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$\begin{figure} \par\includegraphics[width=8.8cm]{6734F1.eps}\end{figure}$ Figure 1: The entire HH 212 outflow at 2.122 $\mu$ m, displaying the line emission from the H₂ 1-0 S(1) transition. The image was obtained at the Calar Alto 3.5-m telescope by Zinnecker et al. (1998). The outflow covers an extent of 240 $^{\prime \prime }$ (54 pc). The IRAS source lies between the two bright knots NK 1 and SK 1 with central position RA(2000) = 05 $^{\rm h}$ 43 $^{\rm m}$ 51.4 $^{\rm s}$ , Dec(2000) = -01 $\hbox {$^\circ $ }$ 02 $\hbox {$^\prime $ }$ 52 $\hbox {$^{\prime \prime }$ }$ . The locations of the effective apertures of the IFU observations are superimposed.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{67340201.eps}\vspace*{3mm} \par\includegraphics[width=15.5cm,clip]{67340202.eps}\end{figure}$ Figure 2: Spectra of the NK 1 knot ( upper) & the SK 1 knot ( lower panel) between 1.5 $\mu$ m and 2.5 $\mu$ m. The spectra were extracted over an area of 2 $.\!\!^{\prime\prime}$ 5 $\times$ 3 $.\!\!^{\prime\prime}$ 5 centered on the emission peak. The asterisk in the top panel indicates a spurious pixel value. Narrow absorption spikes are probably due to bad pixels or cosmic ray hits in the object, sky or standard-star data. Anomolous features may also result from poor telluric correction in parts of the K-band window.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=2.1cm,clip]{67340301.eps}\hspace... ...}\hspace{0.3cm} \includegraphics[width=1.85cm,clip]{67340318.eps} } \end{figure}$ Figure 3: Extracted line emission images for NK 1. The peak flux positions were estimated by Gaussian fitting of the image peaks and are indicated by the crosses. X-axis offsets increase toward the west; Y-axis offsets increase roughly northward along the jet axis (see Fig. 1). A continuum emission image, from data between 1.7 $\mu$ m and 1.71 $\mu$ m, is also provided. The large faint cross in each panel indicates the peak of the 1-0 S(1) line.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=2.1cm,clip]{67340401.eps}\hspace... ...cm} \includegraphics[width=1.85cm,clip]{67340423.eps}\hspace*{1cm}} \end{figure}$ Figure 4: Extracted line emission images for SK 1. See Fig. 3 for details.
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{67340501.eps}\vspace*{3mm} \par\includegraphics[width=15.6cm,clip]{67340502.eps}\end{figure}$ Figure 5: Spectra of the NB 1 bow ( top panel) and SB 1 and SB 2 ( lower panel) between 1.4 and 2.5 $\mu$ m. The NB 1 spectrum is extracted over an area of 1 $.\!\!^{\prime\prime}$ 8 $\times$ 1 $.\!\!^{\prime\prime}$ 8 centered on the NB 1 peak. The SB 1 and SB 2 spectrum is extracted over an area of 2 $.\!\!^{\prime\prime}$ 0 $\times$ 2 $.\!\!^{\prime\prime}$ 0 centered on the SB 1 peak.
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In the text

$\begin{figure} \par\mbox{\hspace*{1cm}\includegraphics[width=2.1cm]{67340601.eps... ...2.eps}\hspace{0.3cm} \includegraphics[width=1.85cm]{67340613.eps} } \end{figure}$ Figure 6: Extracted line emission images of NB 1 and NB 2. NB 2 is the northern, upper-most feature. Where possible, the positions of the peaks were determined via Gaussian fitting and are indicated by crosses (see Fig. 3 for further details). A continuum emission image, from data between 1.7 $\mu$ m and 1.71 $\mu$ m, is also provided. The large faint cross in each panel indicates the peak of the 1-0 S(1) line.
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In the text

