A search for structure in PAH emission in extended sources at 3.3 and 3.4 $\mu$m
Session 49 -- Interstellar Dust and Polarization
Display presentation, Tuesday, 10, 1995, 9:20am - 6:30pm

## [49.05] A search for structure in PAH emission in extended sources at 3.3 and 3.4 $\mu$m

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

We have observed three extended sources of the infrared emission features associated with polycyclic aromatic hydrocarbons (PAHs), using a 128$\times$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 $\mu$m PAH features in NGC 1333 \#3, Sharpless 106, and the Orion Bar. In all three sources, the 3.29 and 3.40 $\mu$m 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 $\mu$m feature to the main feature at 3.29 $\mu$m. The 3.40 $\mu$m feature may be a vibrational overtone of the 3.29 $\mu$m feature, or it may arise from attached molecular sidegroups.