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We compile observations of high-frequency quasi-periodic oscillations (QPOs)around black holes, both stellar and supermassive, and compare their positionsin the parameter space of black hole mass, spin, and oscillation frequency. Wefind that supermassive black holes occupy a separate region of parameter spacethan stellar, and further, that QPOs seen around tidal disruption events ratherthan Seyfert-type AGN occupy an entirely different space. We then compare theseresults to the orbital resonance, diskoseismic, warped disk, and disk-jetcoupling theoretical models for the origin of high-frequency QPOs. We find thatwhile oscillations around stellar mass black holes are generally consistentwith the above models, supermassive black holes are decidedly not. Oscillationsseen in tidal disruption events are consistent with oscillations near thefrequency of the innermost stable circular orbit (ISCO), while QPOs in AGN arenot accounted for by any of the physical models in consideration. Thisindicates that despite the scale invariance of accretion processes implied by adecades-wide correlation between QPO frequency and black hole mass, any theoryof high frequency QPOs must relate the frequency to more than just the mass andspin.

Confrontation of Observation and Theory: High Frequency QPOs in X-ray Binaries, Tidal Disruption Events, and Active Galactic Nuclei