A two-stage outflow in NGC 1068
  We present an analysis of the Seyfert 2 galaxy NGC 1068 with archive data
from SINFONI-VLT, in the HK bands with pixel scales of 0.1 (data set 1 - DS1)
and 0.025 (DS2) arcsec. The data are revisited with a sophisticated data
treatment, such as the differential atmospheric refraction correction and the
application of a Butterworth filtering and deconvolution. The gain in the
process is quantified by a significant improvement in the Strehl ratio and it
shows that an unprecedented high spatial resolution is achieved. For DS1, a
detailed study of the H$_{2}$, [Fe II] and [Si VI] emission lines reveals a
three-phase gas morphology: (1) the low-velocity [Fe II] emission representing
the glowingwall of an hourglass structure, (2) the high-velocity compact blobs
of low and high ionization emissions filling the hourglass volume and (3) the
distribution of H$_{2}$ molecular gas defines the thick and irregular walls of
a bubble surrounding a cavity. Both the hourglass and the molecular emissions
have an asymmetry caused by the fragmentation of the north-eastern molecular
wall, closest to the active galactic nucleus, resulting in highvelocity compact
blobs of ionized gas outside the bubble. The south-western part of the bubble
is excavated by the jet, where the blobs remain confined and are blown along
the bubble's inner boundary. We propose that those blobs are driven by a hot
"secondary wind" coming from the spot where the jet interacts and injects its
energy in the molecular gas. The combination of a primary wind launched by the
central source and the secondary wind is what we call a two-stage outflow. For
DS2, we detected a [Si VI] outflow nearly coplanar to the maser disc and
orthogonal to the CO outflow found by a previous study. Such unexpected
scenario is interpreted as the interaction between the central radiation field
and a two-phase gas density torus.
