Photometry of Bright Stars
While Kepler was engineered primarily to look at thousands of faint stars to do population statistics, planets transiting naked-eye stars, like the super-Earth 55 Cnc e, are the best targets for detailed characterization. Unfortunately, stars this bright saturate the Kepler and TESS detectors, making them hard or impossible to observe conventionally. Using 'smear' and 'halo' photometry, we can achieve normal Kepler-like precision on stars orders of magnitude brighter than it was ever meant to observe.
Smear Photometry
Collateral "smear" data, normally used as a calibration step for calibrating Kepler photometry, can obtain light curves of stars too bright to observe conventionally. This is described in our MNRAS Letters paper. Many stars in the Kepler and K2 fields were unobserved or under-observed because of saturation, and smear photometry opens a new window on the Kepler archive. We published a full catalog of smear light curves in ApJS for the Kepler Smear Campaign, using smear to obtain light curves of the 102 brightest (Kp<9) stars in Kepler that were not otherwise observed. Light curves are available on GitHub or from MAST. See this Bokeh interactive HR diagram of the smear campaign sample overlaid on the gaia-kepler.fun sample.
Halo Photometry
In collaboration with Tim White we developed 'halo photometry', a new method using weighted sums of unsaturated pixels to minimize instrumental systematics. This revealed variability in the Seven Sisters of the Pleiades and oscillations in the red giant Aldebaran. We produced a systematic reduction of all the naked-eye stars in K2, published in ApJS. The paper source code, documentation and lightcurves for this K2 Bright Star Survey are available on GitHub and the light curves are available as a High Level Science Product on MAST. See this Bokeh interactive HR diagram of the halo campaign sample.
