MEASURING TRANSIT SIGNAL RECOVERY IN THE KEPLER PIPELINE. III. COMPLETENESS OF THE Q1–Q17 DR24 PLANET CANDIDATE CATALOG WITH IMPORTANT CAVEATS FOR OCCURRENCE RATE CALCULATIONS
MEASURING TRANSIT SIGNAL RECOVERY IN THE KEPLER PIPELINE. III. COMPLETENESS OF THE Q1–Q17 DR24 PLANET CANDIDATE CATALOG WITH IMPORTANT CAVEATS FOR OCCURRENCE RATE CALCULATIONS
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DOI：
10.3847/0004-637x/828/2/99
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发表时间：
2016-05
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通讯作者：
J. Christiansen;B. Clarke;C. Burke;J. Jenkins;S. Bryson;J. Coughlin;F. Mullally;S. Thompson;J. Twicken;N. Batalha;M. Haas;J. Catanzarite;Jennifer Campbell;A. K. Uddin;Khadeejah A. Zamudio;Jeffrey C. Smith;C. Henze
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作者：
J. Christiansen;B. Clarke;C. Burke;J. Jenkins;S. Bryson;J. Coughlin;F. Mullally;S. Thompson;J. Twicken;N. Batalha;M. Haas;J. Catanzarite;Jennifer Campbell;A. K. Uddin;Khadeejah A. Zamudio;Jeffrey C. Smith;C. Henze
随着开普勒管道和产生的行星候选目录的每个新版本，底层行星人口的更新测量只能通过开普勒管道检测效率的相应测量来恢复。在这里，我们介绍了用于生成Q1-Q17 DR 24行星候选目录的管道（版本9.2）的灵敏度测量。我们通过将模拟的凌日行星注入到整个开普勒焦平面上159，013个目标的像素级数据中来测量这一点，并检查恢复率。与以前版本的开普勒管道不同，我们发现测量的探测效率具有很强的周期依赖性，较长（>40天）的周期比较短的周期具有明显较低的可探测性，部分原因是错误地实施否决权。因此，9.2管道的灵敏度不能被转换为候选行星信号的信号强度的简单一维函数，而对于管道的先前版本是可能的。我们报告了基于Q1-Q17 DR 24行星候选目录的发生率计算的影响，并为执行此类计算提供了重要的警告和建议。和以前一样，我们提供了整个注入行星参数表以及它们是否被管道恢复，使读者能够在他们选择的行星和/或恒星参数空间中获得管道检测灵敏度。
With each new version of the Kepler pipeline and resulting planet candidate catalog, an updated measurement of the underlying planet population can only be recovered with a corresponding measurement of the Kepler pipeline detection efficiency. Here we present measurements of the sensitivity of the pipeline (version 9.2) used to generate the Q1–Q17 DR24 planet candidate catalog. We measure this by injecting simulated transiting planets into the pixel-level data of 159,013 targets across the entire Kepler focal plane, and examining the recovery rate. Unlike previous versions of the Kepler pipeline, we find a strong period dependence in the measured detection efficiency, with longer (>40 day) periods having a significantly lower detectability than shorter periods, introduced in part by an incorrectly implemented veto. Consequently, the sensitivity of the 9.2 pipeline cannot be cast as a simple one-dimensional function of the signal strength of the candidate planet signal, as was possible for previous versions of the pipeline. We report on the implications for occurrence rate calculations based on the Q1–Q17 DR24 planet candidate catalog, and offer important caveats and recommendations for performing such calculations. As before, we make available the entire table of injected planet parameters and whether they were recovered by the pipeline, enabling readers to derive the pipeline detection sensitivity in the planet and/or stellar parameter space of their choice.