  In Bastien et al. (2013) we found that high quality light curves, such as
those obtained by Kepler, may be used to measure stellar surface gravity via
granulation-driven light curve "flicker". Here, we update and extend the
relation originally presented in Bastien et al. (2013) after calibrating
flicker against a more robust set of asteroseismically derived surface
gravities. We describe in detail how we extract the flicker signal from the
light curves, including how we treat phenomena, such as exoplanet transits and
shot noise, that adversely affect the measurement of flicker. We examine the
limitations of the technique, and, as a result, we now provide an updated
treatment of the flicker-based logg error. We briefly highlight further
applications of the technique, such as astrodensity profiling or its use in
other types of stars with convective outer layers. We discuss potential uses in
current and upcoming space-based photometric missions. Finally, we supply
flicker-based logg values, and their uncertainties, for 27 628 Kepler stars not
identified as transiting-planet hosts, with 4500<teff<7150 K, 2.5<logg<4.6,
Kepler magnitude <13.5, and overall photometric amplitudes <10 parts per
thousand.
