A large bulk of our program is photometry. We are currently carrying out photometry on an increasing number of red dwarfs (basically as many stars as we can manage at any given time).

Red dwarfs have received VERY little time-series photometry of the years. Most have been the target of single multi-band observations to establish color indices and magnitudes, but repeat observations (to establish photometric variations due to flaring and, especially, rotation) have been extremely scarce.

A very limited number of photometric rotation periods have been determined, but always for red dwarfs of short periods (almost all less than 5 days or so).

There is a larger number of spectroscopically inferred rotation periods, through v sin i measures. However, these observations must be carefully carried out and calibrated, and are still subject to sufficient errors and detection limits to inhibit the accurate determination of "slower" rotations.