  We have used the Gemini Near-Infrared Integral Field Spectrograph (NIFS) in
the J and K bands to map the distribution, excitation and kinematics of the
ionized HII and warm molecular gas H$_2$, in the inner few 100 pc of 6 nearby
active galaxies: NGC 788, Mrk 607, NGC 3227, NGC 3516, NGC 5506, NGC 5899. {For
most galaxies, this is the first time that such maps have been obtained}. The
ionized and H$_2$ gas show distinct kinematics: while the H$_2$ gas is mostly
rotating in the galaxy plane with low velocity dispersion ($\sigma$), the
ionized gas usually shows signatures of outflows associated with higher
$\sigma$ values, most clearly seen in the [FeII] emission line. These two gas
species also present distinct flux distributions: the H$_2$ is more uniformly
spread over the whole galaxy plane, while the ionized gas is more concentrated
around the nucleus and/or collimated along the ionization axis of its Active
Galactic Nucleus (AGN), presenting a steeper gradient in the average surface
mass density profile than the H$_2$ gas. The total HII masses cover the range
$2\times10^5-2\times10^7$ M$_{\odot}$, with surface mass densities in the range
3-150 M$_{\odot}$ pc$^{-2}$, while for the warm H$_2$ the values are 10$^{3-4}$
times lower. We estimate that the available gas reservoir is at least $\approx$
100 times more massive than needed to power the AGN. If this gas form new stars
the star-formation rates, obtained from the Kennicutt-schmidt scalling
relation, are in the range 1-260$\times$ 10$^{-3}$ M$_{\odot}$ yr$^{-1}$. But
the gas will also - at least in part - be ejected in the form of the observed
otflows.
