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PHOTOIONIZATION OF HIGH-LATITUDE GAS IN NGC 891

NGC 891 by the UV radiation from various in situ stellar populations. We find that although OB stars dominate the production of stellar UV photons, models using only OB stars cannot reproduce the observed [N II] λ6584/Hα ratios seen throughout this diffuse ionized medium (DIM). Models that combine OB stars with the high-temperature end of the white-dwarf distribution and the central stars of planetary nebulae are capable of reproducing the observed [N II] λ6584/Hα ratios. Estimation of ionizing photon fluxes, using free-free and infrared emission, combined with these models requires the filling factor throughout the DIM in NGC 891 to be of order 10-2^ and that white dwarfs and planetary nebula central stars contribute ~25% of the ionizing photons at |z| = 250 pc. Our model results indicate that the filling factor of the DIM in the Milky Way is approximately 10-1^, in agreement with previous estimates.