$\begin{figure} \par\mbox{\hspace*{1cm}\includegraphics[width=2.1cm]{67340701.eps... ...2.eps}\hspace{0.3cm} \includegraphics[width=1.85cm]{67340713.eps} } \end{figure}$ Figure 7: Extracted line emission images of SB 1/SB 2 (see Fig. 3 for details). These two faint knots, labelled in Fig. 1, are essentially unresolved here. The large faint cross in each panel indicates the peak of the 1-0 S(1) line.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=6.6cm,clip]{67340801.eps}\includ... ...ip]{67340803.eps}\includegraphics[width=6.6cm,clip]{67340804.eps} } \end{figure}$ Figure 8: Column density ratio (CDR) diagrams for NK 1 ( left panels) and SK 1 ( right panels). The upper panels display data assuming no extinction whereas in the lower panels the extinction has been adjusted to minimise the difference between the 1-0 S-branch and Q-branch lines originating from the same upper energy level. H₂ v = 1-0 transitions are represented by squares, 2-1 transitions by crosses and 3-2 by triangles. The faint squares represent the 1-0 Q-branch measurements. The CDRs predicted by the best fit J-type bow shock model are also shown; the solid line represents the first vibrational level, dotted represents the second, and the dot-dashed line shows the third vibrational level.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=2.15cm,clip]{67340901.eps}\hspac... ...p]{67340905.eps}\includegraphics[width=2.35cm,clip]{67340906.eps} } \end{figure}$ Figure 9: Left: H₂ 1-0 S(1) image of NK 1 ( upper panels) and SK 1 ( lower panels) overlaid with [Fe II] contours. Middle and right: H₂ (2-1)/(1-0) S(1) ratio image of NK 1 ( upper) and SK 1 ( lower) overlaid with H₂ 1-0 S(1) and [Fe II] contours.
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In the text

$\begin{figure} \par\includegraphics[width=6.55cm,clip]{67341001.eps}\vspace*{0.3cm} \par\includegraphics[width=6.55cm,clip]{67341002.eps}\end{figure}$ Figure 10: The x ( upper panel) and y ( lower panel) peak flux positions relative to the 1-0 S(1) line are plotted against the upper energy level of each transition for NK 1. Crosses represent the v = 1-0 transitions, squares the v = 2-1, and the triangle represents the [Fe II] ⁴D_7/2 - ⁴F_9/2 transition at 1.644 $\mu$ m. The estimated systematic errors are indicated by error bars. Note that, in the top panel, the lower-excitation lines appear at negative (eastern) offsets, while the higher-excitation H₂ and [Fe II] lines appear at positive (western) offsets. No such trend is seen along the y-axis (the flow axis) in the lower panel.
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In the text

$\begin{figure} \par\hspace*{0.15cm}\includegraphics[width=6.65cm,clip]{67341101.... ...\vspace*{0.3cm} \par\includegraphics[width=6.8cm,clip]{67341102.eps}\end{figure}$ Figure 11: The x ( upper panel) and y( lower panel) peak flux positions relative to the 1-0 S(1) line are plotted against the upper energy of each transition for SK 1. The symbols are as in Fig. 10 and the diamond represents the 3-2 S(3) peak position. In SK 1, the excitation increases from east to west ( upper panel - like NK 1) but also from north to south ( lower panel) along the jet axis. Peak postions were derived from the convolved data.
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In the text

$\begin{figure} \par\includegraphics[height=4.55cm,width=5.5cm,clip]{67341201.eps... ... \par\includegraphics[height=4.55cm,width=5.35cm,clip]{67341202.eps}\end{figure}$ Figure 12: The x ( upper panel) and y ( lower panel) offsets relative to 1-0 S(1) position predicted by the model. Note that 6.7 $\times$ 10¹⁵ cm corresponds to 1 $\hbox {$^{\prime \prime }$ }$ at the adopted distance. The symbols are as defined in Fig. 10. To predict the offsets a Gaussian fit was performed to locate the peak position. In order not to include faint emission, the Gaussian fit was limited to values above 40% of the maximum value (as was the case in determining the peaks for the observed images). These plots are here compared in the inset panels to the observational data in Fig. 11 for SK1.
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In the text

