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Observations of Interstellar Carbon Compounds

Published online by Cambridge University Press:  30 March 2011

C. Joblin ,
A.G.G.M. Tielens  and
E. Dartois
E. Dartois*
Affiliation:
Institut d’Astrophysique Spatiale, UMR-8617, Université Paris-Sud, Bâtiment 121, 91405 Orsay, France

Abstract

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Infrared absorption and emission features observed spectroscopically in our Galaxy allowto probe the composition of solid dust grains, their evolution and thus follow the cyclingof matter in the Galaxy. Many observables do reveal the presence of large amounts ofcarbonaceous particles in space, other than the PAH-like emission lines. The carbonaceousmaterials observed include amorphous carbons, diamondoids showing in emission for a fewspecific sources, and the recently detected fullerenes. An important hydrogenatedamorphous carbon component (HAC or a-C:H), traced by the 2940 cm-1 structuredabsorption feature is observed against Galactic background sources. Since the discovery ofthis feature in the early eighties (Allen 1981), theobservation of a-C:H has been extended to the mid-infrared by space observatories, givinginsight into additional associated features. They are also observed in external galaxies,showing the ubiquitous nature of these components. We will focus on astronomicalobservations of organic matter other than PAHs, amorphous carbons and associatedlaboratory dust analogues relevant to astrophysical applications.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 46: PAHs and the Universe: A Symposium to Celebrate the 25thAnniversary of the PAH Hypothesis , 2011 , pp. 381 - 391
Copyright
© EAS, EDP Sciences 2011

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