  We present a two-dimensional mapping of stellar population age components,
emission-line fluxes, gas excitation and kinematics within the inner $\sim200$
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 $\sim22$
pc. The unresolved nuclear continuum is originated in combined contributions of
young stellar population (SP; age$\leq100$ Myr), a featureless AGN continuum
and hot dust emission. The young-intermediate SP ($100<$age$\leq700$ Myr) is
distributed in a ring-shaped structure at $\approx140$ pc from the nucleus,
which is roughly coincident with the lowest values of the stellar velocity
dispersion. In the inner $\approx115$ pc the old SP (age$>2$ Gyr) is dominant.
The [FeII]1.25$\mu$m 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 [FeII] emission. We estimate: (1) an ionized gas
mass outflow rate of $\sim0.5$ M$_\odot$/yr at $\sim$70 pc from the nucleus;
and (2) a kinetic power for the outflow of only 0.05% of the AGN bolometric
luminosity implying weak feedback effect on the galaxy.
