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Kinematics and excitation mechanisms of molecular hydrogen and [FeII] lines in active galactic nuclei

Published online by Cambridge University Press:  24 November 2004

M. G. Pastoriza ,
Alberto Rodriguez-Ardila ,
Sueli Viegas ,
T. A. A. Sigut  and
Anil K. Pradhan
M. G. Pastoriza
Affiliation:
Departamento de Astronomia, Instituto de Fisica, UFRGS, Av. Bento Gonçalves 9500, C.P. 15051, 91501-970, Porto Alegre, RS, Brazil
Alberto Rodriguez-Ardila
Affiliation:
Laboratorio Nacional de Astrofisica/CNPq, Brasopolis, MG, Brazil
Sueli Viegas
Affiliation:
Instituto de Astronomia, Geofisica e Ciencias Atmosfericas, USP, Sao Paulo, SP, Brazil
T. A. A. Sigut
Affiliation:
Department of Physics and Astronomy, The University of Western Ontario, London, ON, N6A 3K7, Canada
Anil K. Pradhan
Affiliation:
Department of Astronomy, The Ohio State University, Columbus, OH, US 43210-1106, USA
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Abstract

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Near-infrared spectroscopic observations in the range 0.8-2.4μm are used to study the kinematics and excitation mechanisms of Molecular Hydrogen and [FeII] lines in a sample of AGNs. The width of H2 lines is narrower than [FeII] lines, therefore they do not originate from the same parcel of gas. The molecular emission is found to be purely thermal but with heating processes which vary among the objects. A clear correlation between H2/Brγ and [FeII] 1.257μm/Paβ is found for our sample objects supplemented with data from the literature. The correlation of these line ratios is a useful diagnostic tool in the NIR to separate emitting line objects by their level of nuclear activity.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
ORAL CONTRIBUTIONS
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS222 , March 2004 , pp. 279 - 282
Copyright
© 2004 International Astronomical Union