The Distribution of X-ray Column Densities in Seyfert 1.8 and 1.9 Galaxies

Details The Distribution of X-ray Column Densities in Seyfert 1.8 and 1.9 Galaxies The Distribution of X-ray Column Densities in Seyfert 1.8 and 1.9 Galaxies

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.0806t&link_type=abstract

American Astronomical Society, HEAD meeting #11, #8.06; Bulletin of the American Astronomical Society, Vol. 41, p.663

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Seyfert 1.8 and 1.9 galaxies are often fit into the unified model of AGN as objects viewed along a line of sight that grazes the outer edge of a central obscuring torus. This picture was supported by Risaliti et al. (1999), who reported that the gas columns from X-ray observations of Seyfert 1.8 and 1.9 galaxies are significantly less than in Seyfert 2s, though still larger than in Seyfert 1s. However, when we obtained new optical spectra of a sample of 32 objects classified intermediate-type Seyferts, careful de-convolution of the H-alpha line from [N II] showed that most of the ``1.8 and 1.9s'' in Risaliti's original sample were misclassified, or changed optical type over time. For the five objects that do appear as 1.8s and 1.9s in our optical spectra that were previously observed by XMM, we downloaded and fit spectral models to their archival EPIC pn data. While the XMM spectra show significant absorption, none of the objects are heavily obscured by Seyfert 2-like columns, thus confirming the result of Risaliti et al., that (non-variable) intermediate Seyferts are absorbed by intermediate columns. These results suggest that some Seyfert 1.8/1.9s (those that do not change type) appear to have weak broad lines due to reddening of their broad-line regions, while others (those that change type) may simply be Seyfert 1s experiencing a temporary drop in ionizing continuum flux.

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