All Figures

	Figure 1: a) The H2 v=1-0 S(1) image of AFGL 5157 over a field of . North is at the top and east is to the left. The shell structure around the infrared cluster is marked. b) The image of AFGL 5157 over a field of 6 , similar to the left panel. The infrared cluster is marked. The faint surrounding is the infrared nebula, coinciding well with the shell structure.
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In the text

	Figure 2: The continuum-subtracted H2 image of AFGL 5157. The H2 knots and ridges of shell structure are marked, respectively. The superposed are the contours of the NH3 core (Torrelles et al. 1992a; Pastor et al. 1991; Verdes-Montenegro et al. 1989), together with several plus symbols standing for the H2O masers (Torrelles et al. 1992b; Verdes-Montenegro et al. 1989; Henning et al. 1992).
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In the text

Figure 3: The sketch of observations previously obtained in the literature and the new H2 jet in AFGL 5157. The NH3 core (Torrelles et al. 1992a; Pastor et al. 1991; Verdes-Montenegro et al. 1989) in thick contours is similar to that in Fig. 2, superposed with the H II region in tilted thin contours, H2O masers in plus symbols (Torrelles et al. 1992b; Verdes-Montenegro et al. 1989; Henning et al. 1992), and CO bipolar outflow (Snell et al. 1988; Torrelles et al. 1992b). The red lobe of CO outflow is along the jet. The positions of NGC 1985 (Torrelles et al. 1992a) and IRAS 05345+3157 are also marked, coexisting with the diffuse H2 shell (see Fig. 2 and Chen et al. 1999).

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In the text