H${}_2$ in low-ionization structures of planetary nebulae

Abstract

We report the detection of near-IR H${}_2$ emission from the low-ionization structures (knots) in two planetary nebulae. The deepest ever, high-angular resolution H${}_2$ 1-0 S(1) at 2.122$\mu$, H${}_2$ 2-1 S(1) at 2.248$\mu$ and Br$\gamma$ images of K 4-47 and NGC 7662, obtained using the Near InfraRed Imager and Spectrometer (NIRI) at Gemini-North, are analyzed here. K 4-47 reveals a remarkable highly collimated bipolar structure not only in the optical but also in the molecular hydrogen emission. The H${}_2$ emission emanates from the walls of the bipolar outflows and also from the pair of knots at the tip of the outflows. The H${}_2$ 1-0 S(1)/2-1 S(1) line ratio ranges from ~7 to ~10 suggesting the presence of shock interactions. Our findings can be explained by the interaction of a jet/bullet ejected from the central star with the surrounding asymptotic giant branch material. The strongest H${}_2$ line, v=1-0 S(1) is also detected in several low-ionization knots located at the periphery of the elliptical planetary nebula NGC 7662, but only four of these knots are detected in the H${}_2$ v=2-1 S(1) line. These four knots exhibit an H${}_2$ line ratio between 2 and 3.5, which suggests that the emission is caused by the UV ionizing flux of the central star. Our data confirms the presence of H${}_2$ gas in both fast- and slow-moving low-ionization knots, which has only been confirmed before in the nearby Helix nebula and Hu 1-2. Overall, the low-ionization structures of planetary nebulae are found to share similar traits to photodissociation regions.

arXiv comment9 pages and 5 figures. MNRAS in press

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