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Spatial variations of the 3 micron emission features within UV-excited nebulae - Photochemical evolution of interstellar polycyclic aromatic hydrocarbons
Geballe, T. R.; Tielens, A. G. G. M.; Allamandola, L. J.; Moorhouse, A.; Brand, P. W. J. L.
AA(Joint Astronomy Center, Hilo, HI; ASTRON, Amsterdam, Netherlands), AB(NASA, Ames Research Center, Moffett Field, CA; California, University, Berkeley), AC(NASA, Ames Research Center, Moffett Field, CA), AD(Royal Observatory, Edinburgh, Scotland), AE(Royal Observatory, Edinburgh, Scotland)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 341, June 1, 1989, p. 278-287. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Aromatic Compounds, Hydrocarbons, Infrared Spectra, Interstellar Matter, Orion Nebula, Spectral Line Width, Energy Transfer, Molecular Structure, Photochemical Reactions
Bibliographic Code:


Spectra at 3 microns have been obtained at several positions in the Orion Bar region and in the nebula surrounding HD 44179. Weak emission features at 3.40, 3.46, 3.51, and 3.57 microns are prominent in the Orion Bar region. The 3.40- and 3.51-micron features increase in intensity relative to the dominant 3.29-micron feature. The spectrum obtained in the Red Rectangle region 5 arcsecs north of HD 44179 are similar to those in the Orion Bar, with a weak, broad 3.40-micron feature at the position of HD 44179. The spatial behavior of the weak emission features is explained in terms of hot bands of the CH stretch and overtones, and combination bands of other fundamental vibrations in simple PAHs. Based on the susceptibility of PAHs to destruction by the far UV fields in both regions, PAH sizes are estimated at 20-50 carbon atoms.

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