Joint Analysis of Multicolor Photometry: A New Approach to Constrain the Nature of Multiple-star Systems Hosting Exoplanet Candidates
Joint Analysis of Multicolor Photometry: A New Approach to Constrain the Nature of Multiple-star Systems Hosting Exoplanet Candidates
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DOI：
10.3847/1538-3881/abf500
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发表时间：
2021-05
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影响因子：
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通讯作者：
K. Miyakawa;T. Hirano;B. Sato;A. Fukui;N. Narita
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作者：
K. Miyakawa;T. Hirano;B. Sato;A. Fukui;N. Narita
我们提出了一种用多色光度法评估过境候选行星性质的新方法。通过平行分析多色的过境/日食光曲线和目标的视星等，该方法试图确定系统的性质，并对未解析伴星的性质提供定量约束。我们通过观测K2任务（EPIC 206036749, EPIC 206500801, EPIC 210513446, EPIC 211800191， EPIC 220621087和EPIC 220696233）确定的六个拥有候选凌日行星的系统来证明我们的方法。将我们的分析代码应用于六个目标，我们发现EPIC 206036749， EPIC 210513446和EPIC 211800191可能是包含食双星的三星系统，而EPIC 220696233可能是一个行星系统，尽管需要进一步的观测来确认其性质。此外，我们证实了采用特定等时模型和观测仪器（通带）所得到的系统参数的系统误差相对较小。虽然这种方法本身不足以验证或反驳候选行星，但该技术使我们能够约束已解决/未解决的伴星的特性，并优先考虑候选行星进行进一步的后续观测（例如，径向速度测量）。
We present a new method to assess the properties of transiting planet candidates by multicolor photometry. By analyzing multicolor transit/eclipse light curves and apparent magnitudes of the target in parallel, this method attempts to identify the nature of the system and provide a quantitative constraint on the properties of unresolved companion(s). We demonstrate our method by observing the six systems hosting candidate transiting planets, identified by the K2 mission (EPIC 206036749, EPIC 206500801, EPIC 210513446, EPIC 211800191, EPIC 220621087, and EPIC 220696233). Applying our analysis code to the six targets, we find that EPIC 206036749, EPIC 210513446, and EPIC 211800191 are likely to be triple-star systems including eclipsing binaries, and EPIC 220696233 is likely a planetary system, albeit further observations are required to confirm the nature. Additionally, we confirm that the systematic errors in the derived system parameters arising from adopting specific isochrone models and observing instruments (passbands) are relatively small. While this approach alone is not powerful enough to validate or refute planet candidates, the technique allows us to constrain the properties of resolved/unresolved companions, and prioritize the planet candidates for further follow-up observations (e.g., radial-velocity measurements).