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Broad line regions of many AGN frequently show strong optical Fe II emission. The origin of this is not understood, nor is the mystery of why the optical Fe II emission is strong in some objects and much weaker in others. Gaskell (1985, ApJ, 291, 112) found that the AGNs with the narrowest broad lines appeared to have the weakest Balmer lines. Since, for some models of Fe II emission, this might imply differences in the high ionization lines, we obtained UV spectra of Mrk 42 and Mrk 957, two of the most extreme examples of AGNs with strong and very narrow optical Fe II emission. We compare these spectra with UV spectra of more "normal" AGNs with less extreme (or no) optical Fe II emission and with broader broad lines and we discuss the results in terms of various models of AGNs.
This research was funded in part by NASA grant NAG5-1001.
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