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星際與拱星介質

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CO(6-5) line at 690 GHz of the proto-planetary nebula CRL 618

圖片來源: Nakashima et al.

The CO(6-5) line at 690 GHz of the proto-planetary nebula CRL 618 is first detected and imaged by the SMA. CRL 618 exhibits two different kinematical components, which are interpreted as high and low velocity bipolar outflows. The blue and red contours re

The collimated high velocity jet in young planetary nebula CRL 618 as traced by the sub-millimeter rotational line CO(6-5) has recently been imaged using the SMA (Figure 3). For the first time we are able to trace clearly the warm and dense molecular gas in the fast outflow and the shocked gas produced by the interaction between the fast outflow and the remnant slowly expanding circumstellar envelope. The collimated high velocity jet clearly shows bipolar morphology while the compact emission around the systemic velocity traces the dense inner envelope. The new SMA imaging data have allowed us to infer an improved and more consistent structure of the CRL 618 nebula.