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We have developed a method to estimate surface gravity (log g) from lightcurves by measuring the granulation background, similar to the "flicker" methodby Bastien et al. (2016) but working in the Fourier power spectrum. Wecalibrated the method using Kepler stars for which asteroseismology has beenpossible with short-cadence data, demonstrating a precision in log g of about0.05 dex. We also derived a correction for white noise as a function of Keplermagnitude by measuring white noise directly from observations. We then appliedthe method to the same sample of long-cadence stars as Bastien et al. We foundthat about half the stars are too faint for the granulation background to bereliably detected above the white noise. We provide a catalogue of log g valuesfor about 15,000 stars having uncertainties better than 0.5 dex. We used GaiaDR2 parallaxes to validate that granulation is a powerful method to measure logg from light curves. Our method can also be applied to the large number oflight curves collected by K2 and TESS.

Surface gravities for 15,000 Kepler stars measured from stellar granulation and validated with Gaia DR2 parallaxes