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Astronomical observations of the PAH emissionbands

Published online by Cambridge University Press:  30 March 2011

C. Joblin ,
A.G.G.M. Tielens  and
E. Peeters
E. Peeters*
Affiliation:
Department of Physics and Astronomy, University of Western Ontario, London, ON N6A 3K7, Canada SETI Institute, 189 N. Bernardo Ave., Suite 100, Mountain View, CA 94043, USA

Abstract

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The infrared (IR) spectra of many galactic and extragalactic objects are dominated byemission features at 3.3, 6.2, 7.7, 8.6 and 11.2 μm, generally attributedto the IR fluorescence of Polycyclic Aromatic Hydrocarbon molecules (PAHs). These PAHbands have been found in a wide variety of environments throughout theUniverse and containup to 10% of the total power output of star-forming galaxies.

Ground-based telescopes, the Infrared Space Observatory (ISO) and the Spitzer SpaceTelescope revealed a plethora of weaker PAH bands and provided extensive evidence forsignificant variability in the PAH spectrum from source to source and spatially withinsources. Here we review the spectral characteristics of astronomical PAHs, theirdependence on the local physical conditions and the implications for the physical andchemical characteristics of the carriers.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 46: PAHs and the Universe: A Symposium to Celebrate the 25th Anniversary of the PAH Hypothesis , 2011 , pp. 13 - 27
Copyright
© EAS, EDP Sciences 2011

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