A Study of the 3.3 and 3.4 μm Emission Features in Proto–Planetary Nebulae

Abstract

Medium-resolution spectra have been obtained of seven carbon-rich protoYplanetary nebulae (PPNs) and one young planetary nebula from 3.2 to 3.8 m, an interval containing the prominent hydrocarbon CÀH stretches at 3.3 and 3.4 m due to aromatic and aliphatic structures, respectively. The 3.3 m feature is newly identified in IRAS 23304+6147, 22223+4327, and 06530À0213 and is confirmed in Z02229+6208. Three of the PPNs emit in the 3.4 m feature, two of these being new identifications, IRAS 20000+3239 and 01005+7910, with two others showing possible detections. The 3.3 and 3.4 m emission features in IRAS 22272+5435 are seen in the nebula offset from the star but not at the position of the central star, consistent with the 2003 results of Goto et al. A similar distribution is seen for the 3.3 m feature in IRAS 22223+4327. All of the PPNs except IRAS 22272+5435 show Class A 3 m emission features. These observations, when combined with those of the approximately equal number of other carbon-rich PPNs pre-viously observed, demonstrate that there are large differences in the 3 m emission bands, even for PPNs with central stars of similar spectral type, and thus that the behavior of the bands does not depend solely on spectral type. We also investigated other possible correlations to help explain these differences. These differences do not depend on the C/O value, since the Class B sources fall within the C/O range found for Class A. All of these 3.3 m sources also show C 2 absorption and 21 m emission features, except IRAS 01005+7910, which is the hottest source at B0. Subject headingg s: circumstellar matter — infrared: ISM — infrared: stars — ISM: lines and bands — planetary nebulae: general — stars: AGB and post-AGB