A search for structure in PAH emission in extended sources at 3.3 and 3.4 microns

Jesse Bregman (NASA Ames), P. Temi, D.M. Rank (UCSC/UCO) G.C. Sloan, A.S.B. Schultz (NASA Ames)

1994, BAAS, 26, 1392

We have observed three extended sources of the infrared emission features associated with polycyclic aromatic hydrocarbons (PAHs), using a 128×128 InSb array mounted on the 1.5 m NASA/Steward telescope on Mt. Lemmon. We used a CVF (1.5% bandpass) to isolate the emission from the 3.29 and 3.40 µm PAH features in NGC 1333 #3, Sharpless 106, and the Orion Bar. In all three sources, the 3.29 and 3.40 µm emission features arise from the same regions, but show decidedly different structure. We are analyzing the images to determine the relationship of the 3.40 µm feature to the main feature at 3.29 µm. The 3.40 µm feature may be a vibrational overtone of the 3.29 µm feature, or it may arise from attached molecular sidegroups.

We presented these results at the January, 1995 meeting of the AAS. More thorough analysis of Orion Bar appeared at the January, 1996 meeting of the AAS (Bregman et al. 1995), followed by results presented in two conference proceedings (Sloan et al. 1996; Bregman and Sloan 1996).

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