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Optically Thin Gas in the BLR of Seyfert Galaxies

Published online by Cambridge University Press:  07 August 2017

Simon L. Morris  and
Martin J. Ward
Simon L. Morris
Affiliation:
Mount Wilson and Las Campanas Obs., 813 Santa Barbara St., Pasadena, CA 91101
Martin J. Ward
Affiliation:
Institute of Astronomy, Madingley Rd., Cambridge CB3 0HA, England

Extract

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Evidence has been accumulating that the gas which produces the broad line emission (BLR gas) in active galaxies has a range of physical conditions, and may indeed come from a distribution of spatially distinct regions (Gaskell 1982, Ulrich et al. 1984, Netzer 1987, Collin-Soufrin et al. 1988). In this paper, we try to separate out any contribution to the BLR emission line profiles from optically thin material. We do this by comparing the profiles of OI λ8446 (a flourescence line only produced by clouds very optically thick to Lyman α, Elitzur and Netzer 1985) and Hα (which can be produced by optically thick and optically thin clouds).

Type
Part 2: BLR and Variability
Information
Symposium - International Astronomical Union , Volume 134: Active Galactic Nuclei , 1989 , pp. 135 - 136
Copyright
Copyright © Kluwer 1989 

References

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