$\begin{figure} \par\includegraphics[width=13.5cm]{3482fig1.eps}\end{figure}$ Figure 1: Line profiles observed toward LkCa15. The dashed line indicates the velocity of the source. Note the different antenna temperature scales for the different features.
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In the text

$\begin{figure} \par\includegraphics[width=13.7cm]{3482fig2.eps}\end{figure}$ Figure 2: Line profiles observed toward TW Hya. Note the different antenna temperature scales for the different features.
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In the text

$\begin{figure} \par\includegraphics[width=13.3cm]{3482fig3.eps}\end{figure}$ Figure 3: Line profiles observed toward MWC 480. Note the different antenna temperature scales for the different features.
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In the text

$\begin{figure} \par\includegraphics[width=13.3cm]{3482fig4.eps}\end{figure}$ Figure 4: Line profiles observed toward HD 163296. Note the different antenna temperature scales for the different features.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=12cm]{3482fig6.ps} \end{figure}$ Figure 6: Observed (full lines) and simulated (dahes lines) ¹²CO $J\!=\!3\!\rightarrow\!2$ spectra. The observations are normalized to the peak values. The simulations are for a single temperature profile disk model (see Table 7 for parameters).
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In the text

$\begin{figure} \par\includegraphics[width=13.5cm]{3482fig1.eps}\end{figure}$	Figure 1: Line profiles observed toward LkCa15. The dashed line indicates the velocity of the source. Note the different antenna temperature scales for the different features.
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$\begin{figure} \par\includegraphics[width=13.7cm]{3482fig2.eps}\end{figure}$	Figure 2: Line profiles observed toward TW Hya. Note the different antenna temperature scales for the different features.
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$\begin{figure} \par\includegraphics[width=13.3cm]{3482fig3.eps}\end{figure}$	Figure 3: Line profiles observed toward MWC 480. Note the different antenna temperature scales for the different features.
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$\begin{figure} \par\includegraphics[width=13.3cm]{3482fig4.eps}\end{figure}$	Figure 4: Line profiles observed toward HD 163296. Note the different antenna temperature scales for the different features.
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$\begin{figure} \par\includegraphics[width=14cm]{3482fig5.eps} \end{figure}$	Figure 5: ¹²CO $J\!=\!3\!\rightarrow\!2$ maps toward TW Hya, LkCa 15, HD 163296 and MWC 480.
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$\begin{figure} \par\includegraphics[angle=90,width=12cm]{3482fig6.ps} \end{figure}$	Figure 6: Observed (full lines) and simulated (dahes lines) ¹²CO $J\!=\!3\!\rightarrow\!2$ spectra. The observations are normalized to the peak values. The simulations are for a single temperature profile disk model (see Table 7 for parameters).
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