在模拟PLATO数据中探测凌星系外行星：光变曲线滤波与凌星搜索算法的比较
Detecting transiting exoplanets in simulated PLATO data: A comparison of light curve filter and transit search algorithms
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中文总结 AI 辅助
本研究通过模拟PLATO数据比较三种凌星搜索算法，发现nuance性能最佳，但计算成本高；建议PLATO流水线采用多窗口Huber样条滤波，并更新CETRA模板。
中文摘要 AI 辅助
目的：我们的目标是测试并比较凌星搜索方法，并为即将开展的欧空局PLATO任务提供最佳实践建议，以实现其探测类太阳恒星宜居带内类地行星的目标。方法：我们生成了为期两年的模拟PLATO光变曲线，并注入了大小为0.5–2.0 $R_\oplus$的行星，比较了CETRA、umbra和nuance三种凌星搜索方法的性能。CETRA和umbra需要预滤波的光变曲线，我们测试了biweight、Huber样条、Lowess和YSD-Lowess滤波器。nuance使用高斯过程对所有拟议的凌星参数下的恒星变率进行建模。结果：nuance取得了最佳性能，使用简谐振荡器高斯过程核恢复了61.2%的信号，并且在热星和快速自转恒星上表现尤为出色。然而，当考虑多个Huber样条滤波窗口时，CETRA和umbra都能达到nuance的性能。CETRA使用四个窗口时与nuance相当，恢复了61.3%的信号。umbra使用两个窗口时与nuance相当，恢复了61.7%的信号。使用更多窗口可以实现超过nuance的恢复率。运行nuance的计算成本非常高，因此优先选择在多个窗口上运行CETRA或umbra。结论：PLATO流水线应使用具有一系列窗口大小的Huber样条作为其主要光变曲线滤波器。CETRA应更新为使用umbra中实现的最小二乘模板。对于热的、快速自转的恒星，应考虑使用nuance。
英文摘要
Aims: Our goal is to test and compare transit search methodologies, and provide recommendations as to the best practices to be implemented by the upcoming ESA PLATO mission, in order to achieve its goal of detecting Earth-like planets in the habitable zones of Sun-like stars. Methods: We generate simulated two-year PLATO light curves with injected planets with sizes 0.5--2.0 $R_\oplus$, and compare the performance of the CETRA, umbra, and nuance transit search methods. CETRA and umbra require pre-filtered light curves and we test the biweight, Huber spline, Lowess, and YSD-Lowess filters. nuance uses a Gaussian process to model the stellar variability at all proposed transit parameters. Results: nuance achieves the best performance, recovering 61.2% signals using a simple harmonic oscillator Gaussian process kernel, and it performs especially well for both hot and fast-rotating stars. However, when multiple Huber spline filter windows are considered, both CETRA and umbra can match nuance's performance. CETRA matches nuance with four windows, recovering 61.3% of signals. umbra matches nuance with two windows, recovering 61.7% of signals. Recovery rates exceeding nuance are possible by using more windows. The computational cost of running nuance is so high that running CETRA or umbra on multiple windows is preferred. Conclusions: The PLATO pipeline should use the Huber spline with a range of window sizes as its primary light curve filter. CETRA should be updated to use the warped least-squares templates implemented in umbra. The use of nuance should be considered for hot, rapidly rotating stars.
发表机构
- University of Oxford（牛津大学）
- University of Cambridge（剑桥大学）
- Università di Padova（帕多瓦大学）
- INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）
- Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理学中心）
机构由 AI 辅助整理，请以论文原文为准。