$\begin{figure} \par\includegraphics[width=11.7cm,clip]{67341301.eps}\vspace*{3mm} \par\includegraphics[width=11.7cm,clip]{67341302.eps}\end{figure}$ Figure 13: A J-type bow shock model for SK 1. The x and y axis units represent 3.9 $\times$ 10¹⁴ cm, equivalent to 0.057 $\hbox {$^{\prime \prime }$ }$ at the adopted distance of 460 pc. In the lower panel the images have been smoothed with a Gaussian of FWHM = 9 pixels, which is equivalent to 3.5 $\times$ 10¹⁵ cm and $\sim$ 0.5 $\hbox {$^{\prime \prime }$ }$ (the average seeing throughout the observations). The crosses mark the positions of the peak emission. The equivalent observed images for SK1 are also displayed.
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In the text

$\begin{figure} \par\includegraphics[width=4.4cm,clip]{67341401.eps}\end{figure}$ Figure 14: The model (2-1 S(1)/1-0) S(1) ratio image is shown with overplotted contours corresponding to the model [Fe II] emission for comparison with the equivalent SK1 data extracted from Fig. 9.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{67341501.eps}\par\includegraphics[width=8cm,clip]{67341502.eps}\end{figure}$ Figure 15: An explanation for the inter-knot emission is provided by the the combined effect of a forward shock and a curved reverse shock. Whereas the ambient material is entrained and propelled outward by the forward shock, the jet shock entrains the jet material into a more collimated and focused flow which, under certain conditions such as high density, can breach ahead of the forward bow. As shown in the lower sketch, the knots can be asymmetric with oblique shocks exciting gas in the inter-knot region.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=2.1cm,clip]{67340401.eps}\hspace... ...cm} \includegraphics[width=1.85cm,clip]{67340423.eps}\hspace*{1cm}} \end{figure}$	Figure 4: Extracted line emission images for SK 1. See Fig. 3 for details.
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$\begin{figure} \par\includegraphics[width=15.6cm,clip]{67340501.eps}\vspace*{3mm} \par\includegraphics[width=15.6cm,clip]{67340502.eps}\end{figure}$	Figure 5: Spectra of the NB 1 bow ( top panel) and SB 1 and SB 2 ( lower panel) between 1.4 and 2.5 $\mu$ m. The NB 1 spectrum is extracted over an area of 1 $.\!\!^{\prime\prime}$ 8 $\times$ 1 $.\!\!^{\prime\prime}$ 8 centered on the NB 1 peak. The SB 1 and SB 2 spectrum is extracted over an area of 2 $.\!\!^{\prime\prime}$ 0 $\times$ 2 $.\!\!^{\prime\prime}$ 0 centered on the SB 1 peak.
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$\begin{figure} \par\mbox{\hspace*{1cm}\includegraphics[width=2.1cm]{67340701.eps... ...2.eps}\hspace{0.3cm} \includegraphics[width=1.85cm]{67340713.eps} } \end{figure}$	Figure 7: Extracted line emission images of SB 1/SB 2 (see Fig. 3 for details). These two faint knots, labelled in Fig. 1, are essentially unresolved here. The large faint cross in each panel indicates the peak of the 1-0 S(1) line.
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$\begin{figure} \par\mbox{\includegraphics[width=2.15cm,clip]{67340901.eps}\hspac... ...p]{67340905.eps}\includegraphics[width=2.35cm,clip]{67340906.eps} } \end{figure}$	Figure 9: Left: H₂ 1-0 S(1) image of NK 1 ( upper panels) and SK 1 ( lower panels) overlaid with [Fe II] contours. Middle and right: H₂ (2-1)/(1-0) S(1) ratio image of NK 1 ( upper) and SK 1 ( lower) overlaid with H₂ 1-0 S(1) and [Fe II] contours.
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$\begin{figure} \par\includegraphics[width=4.4cm,clip]{67341401.eps}\end{figure}$	Figure 14: The model (2-1 S(1)/1-0) S(1) ratio image is shown with overplotted contours corresponding to the model [Fe II] emission for comparison with the equivalent SK1 data extracted from Fig. 9.
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