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Helium I λ10830 Observations of Seyfert 2 Galaxies

Published online by Cambridge University Press:  07 August 2017

Ross D. Cohen ,
Richard J. Rudy ,
George S. Rossano ,
R. C. Puetter  and
Scott D. Chapman
Ross D. Cohen
Affiliation:
The Center for Astrophysics and Space Sciences, UCSD, La Jolla, CA 92093 Space Sciences Laboratory, The Aerospace Corporation, M2/266 P.O. Box 92957, Los Angeles, CA 90009
Richard J. Rudy
Affiliation:
The Center for Astrophysics and Space Sciences, UCSD, La Jolla, CA 92093 Space Sciences Laboratory, The Aerospace Corporation, M2/266 P.O. Box 92957, Los Angeles, CA 90009
George S. Rossano
Affiliation:
The Center for Astrophysics and Space Sciences, UCSD, La Jolla, CA 92093 Space Sciences Laboratory, The Aerospace Corporation, M2/266 P.O. Box 92957, Los Angeles, CA 90009
R. C. Puetter
Affiliation:
The Center for Astrophysics and Space Sciences, UCSD, La Jolla, CA 92093 Space Sciences Laboratory, The Aerospace Corporation, M2/266 P.O. Box 92957, Los Angeles, CA 90009
Scott D. Chapman
Affiliation:
The Center for Astrophysics and Space Sciences, UCSD, La Jolla, CA 92093 Space Sciences Laboratory, The Aerospace Corporation, M2/266 P.O. Box 92957, Los Angeles, CA 90009

Extract

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Because of the metastability of the 23S level of He I, a variety of effects can change the line strengths from pure recombination values in Seyfert galaxies (see Feldman and MacAlpine 1978). This occurs because the population which builds up in the 23S level can be collisionally excited to the 23P level, enhancing λ10830. The expected ratios of λ10830/λ5876 can be altered by internal or external reddening and vary with temperature, density and optical depth.

Type
Part 2: BLR and Variability
Information
Symposium - International Astronomical Union , Volume 134: Active Galactic Nuclei , 1989 , pp. 126 - 127
Copyright
Copyright © Kluwer 1989 

References

Antonucci, R.R.J., and Miller, J.S. 1985, Ap. J., 297, 621.CrossRefGoogle Scholar
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