The Detection of 6.9 μm Emission Features in the Infrared Spectra of IRAS 04296+3429, IRAS 05341+0852, and IRAS 22272+5435: Evidence for the Presence of H n -PAHs in Post-AGB Stars

Polycyclic aromatic hydrocarbons (PAHs) are generally believed to be ubiquitous in space and responsible for numerous telltale interstellar infrared emission bands. In Sandford et al., we suggested that PAHs with excess hydrogenation at their periphery ( -PAHs) may be an important subclass of these molecules in some astrophysical environments. These molecules are candidates to explain objects with anomalously large 3.4 μ m features, which are presumed to be associated with the aliphatic C–H stretching vibrations of the excess hydrogen. In that work, we suggest that for H n -PAHs to be a viable candidate as the source for this 3.4 μ m feature, we must also expect to observe methylene scissoring modes at 6.9 μ m. In this work, we continue to develop the hypothesis with a focus on the 6.9 μ m feature. We also present some new observations of three post-asymptotic giant branch (post-AGB) objects with abnormally large 3.4 μ m features, IRAS 04296+3429, IRAS 05341+0852, and IRAS 22272+5435, in addition to one post-AGB object with normal PAH emissions, IRAS 20000+3239. These observations were made using the FORCAST instrument in grism mode on the Stratospheric Observatory for Infrared Astronomy aircraft and demonstrate the presence of a 6.9 μ m feature for the three objects with abnormally large 3.4 μ m features and no detectable 6.9 μ m feature for the normal PAH emitter. These results are consistent with the hypothesis that H n -PAHs are a possible source of these infrared emission bands.