TY - JOUR
AU - A. Amorim
AU - M. Bauböck
AU - W. Brandner
AU - M. Bolzer
AU - Y. Clenet
AU - R. Davies
AU - P. de Zeeuw
AU - Jason Dexter
AU - et al.
AB - Using VLTI/GRAVITY and SINFONI data, we investigate the subparsec gas and dust structure around the nearby type 1 active galactic nucleus
(AGN) hosted by NGC3783. The K-band coverage of GRAVITY uniquely allows simultaneous analysis of the size and kinematics of the broad
line region (BLR), the size and structure of the near-infrared(near-IR)-continuum-emitting hot dust, and the size of the coronal line region (CLR).
We find the BLR, probed through broad Br
 emission, to be well described by a rotating, thick disc 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 ten-day time-lag that would be measured,
which closely matches the ten-day time-lag that has been measured by reverberation mapping. We measure a hot dust full-width at half-maximum
(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) oset cloud that
we interpret as an accreting or outflowing cloud heated by the central AGN. Finally, we directly measure the FWHM size of the nuclear CLR
as traced by the [Ca viii] and narrow Br
 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 to 100 pc.
BT - Astronomy & Astrophysics
DA - 2021-04
DO - 10.1051/0004-6361/202040061
N2 - Using VLTI/GRAVITY and SINFONI data, we investigate the subparsec gas and dust structure around the nearby type 1 active galactic nucleus
(AGN) hosted by NGC3783. The K-band coverage of GRAVITY uniquely allows simultaneous analysis of the size and kinematics of the broad
line region (BLR), the size and structure of the near-infrared(near-IR)-continuum-emitting hot dust, and the size of the coronal line region (CLR).
We find the BLR, probed through broad Br
 emission, to be well described by a rotating, thick disc 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 ten-day time-lag that would be measured,
which closely matches the ten-day time-lag that has been measured by reverberation mapping. We measure a hot dust full-width at half-maximum
(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) oset cloud that
we interpret as an accreting or outflowing cloud heated by the central AGN. Finally, we directly measure the FWHM size of the nuclear CLR
as traced by the [Ca viii] and narrow Br
 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 to 100 pc.
PY - 2021
EP - A117
T2 - Astronomy & Astrophysics
TI - The central parsec of NGC 3783: a rotating broad emission line region, asymmetric hot dust structure, and compact coronal line region
UR - https://arxiv.org/abs/2102.00068
VL - 648
ER -