No circumbinary planets have been discovered smaller than 3 R _⊕, yet planets of this small size comprise over 75% of the discoveries around single stars. The observations do not prove the nonexistence of small circumbinary planets; rather, they are much harder to find than around single stars because their transit timing variations are much larger than the transit durations. We present Stanley, an automated algorithm to find small circumbinary planets. It employs custom methods to detrend eclipsing binary light curves and stack shallow transits of variable duration and interval using N-body integrations. Applied to the Kepler circumbinaries, we recover all known planets, including the three planets of Kepler-47, and constrain the absence of additional planets of similar or smaller size. We also show that we could have detected <3 R _⊕ planets in half of the known systems. Our work will ultimately be applied to a broad sample of eclipsing binaries to (hopefully) produce new discoveries and derive a circumbinary size distribution that can be compared to that for single stars.

尚未发现小于 3 R _{⊕ 的}双环行星，但这种小尺寸的行星占单星周围发现的 75% 以上。观测结果并不能证明小型环绕双星行星不存在；相反，它们比在单颗恒星周围更难找到，因为它们的凌日时间变化远大于凌日持续时间。我们展示了Stanley，这是一种自动算法，用于寻找小型环绕双星行星。它采用自定义方法来消除日食二元光变曲线的趋势，并使用N堆叠可变持续时间和间隔的浅层过渡-身体整合。应用于开普勒双星，我们恢复了所有已知的行星，包括开普勒 47 的三颗行星，并限制没有其他类似或更小尺寸的行星。我们还表明，我们可以在一半的已知系统中检测到 <3 R _⊕行星。我们的工作最终将应用于食双星的广泛样本，以（希望）产生新的发现并推导出可以与单颗恒星进行比较的环绕双星大小分布。