ALMA backed NIR high resolution integral field spectroscopy of the NUGA
  galaxy NGC 1433
  We present the results of near-infrared (NIR) H- and K-band European Southern
Observatory SINFONI integral field spectroscopy (IFS) of the Seyfert 2 galaxy
NGC 1433. We present emission and absorption line measurements in the central
kpc of NGC 1433. We detect a narrow Balmer line and several H2 lines. We find
that the stellar continuum peaks in the optical and NIR in the same position,
indicating that there is no covering of the center by a nuclear dust lane. A
strong velocity gradient is detected in all emission lines at that position.
The position angle of this gradient is at 155\deg whereas the galactic rotation
is at a position angle of 201\deg. Our measures of the molecular hydrogen
lines, hydrogen recombination lines, and [Feii] indicate that the excitation at
the nucleus is caused by thermal excitation, i.e. shocks which can be
associated with active galactic nuclei emission, supernovae or outflows. The
line ratios [Feii]/Pa{\beta} and H2/Br{\gamma} show a Seyfert to LINER
identification of the nucleus. The stellar continuum is dominated by spectral
signatures of red-giant M stars. The stellar line-of-sight velocity follows the
galactic field whereas the light continuum follows the nuclear bar. The
dynamical center of NGC 1433 coincides with the optical and NIR center of the
galaxy and the black hole position. Within the central arcsecond, the molecular
hydrogen and the 12CO(3-2) emissions - observed in the NIR and in the
sub-millimeter with SINFONI and ALMA, respectively - are indicative for a
nuclear outflow originating from the galaxy's SMBH. A small circum nuclear disk
cannot be fully excluded. Derived gravitational torques show that the nuclear
bar is able to drive gas inwards to scales where viscosity torques and
dynamical friction become important. The black hole mass derived using stellar
velocity dispersion is 10^7 M_sun.
