Ionized and hot molecular outflows in the inner 500 pc of NGC1275
  The role of feedback from Active Galactic Nuclei (AGN) in the evolution of
galaxies is still not not fully understood, mostly due to the lack of
observational constraints in the multi-phase gas kinematics on the ten to
hundred parsec scales. We have used the Gemini Near-infrared Integral Field
Spectrograph (NIFS) to map the molecular and ionized gas kinematics in the
inner 900$\times$900 pc$^2$ of the Seyfert galaxy NGC1275 at a spatial
resolution of $\sim$70 pc. From the fitting of the CO absorption bandheads in
the K-band, we derive a stellar velocity dispersion of $265\pm26$ km s$^{-1}$,
which implies a black hole mass of $M_{\rm SMBH}=1.1^{+0.9}_{-0.5}\times10^9$
M$_\odot$. We find hot ($T\gtrsim1000$ K) molecular and ionized outflows with
velocities of up to 2 000 km s$^{-1}$ and mass outflow rates of
$2.7\times10^{-2} {\rm M_\odot}$ yr$^{-1}$ and $1.6 {\rm M_\odot}$ yr$^{-1}$,
respectively, in each of these gas phases. The kinetic power of the ionized
outflows corresponds to only 0.05 per cent of the luminosity of the AGN of NGC
1275, indicating that they are not powerful enough to provide significant AGN
feedback, but may be effective in redistributing the gas in the central region
of the galaxy. The AGN driven outflows seem to be responsible for the shocks
necessary to produce the observed H$_2$ and [Fe II] line emission.
