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Infrared [FeII] and H2 Line Emission in Active Galactic Nuclei

Published online by Cambridge University Press:  07 August 2017

A.F.M. Moorwood  and
E. Oliva
A.F.M. Moorwood
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Str. 2, D-8046 Garching bei München, Fed. Rep. of Germany
E. Oliva
Affiliation:
Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 1-50125 Firenze, Italy

Abstract

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Infrared spectra around [FeII](1.644μm), H2 (v = 1-0 S(1) at 2.121μm) and Brγ (H 7-4 at 2.167μm) have been obtained of 35 emission line nuclei whose optical spectra range from pure HII regionlike to Seyfert 1. All three emission lines have been detected in a large fraction of those nuclei exhibiting starburst activity but not in “pure” Seyferts. The highest detection frequency, however, was found for composite nuclei showing evidence for both starburst and Seyfert activity. Several arguments suggest that both the [FeII] and H2 are shock excited and could be largely attributed to supernova remnants. The fact that the [FeII]/Brγ and H2/Brγ ratios tend to be somewhat larger in composite than in pure starburst nuclei, however, plus significant spatial displacements between the [FeII] and H2 emitting regions found recently during follow-up observations of selected galaxies suggest that large scale phenomena, e.g. SN winds or mass outflows from AGN, may also be important.

Type
Part 7: Dust, Molecules, Infrared and MM Radiation
Information
Symposium - International Astronomical Union , Volume 134: Active Galactic Nuclei , 1989 , pp. 365 - 371
Copyright
Copyright © Kluwer 1989 

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