My dissertation project focuses on determining the underlying physical cause of a Seyfert galaxy's appearance as type a 1.8 or 1.9. Are these "intermediate" Seyfert types typical Seyfert 1 nuclei reddened by central dusty tori or by nuclear dust lanes/spirals in the narrow-line region? Or, are they similar to NGC 2992, objects that have intrinsically weak continua and weak broad emission lines? My study compares measurements of the reddenings of the narrow and broad-line regions with each other and with the X-ray column derived from {\it XMM Newton} 0.5-10 keV spectra to determine the presence and location of dust in the line of sight. .