Simulation Of Organic Interstellar Dust In The Laboratory

Details Simulation Of Organic Interstellar Dust In The Laboratory Simulation Of Organic Interstellar Dust In The Laboratory

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.2404d&link_type=abstract

American Astronomical Society Meeting 208, #24.04; Bulletin of the American Astronomical Society, Vol. 38, p.104

Astronomy and Astrophysics

Astronomy

Scientific paper

Spectra of carbonaceous solids having a composition similar to that of interstellar dust are discussed in the context of observational data. Specific examples include both hydrogenated and dehydrogenated materials. Infrared spectra of long-chain n-alkane molecules, CH3(CH2)mCH3, with m > 8 have been obtained in absorption and emission and are compared to spectra of a variety of interstellar sources. Absorption spectra of these molecules in the 3.4 μm region are remarkably similar, consisting of narrow features at 3.384, 3.425 and 3.508 μm, independent of chain length. These features are not seen in absorption in interstellar clouds. Thermal spectra of these molecules show a number of characteristic features near 6.8, 7.3 and 13.9 μm that should be useful in determining whether large n-alkane molecules are present in interstellar emission sources. UV spectra of dehydrogenated carbons exhibit a feature at 217.5 nm that may be associated with the well-known interstellar band at this wavelength. These experiments lead to the conclusion that dehydrogenated coronene molecules and their cations may be important interstellar molecules.

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