Resolving the Hot Dust Disk of ESO323-G77
  Infrared interferometry has fuelled a paradigm shift in our understanding of
the dusty structure in the central parsecs of Active Galactic Nuclei (AGN). The
dust is now thought to comprise of a hot ($\sim1000\,$K) equatorial disk, some
of which is blown into a cooler ($\sim300\,$K) polar dusty wind by radiation
pressure. In this paper, we utilise the new near-IR interferometer GRAVITY on
the Very Large Telescope Interferometer (VLTI) to study a Type 1.2 AGN hosted
in the nearby Seyfert galaxy ESO323-G77. By modelling the squared visibility
and 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 same
direction. Furthermore, the data is fully consistent with the hot dust size
determined by K band reverberation mapping as well as the predicted size from a
CAT3D-WIND model created in previous work using the SED of ESO323-G77 and
observations in the mid-IR from VLTI/MIDI.
