We present stellar and gaseous kinematics of the inner \approx 350 pc radius of the Seyfert galaxy Mrk 1066 derived from J and K _ { l } bands data obtained with the Gemini ’ s Near-Infrared Integral Field Spectrograph ( NIFS ) at a spatial resolution of \approx 35 pc .
The stellar velocity field is dominated by rotation in the galaxy plane but shows an S-shape distortion along the galaxy minor axis which seems to be due to an oval structure seen in an optical continuum image .
Along this oval , between 170 and 280 pc from the nucleus we find a partial ring of low \sigma _ { * } ( \approx 50 km s ^ { -1 } ) attributed to an intermediate age stellar population .
The velocity dispersion of the stellar bulge ( \sigma _ { * } \approx 90 km s ^ { -1 } ) implies a super-massive black hole mass of \approx 5.4 \times 10 ^ { 6 } M _ { \odot } .
From measurements of the emission-line fluxes and profiles ( [ P ii ] \lambda 1.1886 \mu m , [ Fe ii ] \lambda 1.2570 \mu m , Pa \beta and H _ { 2 } \lambda 2.1218 \mu m ) , we have constructed maps for the gas centroid velocity , velocity dispersion , as well as channel maps .
The velocity fields for all emission lines are dominated by a similar rotation pattern to that observed for the stars , but are distorted by the presence of two structures : ( i ) a compact rotating disc with radius r \approx 70 pc ; ( ii ) outflows along the radio jet which is oriented approximately along the galaxy major axis .
The compact rotating disc is more conspicuous in the H _ { 2 } emitting gas , which presents the smallest \sigma values ( \leq 70 km s ^ { -1 } ) and most clear rotation pattern , supporting a location in the galaxy plane .
We estimate a gas mass for the disc of \sim 10 ^ { 7 } { M _ { \odot } } .
The H _ { 2 } kinematics further suggests that the nuclear disc is being fed by gas coming from the outer regions .
The outflow is more conspicuous in the [ Fe ii ] emitting gas , which presents the highest \sigma values ( up to 150 km s ^ { -1 } ) and the highest blue and redshifts of up to 500 km s ^ { -1 } , while the highest stellar rotation velocity is only \approx 130 km s ^ { -1 } .
We estimate a mass-outflow rate in ionized gas of \approx 6 \times 10 ^ { -2 } { M _ { \odot } yr ^ { -1 } } .
The derived kinematics for the emitting gas is similar to that observed in previous studies supporting that the H _ { 2 } is a tracer of the AGN feeding and the [ Fe ii ] of its feedback .