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Calcium Infrared Triplet Emission in AGN

Published online by Cambridge University Press:  07 August 2017

S. E. Persson  and
G. J. Ferland
S. E. Persson
Affiliation:
Mt. Wilson and Las Campanas Observatories, 813 Santa Barbara St., Pasadena, CA 91101
G. J. Ferland
Affiliation:
Dept. of Astronomy, Ohio State University, Columbus, OH 43210

Abstract

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Emission in the Ca II infrared triplet lines has been detected in 15 AGN. Correlations with optical Fe II emission and O I λ8446 linewidths indicate that Ca II emission comes from neutral gas within the BLR. A new series of ionization models that extend to column densities NH of 1025 cm−2 match the Ca II line strengths and various line ratios. The solution to the Ca II problem, which also solves the “Fe II problem” and the “energy puzzle”, is that a small amount of H− dominates the heating, even for NH ∼1022 cm−2, by absorbing the powerful near-infrared (1 μm) continuum.

Type
Part 5: Structure of the Central Object and NLR
Information
Symposium - International Astronomical Union , Volume 134: Active Galactic Nuclei , 1989 , pp. 293 - 295
Copyright
Copyright © Kluwer 1989 

References

Collin-Souffrin, S., 1986, Astr.Ap., 166, 115.Google Scholar
Davidson, K., and Netzer, H 1979, Rev. Mod. Phys., 51, 715.Google Scholar
Ferland, G. J., and Rees, M. J. 1988, preprint.Google Scholar
Mathews, W. G., and Ferland, G. J. 1987, Ap.J., 323, 456.Google Scholar
Netzer, H. 1985, Ap.J., 289, 451.Google Scholar
Persson, S. E. 1988, Ap.J., 330, 751.Google Scholar