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Properties of Warm Absorbers and Constraints from their Optical and UV Line Emission

Published online by Cambridge University Press:  12 April 2016

Stefanie Komossa  and
Henner Fink
Stefanie Komossa
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik, D-85740 Garching, Germany
Henner Fink
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik, D-85740 Garching, Germany

Extract

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We have studied the warm absorbers in several Seyfert galaxies using both PI and archival ROSAT data. The parameters that govern the emissivity of the ionized material, ionization parameter U, warm-absorber column density Nwa, and the source intrinsic power-law photon index Γx, are determined from X-ray spectral fits. These are then used to predict the expected IR to UV line emission of the ionized material in the individual objects. In particular, the possibility of a warm-absorber origin of one of the known emission-line regions in AGN is assessed. Good ‘candidate components’ are, e.g., the coronal-line region, and/or the high-ionization component of the NLR, or the component responsible for broad wings in the Balmer lines. All calculations have been carried out using the code CLOUDY (Ferland 1993).

Type
V. Emission Lines, Absorption Lines, the Continuum, and their Relationships
Information
International Astronomical Union Colloquium , Volume 159: Emission Lines in Active Galaxies: New Methods and Techniques , 1997 , pp. 246 - 247
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

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