SPATIAL VARIATION OF THE 3.29 AND 3.40 MICRON EMISSION BANDS WITHIN REFLECTION NEBULAE AND THE PHOTOCHEMICAL EVOLUTION OF METHYLATED POLYCYCLIC AROMATIC-HYDROCARBONS

Spectra of 3 mu m emission features have been obtained at several posi tions within the reflection nebulae NGC 1333 SVS3 and NGC 2023. Strong variations of the relative intensities of the 3.29 mu m feature and i ts most prominent satellite band at 3.40 mu m are found. It is shown t hat (i) the 3.40 mu m band is too intense with respect to the 3.29 mu m band at certain positions to arise from hot band emission alone, (ii ) the 3.40 Irm band can be reasonably well matched by new laboratory s pectra of gas-phase polycyclic aromatic hydrocarbons (PAHs) with alkyl (-CH3) side groups, and (iii) the variations in the 3.40 mu m to 3.29 mu m band intensity ratios are consistent with the photochemical eros ion of alkylated PAHs. We conclude that the 3.40 mu m emission feature is attributable to -CH3 side groups on PAH molecules. We predict a va lue of 0.5 for the peak intensity ratio of the 3.40 and 3.29 mu m emis sion bands from free PAHs in the diffuse interstellar medium, which wo uld correspond to a proportion of one methyl group for four peripheral hydrogens. We also compare the 3 mu m spectrum of the proto-planetary nebula IRAS 05341+0852 with the spectrum of the planetary nebula IRAS 21282+5050. We suggest that a photochemical evolution of the initial aliphatic and aromatic hydrocarbon mixture formed in the outflow is re sponsible for the changes observed in the 3 mu m emission spectra of t hese objects.