The central parsec of NGC 3783: a rotating broad emission line region,
  asymmetric hot dust structure, and compact coronal line region
  Using VLTI/GRAVITY and SINFONI data, we investigate the sub-pc gas and dust
structure around the nearby type 1 AGN hosted by NGC 3783. The K-band coverage
of GRAVITY uniquely allows a simultaneous analysis of the size and kinematics
of the broad line region (BLR), the size and structure of the near-IR continuum
emitting hot dust, and the size of the coronal line region (CLR). We find the
BLR probed through broad Br$\gamma$ emission is well described by a rotating,
thick disk with a radial distribution of clouds peaking in the inner region. In
our BLR model the physical mean radius of 16 light days is nearly twice the 10
day time lag that would be measured, which matches very well the 10 day time
lag that has been measured by reverberation mapping. We measure a hot dust FWHM
size of 0.74 mas (0.14 pc) and further reconstruct an image of the hot dust
which reveals a faint (5% of the total flux) offset cloud which we interpret as
an accreting cloud heated by the central AGN. Finally, we directly measure the
FWHM size of the nuclear CLR as traced by the [CaVIII] and narrow Br$\gamma$
line. We find a FWHM size of 2.2 mas (0.4 pc), fully in line with the
expectation of the CLR located between the BLR and narrow line region.
Combining all of these measurements together with larger scale near-IR integral
field unit and mid-IR interferometry data, we are able to comprehensively map
the structure and dynamics of gas and dust from 0.01--100 pc.
