A Multi-Wavelength Investigation of Seyfert 1.8 and 1.9 Galaxies

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Our current study focuses on determining the cause of a Seyfert galaxy's appearance as an "intermediate type” AGN, characterized by an optical spectrum with a weaker featureless continuum and weaker broad Balmer emission lines than a Type 1 AGN. Are most Seyfert 1.8/1.9 galaxies typical Seyfert 1 nuclei observed via a line of sight that grazes the edge of a dusty central torus, which obscures most of the broad emission-line region except the strongest line, Hα, and perhaps the next strongest, Hβ? Or are they similar to NGC 2992, objects that have intrinsically weak continua and smallish broad components, which may be diminished or even extinguished by dust in the host galaxy? Using new ground-based optical spectra and a variety of archival data from other wavelength regimes as clues to the underlying physical situation, we attempt to sort out the apparently diverse category of "intermediate Seyferts” into one of these groups. In this way, we hope to isolate those Seyferts suitable for use in studies of the dust and gas properties of the torus from those in which the optical extinction is unrelated to the torus.

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