binary system. We also excluded systems fainter than Kepler magnitude ${\rm Kp} \approx 13$ unless they seemed particularly interesting based on an initial appraisal of the light curve or other information available. These points of interest are noted in section \[notes\_sec\].

The list of stars selected for further analysis is shown in Table \[lcinfo\] together with some basic characteristics of the light curves. The rotation periods $P_{\rm rot}$ listed in this table were determined as part of the detrending process described in section \[detrend\_sec\].

Aperture photometry and detrending \[detrend\_sec\]
---------------------------------------------------

We downloaded the target pixel files for each target from MAST and used these data to produce light curves using synthetic aperture photometry. We first calculated the median value for every pixel in the data cube. The pixels in the lowest 10-percentile of this median image were then used to calculate the background level in the individual images. We used the target aperture specified in the target pixel file where available, otherwise we used a circular aperture centered on the flux-weighted centroid of the median image with a radius selected by-eye to encompass most of the flux in the star – typically 4–8 pixels. We also calculated the flux-weighted centroid 