Dust in the Broad-Line Regions of Seyfert Galaxies

Details Dust in the Broad-Line Regions of Seyfert Galaxies Dust in the Broad-Line Regions of Seyfert Galaxies

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6704g&link_type=abstract

HST Proposal ID #6704

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Hst Proposal Id #6704 Agn

Scientific paper

The classes of objects called Seyfert 1.8 and Seyfert 1.9galaxies show weak broad Balmer lines and a weak nonstellarcontinuum. Two theories have been proposed to explain theircharacteristics: (1) dust along the line of sight to the broad-line region (BLR) and the continuum reddens and weakens thenuclear spectrum, and (2) low optical depth and low ionizationparameter in the BLR, which has been shown to give largeBalmer decrements. These competing theories can be criticallytested by observing both LyAlpha and HAlpha and comparingtheir strengths. In the reddening hypothesis LyAlpha should bereduced by a factor of ~ 10^-4 from its intrinsic value, whilein the other hypothesis the LyAlpha/HAlpha ratio should besimilar to that seen in Seyfert 1 galaxies. We will use theGHRS and ground-based spectroscopy to obtain nearlysimultaneous LyAlpha and HAlpha spectra of eight Seyfert 1.8and 1.9 galaxies. This will provide a clear and unambiguoustest of the two theories discussed above.

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