The Origin of the Blue Featureless Continuum in Seyfert 2 Nuclei: CYCLE3MEDIUM

Details The Origin of the Blue Featureless Continuum in Seyfert 2 Nuclei: CYCLE3MEDIUM The Origin of the Blue Featureless Continuum in Seyfert 2 Nuclei: CYCLE3MEDIUM

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993hst..prop.4340f&link_type=abstract

HST Proposal ID #4340

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Hst Proposal Id #4340

Scientific paper

Recent spectropolarimetric studies of Seyfert 2 nuclei have shown that NGC 4922B has very low polarization, despite having a rather prominent blue featureless continuum (BFC). Broad permitted lines also appear to be absent, both in direct and reflected light. These observed characteristics conflict with the predictions of simple Seyfert unified models, which assume that the viewing angle is the only parameter that determines whether the object appears as a Seyfert 1 or a Seyfert 2 nucleus. If all Seyfert 2s behave like the prototypical NGC 1068, it is expected that the BFC should be polarized at least a few percent and that broad lines be present in polarized light. A possible explanation for NGC 4922B is that the classical broad-line region does not exist in this object. We should be able to test this by examining the line profiles of Ly-alpha, C IV, and Mg II. If this object does indeed harbor a hidden Seyfert 1 nucleus, we should also be able to detect broad Fe II emission in the UV. Another possibility is that the BFC originates from a population of hot stars. Much evidence has recently been accumulated that hot stars may play a significant role in Seyfert 2 nuclei. If so, then FOS spectra should reveal stellar absorption features (e.g., C IV, Si IV), and FOC images should appear extended. The shape of the UV continuum will also be useful in discriminating between a stellar or an AGN ionizing source. We believe that this study has important implications for the Seyfert unified model.

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