All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f1-1.eps} \end{figure}$ Figure 1: N₂H⁺(1-0) integrated intensity maps. Intensity contour ranges from 30% to 90% of peak intensity, thick contours correspond to half maximum levels. Observed positions are marked by dots and IRAS point sources are marked by stars. The uncertainty ellipses corresponding to 95% confidence level in IRAS point source position are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f2.eps} \end{figure}$ Figure 2: The N₂H⁺(1-0) spectrum toward the intensity peak of G 351.41+0.64. The positions of hyperfine components are indicated.The relative amplitudes of the components correspond to the LTEoptically thin case.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f3.eps} \end{figure}$ Figure 3: Ratio of (12-12) to (23-12) peak temperatures versus ratio of (01-12) to (23-12) peak temperatures (R₁₂ and R₀₂, respectively). The LTE curve is also shown.
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In the text

$\begin{figure} \includegraphics[width=8.8cm,clip]{3576f4.eps} \end{figure}$ Figure 4: Four examples of integrated intensity profiles together with the fitted power-law functions convolved with a Gaussian telescope beam. The data lower than the dashed lines (20% of peak integrated intensity) were neglected.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f5.eps} \end{figure}$ Figure 5: Radial velocity dispersion profiles for the cores with one clump and clumps separated at half maximum intensity level.
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In the text

$\begin{figure} \includegraphics[width=8.8cm,clip]{3576f6-1.eps} \end{figure}$ Figure 6: Local velocity gradient maps superposed on integrated intensity maps. Total velocity gradients are shown by bold arrows together with their values (in km s^-1 pc^-1). IRAS point sources are marked by stars. The uncertainty ellipses are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f6-2.eps}\end{figure}$ Figure 6: continued.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f6-3.eps}\end{figure}$ Figure 6: continued.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f6-4.eps}\end{figure}$ Figure 6: continued.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f6-5.eps}\end{figure}$ Figure 6: continued.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f7.eps} \end{figure}$ Figure 7: Mean line widths versus emission region sizes a) together with regression (solid) line. Dashed and dotted lines correspond to the line width - size relations from Caselli & Myers (1995) and Zinchenko(2000), respectively. Peak N₂H⁺ column densities versus emissionregion sizes b).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f1-1.eps} \end{figure}$	Figure 1: N₂H⁺(1-0) integrated intensity maps. Intensity contour ranges from 30% to 90% of peak intensity, thick contours correspond to half maximum levels. Observed positions are marked by dots and IRAS point sources are marked by stars. The uncertainty ellipses corresponding to 95% confidence level in IRAS point source position are also shown.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f1-2.eps}\end{figure}$	Figure 1: continued.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f2.eps} \end{figure}$	Figure 2: The N₂H⁺(1-0) spectrum toward the intensity peak of G 351.41+0.64. The positions of hyperfine components are indicated.The relative amplitudes of the components correspond to the LTEoptically thin case.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f3.eps} \end{figure}$	Figure 3: Ratio of (12-12) to (23-12) peak temperatures versus ratio of (01-12) to (23-12) peak temperatures (R₁₂ and R₀₂, respectively). The LTE curve is also shown.
Open with DEXTER

$\begin{figure} \includegraphics[width=8.8cm,clip]{3576f4.eps} \end{figure}$	Figure 4: Four examples of integrated intensity profiles together with the fitted power-law functions convolved with a Gaussian telescope beam. The data lower than the dashed lines (20% of peak integrated intensity) were neglected.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f5.eps} \end{figure}$	Figure 5: Radial velocity dispersion profiles for the cores with one clump and clumps separated at half maximum intensity level.
Open with DEXTER

$\begin{figure} \includegraphics[width=8.8cm,clip]{3576f6-1.eps} \end{figure}$	Figure 6: Local velocity gradient maps superposed on integrated intensity maps. Total velocity gradients are shown by bold arrows together with their values (in km s^-1 pc^-1). IRAS point sources are marked by stars. The uncertainty ellipses are also shown.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f6-2.eps}\end{figure}$	Figure 6: continued.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3576f7.eps} \end{figure}$	Figure 7: Mean line widths versus emission region sizes a) together with regression (solid) line. Dashed and dotted lines correspond to the line width - size relations from Caselli & Myers (1995) and Zinchenko(2000), respectively. Peak N₂H⁺ column densities versus emissionregion sizes b).
Open with DEXTER