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Astronomical observations of the PAH emission bands

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 by emission features at 3.3, 6.2, 7.7, 8.6 and 11.2 μm, generally attributed to the IR fluorescence of Polycyclic Aromatic Hydrocarbon molecules (PAHs). These PAH bands have been found in a wide variety of environments throughout theUniverse and contain up to 10% of the total power output of star-forming galaxies.

Ground-based telescopes, the Infrared Space Observatory (ISO) and the Spitzer Space Telescope revealed a plethora of weaker PAH bands and provided extensive evidence for significant variability in the PAH spectrum from source to source and spatially within sources. Here we review the spectral characteristics of astronomical PAHs, their dependence on the local physical conditions and the implications for the physical and chemical 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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