Results from an analysis of low resolution ( R \sim 250 ) near-IR long-slit spectra covering simultaneously the I , J , H , and K bands , for a sample of 15 Seyfert galaxies and the NGC 5253 starburst nucleus , are presented .
The Seyfert galaxies were selected as presenting ‘ linear ’ or cone-like high excitation emission line in the optical , most probably due to the collimation of the central source ’ s radiation by a dusty molecular torus .
Our goal was to look for signatures of this torus , and to investigate the gaseous distribution , excitation and reddening .
The strongest emission lines detected are usually He i 1.083 \mu m and [ S iii ] \lambda 9532 , followed by Pa \beta .
In some cases , [ Fe ii ] 1.26 \mu m and 1.64 \mu m are also seen .
[ Fe ii ] 1.26 \mu m and H _ { 2 } \nu =1 - 0 S ( 1 ) are detected in some of the higher resolution spectra obtained for five galaxies .
The emission lines are spatially extended in most cases , and we have used the [ Fe ii ] /Pa \beta ratio as a measure of the gaseous excitation in Mrk 573 , NGC 1386 , and NGC 7582 .
Values for this ratio between 1.5 and 6 are found , suggesting excitation of [ Fe ii ] by X-rays or shock waves in some regions .
Broad permitted lines are observed in three Seyfert 1 galaxies .
Nuclear Pa \beta in NGC 1365 , and possibly nuclear Br \gamma in Mrk 573 , are also broad .

From analysis of the spatial distribution of the continuum ( J - H ) and ( H - K ) colours derived from our spectra , we find redder colours for the nucleus than the nearby bulge in most of the Seyfert 2s observed .
Comparison with models including emission from dust and stars shows that hot ( T \sim 1000 K ) dust emission dominates the nuclear continuum in NGC 1365 , NGC 2110 , NGC 3281 , NGC 7582 , and ESO362-G18 .
In NGC 1386 , NGC 5643 , and NGC 5728 the main contributor is the underlying stellar population , combined with some foreground reddening and/or cooler dust emission .
In a few cases , the ( J - H ) colours on opposite sides of the nucleus differ by 0.3 – 0.8 mag , an effect that we interpret as partly due to differences in the local stellar population , and possibly extinction gradients .