All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=16.5cm,clip]{2093fig1.eps} \end{figure}$ Figure 1: (Left) Map of the high-velocity outflow emission in the ¹²CO(2-1) line (thick black contours) superposed on the map of the ¹³CO(2-1) emission (thick white contours) and a [S II] image of the region (greyscale; Reipurth et al. 1983). The image has been saturated to outline the ring and the weak emission downstream of HH2. The redshifted wing of the HH 2 outflow is drawn in dashed contours. Contours range from 4 to $20\hbox {\kern 0.20em K}\hbox {\kern 0.20em km\kern 0.20em s$^{-1}$ }$ by step of $2\hbox {\kern 0.20em K}\hbox {\kern 0.20em km\kern 0.20em s$^{-1}$ }$ . The blueshifted wing is drawn in solid contours. First contour and contour interval are 1 and $0.5\hbox {\kern 0.20em K}\hbox {\kern 0.20em km\kern 0.20em s$^{-1}$ }$ respectively. The white stars mark the position of the HH 2 knots A to L. The position of the regions discussed in the text (the "ring'' and the molecular emission peak downstream HH 2) are indicated. (Right) Map of the ¹³CO(2-1) emission integrated between 5.5 and $6.75\hbox {\kern 0.20em km\kern 0.20em s$^{-1}$ }$ (thick white contours) and between 9.5 and $12\hbox {\kern 0.20em km\kern 0.20em s$^{-1}$ }$ (dashed) superposed on a [S II] image of the region (greyscale). Intensity contours range from 6 to $11\hbox {\kern 0.20em K}\hbox {\kern 0.20em km\kern 0.20em s$^{-1}$ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2093fig2.eps} \end{figure}$ Figure 2: Montage of ¹²CO(2-1) and ¹³CO(2-1) spectra at 3 positions: the protostellar core ( top), the "ring'' ( middle), and the "molecular peak'' downstream of HH 2 ( bottom).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=11cm,clip]{2093fig3.eps} \end{figure}$ Figure 3: Velocity-integrated intensity channel map of the SO 3₄-2₃ emission in the HH 1-2 region (contours), superposed on the $5.0{-}8.5~\rm \mu m$ emission map obtained with ISO. First contour and contour interval is $0.2\hbox {\kern 0.20em K}$ . Velocity is indicated in the top left corner of each panel. The position of VLA 1 is marked by a white star. The individual HH knots are drawn in black. Coordinates are in arcsec offset with respect to VLA 1.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2093fig4.eps} \end{figure}$ Figure 4: Spectra of the SO 3₄-2₃ and 2₃-1₂ lines observed towards the molecular emission peak downstream HH 2 at offset position ( $60\hbox {$^{\prime \prime }$ }$ , $-75\hbox {$^{\prime \prime }$ }$ ) and the protostellar source VLA 1. Flux is in main-beam brightness temperature. Line intensities have been multiplied by 2.0 for the VLA 1 spectra.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.4cm,clip]{2093fig5.eps} \end{figure}$ Figure 5: Variations of the SO 3₄-2₃/2₃-1₂ (thick solid) and 6₇-5₆/5₆-4₅ (thick dashed) intensity line ratios with temperature and density at the molecular peak. The SO column density is taken to be $5.6\times 10^{13}\hbox {\kern 0.20em cm$^{-2}$ }$ (see text). Thin contours draw the values at 90 and 110.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{2093fig6.eps} \end{figure}$ Figure 6: Comparison of the emission distribution of the SO 3₄-2₃(black contours) at various velocity intervals (6.5, 9.5, 10, 10.5 km s^-1) with the CO 2-1 high-velocity outflow. First contour and contour interval are $0.2\hbox {\kern 0.20em K}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{2093fig7.eps} \end{figure}$ Figure 7: Map of the velocity-integrated ¹³CO(2-1) intensity in the HH 2 region. First contour and contour interval are 2 and $1\hbox {\kern 0.20em K}\hbox {\kern 0.20em km\kern 0.20em s$^{-1}$ }$ respectively. Velocity interval is indicated in the bottom right corner. The invidual HH knots are drawn in white.