Astronomy & Astrophysics

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$\begin{figure} {\includegraphics[angle=-90,width=15.5cm,clip]{aa6800fig1_colour.ps} }\end{figure}$ Figure 1: a) Contour map of integrated emission in SiO(2-1) superimposed on the new H₂ image. The SiO emission regions are labelled in white. The filled triangle at (0 $\hbox {$^{\prime \prime }$ }$ , 0 $\hbox {$^{\prime \prime }$ }$ ) denotes the driving source MM1 (see Sect. 3.1). Contour levels range from 3 $\sigma$ (0.22 Jy beam^-1 km s^-1) to 39 $\sigma$ by steps of 6 $\sigma$ . The filled ellipse in the lower left corner shows the synthetised PdBI beam (HPBW): $1\hbox{$.\!\!^{\prime\prime}$ }89\times0\hbox{$.\!\!^{\prime\prime}$ }94$ . b) Same as panel a) for the SiO(5-4) emission. The dotted circle indicates the primary beam of the PdBI antennae. H₂ knots are labelled in black. Contour levels range from 3 $\sigma$ (0.42 Jy beam^-1 km s^-1) to 39 $\sigma$ by steps of 3 $\sigma$ . The beam is $0\hbox{$.\!\!^{\prime\prime}$ }78\times0\hbox{$.\!\!^{\prime\prime}$ }34$ . c) Inner 5 $\hbox {$^{\prime \prime }$ }$ of the SiO(5-4) map, superimposed onto the continuum image at 1.4 mm (gray scale and white contours). Continuum contour levels range from 3 $\sigma$ (1.9 mJy beam^-1) to 36 $\sigma$ by steps of 6 $\sigma$ . Labels indicate the HH212 driving source (MM1) and a tentative weaker source (MM2). (This figure is available in color in electronic form.)
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In the text

$\begin{figure} {\includegraphics[angle=-90,width=12.6cm,clip]{6800fig2.ps} }\end{figure}$ Figure 2: Left: position-velocity cut of SiO J=2-1 along the jet axis ( $\rm PA = 22\hbox {$^\circ $ }$ ). Contour levels range from 1.4 K to 27.5 K by 2.9 K (8 $\sigma$ ). Dashed lines mark the position of MM1 and the cloud $V_{\rm LSR}$ (+1.6 km s^-1; Wiseman et al. 2001). Filled triangles with error bars show the velocity centroid and intrinsic FWHM of H₂ knots (Takami et al. 2006). Right: zoomed-in PV cut of the inner jet in SiO J=5-4. Contour levels range from 3 K to 21 K by 3 K (4 $\sigma$ ). Black arrows show the velocity range of H₂O masers $\pm$ $0.1\hbox {$^{\prime \prime }$ }$ from the protostar (Claussen et al. 1998).
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In the text

$\begin{figure} \includegraphics[angle=-90,width=8.5cm]{6800fig3.ps} \end{figure}$ Figure 3: a) PV cuts in SiO(5-4) perpendicular to the jet axis, averaged over each of the four SiO bullets. Contour levels start at 3 $\sigma$ with steps of 6 $\sigma$ . They range from 1 K to 9.3 K (Blue 1), 2.7 to 14.5 K (Blue 2/Red 2), and 1.7 to 11.6 K (Red 1). Dashed lines mark the jet axis at $\rm PA = 22\hbox {$^\circ $ }$ and the $V_{\rm LSR}$ of the cloud (+1.6 km s^-1; Wiseman et al. 2001). A solid line shows the velocity gradient across Red 1. b) Zoom-in of the H₂ image highlighting the jet wiggling. Vertical black arrows indicate the declination range of the Blue 2/Red 2 inner jet.
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In the text