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Geometrically thick accretion flows may be present in black hole X-raybinaries observed in the low/hard state and in low-luminosity active galacticnuclei. Unlike in geometrically thin disks, the angular momentum axis in thesesources is not expected to align with the black hole spin axis. We computeimages from three-dimensional general relativistic magnetohydrodynamicsimulations of misaligned (tilted) accretion flows using relativistic radiativetransfer, and compare the estimated locations of the radiation edge withexpectations from their aligned (untilted) counterparts. The radiation edge inthe tilted simulations is independent of black hole spin for a tilt of 15degrees, in stark contrast to the results for untilted simulations, which agreewith the monotonic dependence on spin expected from thin accretion disk theory.Synthetic emission line profiles from the tilted simulations depend strongly onthe observer's azimuth, and exhibit unique features such as broad "blue wings."Coupled with precession, the azimuthal variation could generate timefluctuations in observed emission lines, which would be a clear "signature" ofa tilted accretion flow. Finally, we evaluate the possibility that the observedlow- and high-frequency quasi-periodic oscillations (QPOs) from black holebinaries could be produced by misaligned accretion flows. Althoughlow-frequency QPOs from precessing, tilted disks remains a viable option, wefind little evidence for significant power in our light curves in the frequencyrange of high-frequency QPOs.

Observational Signatures of Tilted Black Hole Accretion Disks from Simulations