  No circumbinary planets have been discovered smaller than 3 Earth radii, yet
planets of this small size comprise over 75% of the discoveries around single
stars. The observations do not prove the non-existence of small circumbinary
planets, but 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 Earth radii 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 which can
be compared to that for single stars.
