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 NGC 1275 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 \pm 26 km s ^ { -1 } , which implies a black hole mass of M _ { SMBH } = 1.1 ^ { +0.9 } _ { -0.5 } \times 10 ^ { 9 } M _ { \odot } .
We find hot ( T \gtrsim 1000 K ) molecular and ionized outflows with velocities of up to 2 000 km s ^ { -1 } and mass outflow rates of 2.7 \times 10 ^ { -2 } { M _ { \odot } } yr ^ { -1 } and 1.6 { 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 .