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We present high resolution ($R=2200-3300$, $\sim 120-100$ km/s), IR spectra of [FeII] 1.644 $\mu m$, H$_2$ 2.121 $\mu m$, and Br$\gamma$ of 12 Seyfert galaxies (3 Sy1, 9 Sy2) selected from relatively homogeneous and unbiased samples (CfA, 12 $\mu m$, and RSA catalogs). Strengths, line profiles, and line ratios ([FeII]/Br$\gamma$, H$_2$/Br$\gamma$) are used to analyze the physical conditions in the line-emitting regions, as well as the energetic origin of these lines as a function of Seyfert type. We discuss the origin of the [FeII] emission, both by analysis of line widths and through comparison of AGN line ratios with those in starburst galaxies. We hope to distinguish whether the [FeII] is related to stellar processes or arises due to the presence of an AGN wind.
