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arXiv 1305.0280astro-ph.SRastro-ph.EP
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MARVELS-1：伪装成共振行星系统的正面双线双星;以及对径向速度行星搜索中罕见误报的考虑

MARVELS-1: A face-on double-lined binary star masquerading as a resonant planetary system; and consideration of rare false positives in radial velocity planet searches

Jason T. Wright, Arpita Roy, Suvrath Mahadevan, Sharon X. Wang, Eric B. Ford, Matt Payne, Brian L. Lee, Ji Wang, Justin R. Crepp, B. Scott Gaudi, Jason Eastman,… 展开作者

Jason T. Wright, Arpita Roy, Suvrath Mahadevan, Sharon X. Wang, Eric B. Ford, Matt Payne, Brian L. Lee, Ji Wang, Justin R. Crepp, B. Scott Gaudi, Jason Eastman, Joshua Pepper, Jian Ge, Scott W. Fleming, Luan Ghezzi, Jonay I. Gonzalez-Hernandez, Phillip Cargile, Keivan G. Stassun, John Wisniewski, Leticia Dutra-Ferreira, Gustavo F. Porto de Mello, Marcio A. G. Maia, Luiz Nicolaci da Costa, Ricardo L. C. Ogando, Basilio X. Santiago, Donald P. Schneider, Fred R. Hearty

备注：
ApJ 770, 119. 24 pp emulate ApJ style, 12 figures (One is very large). v2: corrects two (important!) errors: A priori chance of this alignment or worse is 0.1% (not 0.01%) and the primary has THREE total companions (not four)
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摘要：

我们已经分析了新的和以前发表的径向速度观测的MARVELS-1，已知有一个表面上的亚恒星同伴在一个6天的轨道。我们发现了与伴星最佳拟合模型的显著（~100 m/s）残差，这些残差与P = 1.965 d的内部巨行星在近乎完美的3：1周期周期内的一致性（|Pb/Pc - 3| < 10^{-4}）。我们已经进行了几次测试，包括动力学分析，寻找光度变化，以及寻找污染的恒星光谱。我们发现了许多对行星解释持批评态度的理由，包括大多数三体动力学解都是不稳定的。我们没有发现凌日的证据，也没有恒星光度变化的证据。我们已经发现了两个明显的同伴MARVELS-1与自适应光学成像在凯克;都是M矮星，一个可能是绑定，另一个可能是前景对象。我们探索假警报的情况下，在数据中的各种好奇心的启发。最后，线轮廓和平分线分析使我们得出结论，~100 m/s的残差是光谱污染的伪像，来自恒星伴星，贡献了系统中约15-30%的可见光。我们的结论是，这种污染的起源是以前检测到的径向速度同伴MARVELS-1，这不是，如以前报道的那样，一个褐矮星，但实际上是一个G矮星在一个面对轨道。

英文摘要：

We have analyzed new and previously published radial velocity observations of MARVELS-1, known to have an ostensibly substellar companion in a ~6- day orbit. We find significant (~100 m/s) residuals to the best-fit model for the companion, and these residuals are naively consistent with an interior giant planet with a P = 1.965d in a nearly perfect 3:1 period commensuribility (|Pb/Pc - 3| < 10^{-4}). We have performed several tests for the reality of such a companion, including a dynamical analysis, a search for photometric variability, and a hunt for contaminating stellar spectra. We find many reasons to be critical of a planetary interpretation, including the fact that most of the three-body dynamical solutions are unstable. We find no evidence for transits, and no evidence of stellar photometric variability. We have discovered two apparent companions to MARVELS-1 with adaptive optics imaging at Keck; both are M dwarfs, one is likely bound, and the other is likely a foreground object. We explore false-alarm scenarios inspired by various curiosities in the data. Ultimately, a line profile and bisector analysis lead us to conclude that the ~100 m/s residuals are an artifact of spectral contamination from a stellar companion contributing ~15-30% of the optical light in the system. We conclude that origin of this contamination is the previously detected radial velocity companion to MARVELS-1, which is not, as previously reported, a brown dwarf, but in fact a G dwarf in a face-on orbit.

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