AAS Meeting #193 - Austin, Texas, January 1999
Session 15. Planetary Nebulae
Display, Wednesday, January 6, 1999, 9:20am-6:30pm, Exhibit Hall 1

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[15.02] Near-Infrared Spectroscopic Imaging of Planetary Nebulae

C. A. Welch, J. L. Pipher, W. J. Forrest (Univ. of Rochester), C. E. Woodward (Wyoming Infrared Observatory)

We present near-infrared spectroscopic imaging of the planetary nebulae (PNs) Hubble 12 and M1-92. Hubble 12 has been observed in the molecular hydrogen v=1--0 S(1) emission line (2.12 \mum), in the forbidden singly ionized iron line ([FeII] at 1.644 \mum), and in the unidentified infrared (UIR) emission feature at 3.29 \mum. M1-92 has been imaged in the molecular hydrogen v=1--0 S(1) emission line (2.12 \mum), in the atomic hydrogen Brackett \gamma emission line (2.166 \mum), and in the water ice absorption feature (3.08 \mum). The observations were made at the Wyoming Infrared Observatory 2.3 m telescope and at the Mount Lemmon Observing Facility 1.5 m telescope with the University of Rochester 3rd Generation Infrared Camera.

Our M1-92 water ice absorption images, when compared with our Brackett \gamma and molecular hydrogen emission images, show the spatial relationship of the exciting source to the nebulosity. Although our nebular data do not have the high spatial resolution offered by Bujarrabal et~al. (1998), our images reveal the location of the obscured exciting star.

The [FeII] emission of Hubble 12 is in the form of limb-brightened bipolar lobes, and is similar to, but less extended than, the molecular hydrogen emission reported by Hora & Latter (1996). Although Hora & Latter (1996) determined (from spectral line ratios) that the molecular hydrogen emission in the central region is UV-excited fluorescence, their spectra do not address the excitation mechanism of the bipolar lobes. Such bright [FeII] emission as seen in our images is very suggestive of shocked gas.

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The author(s) of this abstract have provided an email address for comments about the abstract: carl@pas.rochester.edu

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