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Infrared interferometry has fuelled a paradigm shift in our understanding ofthe dusty structure in the central parsecs of Active Galactic Nuclei (AGN). Thedust is now thought to comprise of a hot ($\sim1000\,$K) equatorial disk, someof which is blown into a cooler ($\sim300\,$K) polar dusty wind by radiationpressure. In this paper, we utilise the new near-IR interferometer GRAVITY onthe Very Large Telescope Interferometer (VLTI) to study a Type 1.2 AGN hostedin the nearby Seyfert galaxy ESO323-G77. By modelling the squared visibilityand closure phase, we find that the hot dust is equatorially extended,consistent with the idea of a disk, and shows signs of asymmetry in the samedirection. Furthermore, the data is fully consistent with the hot dust sizedetermined by K band reverberation mapping as well as the predicted size from aCAT3D-WIND model created in previous work using the SED of ESO323-G77 andobservations in the mid-IR from VLTI/MIDI.

Resolving the Hot Dust Disk of ESO323-G77