We check for correlations of variability and high-frequency PSD slope with accretion rate, black hole mass, redshift, and luminosity. These timescales are consistent more » with orbital timescales or free-fall accretion timescales. Six objects exhibit PSD flattening at characteristic timescales that roughly correlate with black hole mass. The light curves display an astonishing variety of behaviors, many of which would not be detected in ground-based studies, including switching between distinct flux levels. We then present the light curves, power spectral density functions (PSDs), and flux histograms. First, we describe the necessity and development of a customized pipeline for treating Kepler data of stochastically variable sources like AGN. Here, we present a comprehensive analysis of 21 light curves of Type 1 active galactic nuclei (AGN) from the Kepler spacecraft. This indicates that despite the scale invariance of accretion processes implied by a decades-wide correlation between QPO frequency and black hole mass, any theory of high-frequency QPOs must relate the frequency to more than just the mass and = ). Oscillations seen in tidal disruption events are consistent with oscillations near the frequency of the innermost stable circular orbit, while QPOs in AGN are not accounted for by any of the physical models in consideration. We find that while oscillations around stellar mass black holes are generally consistent with the above models, supermassive black holes are decidedly not. We then compare these results to the orbital resonance, diskoseismic, warped disk, and disk–jet coupling theoretical models for the origin of high-frequency QPOs. We find that supermassive black holes occupy a separate region of parameter space than stellar, and further, that QPOs seen around tidal disruption events rather than Seyfert-type active galactic nuclei (AGN) occupy an entirely different space. In this paper, we compile observations of high-frequency quasi-periodic oscillations (QPOs) around black holes, both stellar and supermassive, and compare their positions in the parameter space of black hole mass, spin, and oscillation frequency.

Black hole accretion disk xray