Does the 3.3 micron feature require UV excitation?

Details Does the 3.3 micron feature require UV excitation? Does the 3.3 micron feature require UV excitation?

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...201.7509s&link_type=abstract

American Astronomical Society, 201st AAS Meeting, #75.09; Bulletin of the American Astronomical Society, Vol. 34, p.1225

Astronomy and Astrophysics

Astrophysics

Scientific paper

The so-called unidentified infrared (UIR) emission features at 3.3, 6.2, 7.7, 8.6 and 11.3 μ m have been studied in many astrophysical objects and their origin has been attributed to polycyclic aromatic hydrocarbons (PAHs). Past observations show that UIRs can be detected in UV-rich environments, however, the coolest object observed to have well-defined UIR features is vdB 133, illuminated by the binary system HD 195593 (A+B), which includes an F5Iab (Teff ≈ 6800 K) and a B7II (Teff ≈ 12000 K)-type star. Recently, a new astronomical PAH model (Li & Draine 2002) successfully reproduced the UIBs found in the "UV-weak environment" of vdB 133. We wanted to address the question of whether the 3.3 μ m feature requires UV photons for excitation, and if so, to determine the lower-limit. Toward that end, thirteen stars, ranging in temperature from 15000 K to 3500 K, were observed using SpeX at the NASA Infrared Telescope Facility (IRTF) in August and September, 2002. Li, A., & Draine, B.T. 2002, ApJ, 572, 232.

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