  The near-infrared spectra of Active Galactic Nuclei (AGN) present emission
lines of different atomic and molecular species. The mechanisms involved in the
origin of these emission lines in AGN are still not fully understood. We use J
and K band integral field spectra of six luminous ($43.1<\log L_{\rm bol}/({\rm
erg s^{-1}})<44.4$) Seyfert galaxies (NGC 788, Mrk 607, NGC 3227, NGC 3516, NGC
5506 and NGC 5899) in the Local Universe ($0.0039<z<0.0136$) to investigate the
gas excitation within the inner 100-300 pc radius of the galaxies at spatial
resolutions of a few tens of parsecs. In all galaxies, the H$_2$ emission
originates from thermal processes with excitation temperatures in the range
2400-5200 K. In the high line ratio (HLR) region of the H$_2$/Br$\gamma$ vs.
[Fe II]/Pa$\beta$ diagnostic diagram, which includes 29 % of the spaxels,
shocks are the main excitation mechanism, as indicated by the correlation
between the line widths and line ratios. In the AGN region of the diagram (64 %
of the spaxels) the H$_2$ emission is due to the AGN radiation. The [Fe II]
emission is produced by a combination of photoionisation by the AGN radiation
and shocks in five galaxies and is dominated by photoionisation in NGC 788. The
[S IX]1.2523$\mu$m coronal emission line is present in all galaxies, and its
flux distributions are extended from 80 to 185 pc from the galaxy nuclei,
except for NGC 5899, in which this line is detected only in the integrated
spectrum.
