线建模的角度爱因斯坦半径具有上限。此外，分析还导致我们确定了八种简并构型：四重微透镜视差简并被存在于地面解水平的焦散结构的简并所加倍。为了计算物理参数，同时打破视差简并，我们使用了一系列自变量：χ2层次结构、丰富自变量(指出小视差解更有可能)，以及先前的银河系模型。在概率比至少为4000的情况下，首选的构型是质量相同的宿主，由一颗预计分离的类似土星的行星绕轨道运行，大约是系统雪线的2.1倍。因此，它增加了通过微透镜发现的超出M矮星雪线的亚木星行星的数量。根据选择斯皮策后续事件的实时协议规则，这颗行星将不会进入测量银河系行星分布的样本。
We report the discovery of a sub-Jupiter-mass planet orbiting beyond the snow line of an M dwarf most likely in the Galactic disk as part of the joint Spitzer and ground-based monitoring of planetary microlensing anomalies toward the Galactic bulge. Most of the microlensing parameters are strongly constrained by the light-curve modeling, and in particular there is a Spitzer-based measurement of the microlens parallax, πE. However, there are no caustic crossings, so the angular Einstein radius has only an upper limit based on the light-curve modeling alone. Additionally, the analysis leads us to identify eight degenerate configurations: the fourfold microlensing parallax degeneracy being doubled by a degeneracy in the caustic structure present at the level of the ground-based solutions. To calculate the physical parameters, and at the same time to break the parallax degeneracy, we make use of a series of arguments: the χ2 hierarchy, the Rich argument (stating that the small-parallax solution is more likely), and a prior Galactic model. The preferred configuration, favored by a likelihood ratio of at least 4000, is for a host at with mass , orbited by a Saturn-like planet with at projected separation , about 2.1 times beyond the system snow line. Therefore, it adds to the growing population of sub-Jupiter planets orbiting beyond the snow line of M dwarfs discovered by microlensing. Based on the rules of the real-time protocol for the selection of events to be followed up with Spitzer, this planet will not enter the sample for measuring the Galactic distribution of planets.