All Figures

$\begin{figure} \par {\includegraphics[width=8.3cm,clip]{3439fig1.ps} } \end{figure}$ Figure 1: Velocity integrated emission in the S(1) v= 1-0 H₂ emission line covering the full observed field in OMC1. (0,0) marks the position of TCC0016 05 $^{{\rm h}}$ 35 $^{{\rm m}}$ 14 $.\!\!^{\rm s}$ 91, -05$^$22'39 $.\!\!^{\prime\prime}$ 31 (J2000). The star marks the position of BN. Units are arcseconds, where 1 arcsec = 460 AU.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm]{3439fig2.ps} } \end{figure}$ Figure 2: Larson size-linewidth relations, Eq. (2). Top: velocity dispersion as a function of size for the full velocity field. A power law fit of index 0.205 is overlaid. Centre: velocity dispersion for the filtered velocity image. Power laws of index 0.210 and -0.004 are overlaid. Bottom: velocity dispersion for the outflow region ( upper line) and Peak 1 ( lower line) with power law fits overlaid.
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In the text

$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{3439fig3.ps} } \end{figure}$ Figure 3: Probability distribution functions of velocities. Top: (+) PDF for the full velocity field. ( $\Diamond$ ) PDF with removal of velocities associated with the clump in Fig. 4. Bottom: PDF for the filtered data (see text). Stretched exponentials with $\beta =1.10$ and $\beta =0.86$ respectively are shown for comparison. The dashed lines are Gaussian fits to the core.
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In the text

$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{3439fig4.ps} } \end{figure}$ Figure 4: The brightly emitting clump that causes the hump in the red wing of the PDF (Fig. 3, + symbols). The xy plane is the plane of the sky, the vertical axis shows the radial velocity $v_{\rm lsr}$ . The plane at (x, y, 43) shows the boundary of the region of pixels ignored in the PDF shown as ( $\Diamond$ ) in Fig. 3. The centre of this clump is 6 $.\!\!^{\prime\prime}$ 5 E, 1 $.\!\!^{\prime\prime}$ 5 N of TCC0016. The colour scale refers to brightness in counts pixel^-1 s^-1, see Sect. 2
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In the text

$\begin{figure} \par {\includegraphics[width=8cm]{3439fig5.ps} } \end{figure}$ Figure 5: The variance function for the full velocity field. A power law form with exponent 0.53 is overlaid. The inset displays the variance function of the filtered velocity image compared to the variance function of the full field.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm]{3439fig6.ps} } \end{figure}$ Figure 6: The kurtosis function, Eq. (9), for the full velocity field (solid line). Theoretical predictions for 3 different Reynolds numbers from Eggers & Wang (1998) are shown for comparison.
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In the text

$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{3439fig7.ps} } \end{figure}$ Figure 7: PDFs of eight representative clumps. a), b), c) and d) are multi-modal, e) and f) are stretched exponential, g) and h) are Gaussian. Positions are shown in Figs. 8, 10, 11.
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In the text

$\begin{figure} \par\includegraphics[width=12cm]{3439fig8.eps}\end{figure}$ Figure 8: Position of clumps with bi- or multimodal PDF (blue), stretched exponential PDF (green) and Gaussian PDF (red). The underlying grey background represents the spatial extent of velocity integrated H₂ emission at 2.121 $\mu$ m with brightness greater than ${\sim }2.4 \times 10^{-6}$ W m^-2 sr^-1. The position of BN is marked with a star, IRc2 with a circle. a, b, c, d, e, f, g, h mark clumps shown in Figs. 7, 9.
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In the text

$\begin{figure} \par {\includegraphics[width=8.5cm]{3439fig9.ps} } \end{figure}$ Figure 9: The variance function for the eight individual clumps shown in Fig. 7. Power law fits are overlaid and the value of the exponent is given.
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In the text

$\begin{figure} \par\includegraphics[width=12cm]{3439fi10.eps}\end{figure}$ Figure 10: Clumps with the variance function scaling exponent $\gamma > 1.0$ . As in Fig. 8, the underlying grey background represents the spatial extent of velocity integrated H₂ emission at 2.121 $\mu$ m with brightness greater than ${\sim }2.4 \times 10^{-6}$ W m^-2 sr^-1. The position of BN is marked with a star, IRc2 with a circle. Colours represent brightness in counts per pixel per second in the clumps analyzed in Sect. 5. A and B mark sites of protostellar candidates. a, b, d, f mark clumps shown in Figs. 7, 9.
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In the text

$\begin{figure} \par\includegraphics[width=12cm]{3439fi11.eps}\end{figure}$ Figure 11: Clumps with the variance function scaling exponent $\gamma < 0.67$ . Grey background as in Fig. 10. The position of BN is marked with a star, IRc2 with a circle. Colours represent brightness in counts per pixel per second in the clumps analyzed in Sect. 5. e, h mark clumps shown in Figs. 7, 9.
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In the text

$\begin{figure} \par {\includegraphics[width=8.3cm,clip]{3439fig1.ps} } \end{figure}$	Figure 1: Velocity integrated emission in the S(1) v= 1-0 H₂ emission line covering the full observed field in OMC1. (0,0) marks the position of TCC0016 05 $^{{\rm h}}$ 35 $^{{\rm m}}$ 14 $.\!\!^{\rm s}$ 91, -05$^$22'39 $.\!\!^{\prime\prime}$ 31 (J2000). The star marks the position of BN. Units are arcseconds, where 1 arcsec = 460 AU.
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$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{3439fig3.ps} } \end{figure}$	Figure 3: Probability distribution functions of velocities. Top: (+) PDF for the full velocity field. ( $\Diamond$ ) PDF with removal of velocities associated with the clump in Fig. 4. Bottom: PDF for the filtered data (see text). Stretched exponentials with $\beta =1.10$ and $\beta =0.86$ respectively are shown for comparison. The dashed lines are Gaussian fits to the core.
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$\begin{figure} \par {\includegraphics[width=8cm]{3439fig5.ps} } \end{figure}$	Figure 5: The variance function for the full velocity field. A power law form with exponent 0.53 is overlaid. The inset displays the variance function of the filtered velocity image compared to the variance function of the full field.
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$\begin{figure} \par {\includegraphics[width=8cm]{3439fig6.ps} } \end{figure}$	Figure 6: The kurtosis function, Eq. (9), for the full velocity field (solid line). Theoretical predictions for 3 different Reynolds numbers from Eggers & Wang (1998) are shown for comparison.
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$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{3439fig7.ps} } \end{figure}$	Figure 7: PDFs of eight representative clumps. a), b), c) and d) are multi-modal, e) and f) are stretched exponential, g) and h) are Gaussian. Positions are shown in Figs. 8, 10, 11.
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$\begin{figure} \par {\includegraphics[width=8.5cm]{3439fig9.ps} } \end{figure}$	Figure 9: The variance function for the eight individual clumps shown in Fig. 7. Power law fits are overlaid and the value of the exponent is given.
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$\begin{figure} \par\includegraphics[width=12cm]{3439fi11.eps}\end{figure}$	Figure 11: Clumps with the variance function scaling exponent $\gamma < 0.67$ . Grey background as in Fig. 10. The position of BN is marked with a star, IRc2 with a circle. Colours represent brightness in counts per pixel per second in the clumps analyzed in Sect. 5. e, h mark clumps shown in Figs. 7, 9.
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