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AGN Spectra as Seen by the Infrared Space Observatory: First Results

Published online by Cambridge University Press:  12 April 2016

D. Lutz ,
R. Genzel ,
E. Sturm ,
A.F.M. Moorwood ,
E. Oliva ,
A. Marconi  and
H. Netzer
D. Lutz
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik, Postfach 1603, 85740 Garching, Germany
R. Genzel
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik, Postfach 1603, 85740 Garching, Germany
E. Sturm
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik, Postfach 1603, 85740 Garching, Germany
A.F.M. Moorwood
Affiliation:
European Southern Observatory, Garching, Germany
E. Oliva
Affiliation:
Osservatorio Astrofisico di Arcetri, Firenze, Italy
A. Marconi
Affiliation:
Osservatorio Astrofisico di Arcetri, Firenze, Italy
H. Netzer
Affiliation:
School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel

Abstract

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We discuss 2.5–45 µm spectra of the Circinus galaxy and of Cen A, obtained with the Short Wavelength Spectrometer (SWS) on board the Infrared Space Observatory. The large number of detected ionic fine structure lines, observable also in visually obscured sources, provides strong constraints on the shape of the ionizing spectrum, which is found to exhibit a UV bump peaking at ~ 70 eV in the case of Circinus. Pure rotational emission of molecular hydrogen, directly probing warm molecular gas, can for the first time be detected in external galaxies.

Type
VI. The Narrow-Line Regions and Beyond
Information
International Astronomical Union Colloquium , Volume 159: Emission Lines in Active Galaxies: New Methods and Techniques , 1997 , pp. 333 - 336
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

Matt, G., et al. 1996, MNRAS, 281, L69.Google Scholar
Moorwood, A.F.M., Lutz, D., Oliva, E., Marconi, A., Netzer, H., Genzel, R., Sturm, E., & de Graauw, Th. 1996, A&A, submitted.Google Scholar
Oliva, E., Salvati, M., Moorwood, A.F.M., & Marconi, A. 1994, A&A, 288, 457.Google Scholar
Sturm, E., Lutz, D., & Genzel, R., 1997, this volume.Google Scholar