2019MNRAS.487.3958D

We present a 2D mapping of stellar population age components, emission-line fluxes, gas excitation, and kinematics within the inner ∼200 pc of the Seyfert 2 galaxy NGC 2110. We used the Gemini North Integral Field Spectrograph (NIFS) in the J and K bands at a spatial resolution of ∼22 pc. The unresolved nuclear continuum is originated in combined contributions of young stellar population (SP; age <= 100 Myr), a featureless AGN continuum and hot dust emission. The young-intermediate SP (100 < age <= 700 Myr) is distributed in a ring-shaped structure at ≃140 pc from the nucleus, which is roughly coincident with the lowest values of the stellar velocity dispersion. In the inner ≃115 pc the old SP (age > 2 Gyr) is dominant. The [Fe II] λ1.2570 µm emission-line flux distribution is correlated with the radio emission and its kinematics comprise two components, one from gas rotating in the galaxy plane and another from gas in outflow within a bicone-oriented along north-south. These outflows seem to originate in the interaction of the radio jet with the ambient gas producing shocks that are the main excitation mechanism of the [Fe II] emission. We estimate: (1) an ionized gas mass outflow rate of ∼0.5 M_☉ yr^–1 at ∼70 pc from the nucleus; and (2) a kinetic power for the outflow of only 0.05 per cent of the AGN bolometric luminosity implying weak feedback effect on the galaxy.