INFRARED-SPECTROSCOPY OF PA-BETA AND [FE-II] EMISSION IN NGC-4151

We present spatially resolved 1.24-1.30 mu m spectroscopy with a resol ution of 240 km/s of the Seyfert 1.5 galaxy NGC 4151. Broad Pa beta, n arrow Pa beta, and narrow [Fe II] (lambda=1.2567 mu m) emission lines are identified in the spectrum. Additionally, a spatially unresolved n arrow component probably due to [S IX] (lambda=1.25235 mu m) is observ ed on the nucleus. The narrow Pa beta and [Fe II] lines are observed t o be extended over a scale of 5''. The spatial variation of the veloci ty centers of the Pa beta and [Fe II] lines show remarkable similarity , and additionally show similarities to the velocity structure previou sly observed in ground based spectroscopy of [O III] emission in NGC 4 151. This leads to the conclusion that the [Fe II] emission arises in clouds in the Seyfert narrow line region that are physically correlate d with those narrow line clouds responsible for the optical emission. The [Fe II] emission line, however, is significantly wider than the Pa beta emission line along the full spatial extent of the observed emis sion. This result suggests that despite the correlation between the bu lk kinematics of Pa beta and [Fe II], then is an additional process, p erhaps fast shocks from a wind in the Seyfert nucleus, contributing to the [Fe II] emission. (C) 1996 American Astronomical Society.