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We have mapped the emission-line flux distributions and ratios as well as thegaseous kinematics of the inner 450 pc radius of the Seyfert 1 galaxy Mrk 766using integral field near-IR J- and Kl-band spectra obtained with the Gemininifs at a spatial resolution of 60 pc and velocity resolution of 40 km/s.Emission-line flux distributions in ionized and molecular gas extend up to ~300 pc from the nucleus. Coronal [S IX]{\lambda}1.2523{\mu}m line emission isresolved, being extended up to 150 pc from the nucleus. At the highest fluxlevels, the [Fe II]{\lambda}1.257{\mu}m line emission is most extended to thesouth-east, where a radio jet has been observed.The emission-line ratios [FeII]{\lambda}1.2570{\mu}m/Pa{\beta} and $H_2${\lambda}2.1218{\mu}m/Br{\gamma}show a mixture of Starburst and Seyfert excitation; the Seyfert excitationdominates at the nucleus, to the north-west and in an arc-shaped region between0.2" and 0.6" to the south-east at the location of the radio jet. Acontribution from shocks at this location is supported by enhanced [Fe II]/[PII] line ratios and increased [Fe II] velocity dispersion. The gas velocityfield is dominated by rotation that is more compact for $H_2$ than forPa{\beta}, indicating that the molecular gas has a colder kinematics and islocated in the galaxy plane. There is about $10^3$ solar masses of hot $H_2$,implying ~ $10^9$ solar masses of cold molecular gas. At the location of theradio jet, we observe an increase in the [Fe II] velocity dispersion (150km/s), as well as both blueshift and redshifts in the channel maps, supportingthe presence of an outflow there. The ionized gas mass outflow rate isestimated to be ~ 10 solar masses/yr, and the power of the outflow ~ 0.08$L_{bol}$.

Feeding Versus Feedback in AGNs from Near-Infrared IFU Observations: The Case of Mrk 766