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{2093fig8.eps} \end{figure}$ Figure 8: a) Mid-infrared emission integrated between 5 and $8.5~\rm \mu m$ superposed on an optical [S 2] image of HH 2 (Reipurth 1993). Contours range from 3 to 5.6 mJy by step of 0.2 mJy/pixel (px), from 6 to 10 mJy by step of 1 mJy/px, from 15 to 20 mJy by step of 5 mJy/px. b) High-velocity CO $J=2\rightarrow 1$ emission (white contours) superposed on the $5.0{-}8.5~\rm \mu m$ integrated mid-infrared map (colourscale). Contours range from 4 to 20 K $\hbox {\kern 0.20em km\kern 0.20em s$^{-1}$ }$ by step of 2 K $\hbox {\kern 0.20em km\kern 0.20em s$^{-1}$ }$ . The position of the individual shocks A-L are marked with stars. Red polygons delineate the fields used to compute individual spectra. c) Spectra of the mid-infrared emission between 5.0 and $17~\rm\mu m$ . d) Emission detected towards the "ring'' West of HH 2H in: $\hbox {${}^{13}$ CO(2--1)}$ : contours range from 6 to $11\hbox {\kern 0.20em K}\hbox {\kern 0.20em km\kern 0.20em s$^{-1}$ }$ by step of $1\hbox {\kern 0.20em K}\hbox {\kern 0.20em km\kern 0.20em s$^{-1}$ }$ ; H₂ S(2) $12.2~\rm \mu m$ : contours range from 4 to 10 mJy by step of 2 mJy/px; $13.9{-}15.4 ~\rm \mu m$ continuum: first contour is 4 mJy, following contours range from 4.5 mJy to 7.5 mJy by step of 1 mJy/px; PAH $11.3~\rm \mu m$ band: contours range from 2 to 4.5 mJy by step of 0.5 mJy/px. The CVF maps were convolved with a Gaussian of 12 $^{\prime \prime }$ HPFW to outline the extended emission. The rms in the $11.3~\rm \mu m$ PAH map and the continuum map is $0.3~\rm mJy/$ px; it is $\approx$ $1~\rm mJy/$ px in the $\hbox {H${}_2$ }$ S(2) map.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2093fig2.eps} \end{figure}$	Figure 2: Montage of ¹²CO(2-1) and ¹³CO(2-1) spectra at 3 positions: the protostellar core ( top), the "ring'' ( middle), and the "molecular peak'' downstream of HH 2 ( bottom).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2093fig4.eps} \end{figure}$	Figure 4: Spectra of the SO 3₄-2₃ and 2₃-1₂ lines observed towards the molecular emission peak downstream HH 2 at offset position ( $60\hbox {$^{\prime \prime }$ }$ , $-75\hbox {$^{\prime \prime }$ }$ ) and the protostellar source VLA 1. Flux is in main-beam brightness temperature. Line intensities have been multiplied by 2.0 for the VLA 1 spectra.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.4cm,clip]{2093fig5.eps} \end{figure}$	Figure 5: Variations of the SO 3₄-2₃/2₃-1₂ (thick solid) and 6₇-5₆/5₆-4₅ (thick dashed) intensity line ratios with temperature and density at the molecular peak. The SO column density is taken to be $5.6\times 10^{13}\hbox {\kern 0.20em cm$^{-2}$ }$ (see text). Thin contours draw the values at 90 and 110.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{2093fig6.eps} \end{figure}$	Figure 6: Comparison of the emission distribution of the SO 3₄-2₃(black contours) at various velocity intervals (6.5, 9.5, 10, 10.5 km s^-1) with the CO 2-1 high-velocity outflow. First contour and contour interval are $0.2\hbox {\kern 0.20em K}$ .
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{2093fig7.eps} \end{figure}$	Figure 7: Map of the velocity-integrated ¹³CO(2-1) intensity in the HH 2 region. First contour and contour interval are 2 and $1\hbox {\kern 0.20em K}\hbox {\kern 0.20em km\kern 0.20em s$^{-1}$ }$ respectively. Velocity interval is indicated in the bottom right corner. The invidual HH knots are drawn in white.
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