2000ApJ...536..710A

The ISO-SWS(4) 2.5-45 µm infrared spectroscopic observations of the nucleus of the Seyfert 2 galaxy NGC 1068 (see companion paper) are combined with a compilation of UV to IR narrow emission line data to determine the spectral energy distribution (SED) of the obscured extreme-UV continuum that photoionizes the narrow-line-emitting gas in the active galactic nucleus. We search a large grid of gas-cloud models and SEDs for the combination that best reproduces the observed line fluxes and narrow-line region (NLR) geometry. Our best-fit model reproduces the observed line fluxes to better than a factor of 2 on average and is in general agreement with the observed NLR geometry. It has two gas components that are consistent with a clumpy distribution of dense outflowing gas in the center and a more extended distribution of less dense and more clumpy gas farther out that has no net outflow. The best-fit SED has a deep trough at ∼4 rydbergs, which is consistent with an intrinsic Big Blue Bump that is partially absorbed by ∼6x10¹⁹ cm^–2 of neutral hydrogen interior to the NLR.