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Near-Infrared Emission-Line Spectra of the Orion Nebula, NGC 4151, and Other Seyfert Galaxies

Published online by Cambridge University Press:  07 August 2017

D. E. Osterbrock ,
R. A. Shaw  and
S. Veilleux
D. E. Osterbrock
Affiliation:
Lick Observatory, University of California, Santa Cruz, CA 95064
R. A. Shaw
Affiliation:
Lick Observatory, University of California, Santa Cruz, CA 95064
S. Veilleux
Affiliation:
Lick Observatory, University of California, Santa Cruz, CA 95064

Extract

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CCDs make the near-infrared spectral region out to about 1.1 μ observable. A good deal of information on the spectra of AGNs in this range has been published, which we are trying to systematize and extend at Lick. Our original lens-grism spectrograph camera is opaque over the region λ8600-λ10250, no doubt as a result of a coating on one of the elements of the Nikon lens, making this program impossible with it. However our newer “UV-Schmidt” camera is quite effective in this region. With it we have obtained well exposed spectra at moderate resolution (FWHM ≈ 7 Å) of NGC 4151 in three overlapping segments covering the region 7000–11000 Å. Also, for comparison we obtained similar spectra of NGC 1976, the Orion Nebula. The wavelengths and relative line fluxes were measured, and most of the lines were identified. The strongest three lines in both objects are, in order, [S III] λ9532, He I λ10830, and [S III] λ9069. The Orion Nebula spectrum is very helpful for identifying lines in NGC 4151, and for comparison with it. Among the lines identified in NGC 1976, many of them previously known, are [O II], [S II], [Ar III], [Fe II], [Ni II], [Ni III], [Cl II], [C I], in addition to O I λ8446, many H I Paschen lines and He I.

Type
Part 5: Structure of the Central Object and NLR
Information
Symposium - International Astronomical Union , Volume 134: Active Galactic Nuclei , 1989 , pp. 298 - 300
Copyright
Copyright © Kluwer 1989 

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