All Figures

$\begin{figure} \par\includegraphics[width=18.4cm,clip]{1020fig1.eps} \end{figure}$ Figure 1: Changes in ¹²C, ¹³C, ¹⁴N, and ¹⁶O surface abundances with respect to the hydrogen surface abundance along the evolutionary tracks of non-rotating stars, as indicated by the grid points. The ratios were calculated from the data of Schaller et al. (1992) for solar metallicity. The approximate end of the core H burning and the onset of the core He burning phases are indicated by the two vertical dotted lines in each panel.
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In the text

$\begin{figure} \par\includegraphics[width=18.4cm,clip]{1020fig2.eps} \end{figure}$ Figure 2: Change of the ¹²C/¹³C surface abundance ratio during stellar evolution of non-rotating massive stars at solar metallicity. The ratios are calculated from the tables of Schaller et al. (1992). The dotted lines have the same meaning as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1020fig3.eps} \end{figure}$ Figure 3: Influence of the temperature on the synthetic ¹²CO band emission spectra. Clear band head structures form for $T_{\rm CO} \ge 2000$ K.
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In the text

$\begin{figure} \par\includegraphics[width=18.4cm,clip]{1020fig4.eps} \end{figure}$ Figure 4: Synthetic, optically thin ¹²CO plus ¹³CO first-overtone band spectra computed for $T_{\rm CO} = 3500$ K. The individual panels are for increasing spectral resolutions ( from top to bottom) and for decreasing ¹²C/¹³C ratios ( from left to right).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1020fig5.eps} \end{figure}$ Figure 5: CO Band structure for increasing CO column density ( from bottom to top), i.e., increasing optical thickness.
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In the text

$\begin{figure} \par\includegraphics[width=18.3cm,clip]{1020fig6.eps} \end{figure}$ Figure 6: Comparison of the positions of the galactic B[e] supergiant candidates from Table A.1 with evolutionary tracks of non-rotating ( left panel, from Schaller et al. 1992) and rotating ( right panel, from Meynet & Maeder 2003) stellar evolutionary models at solar metallicity. The dashed and dotted parts of the tracks indicate those evolutionary phases with $20 \ge ^{12}$ C/ $^{13}{\rm C} \ge 15$ and ¹²C/ $^{13}{\rm C} \le 15$ , respectively. The position of GG Car is emphasized.
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In the text

$\begin{figure} \par\includegraphics[width=18.4cm,clip]{1020fig2.eps} \end{figure}$	Figure 2: Change of the ¹²C/¹³C surface abundance ratio during stellar evolution of non-rotating massive stars at solar metallicity. The ratios are calculated from the tables of Schaller et al. (1992). The dotted lines have the same meaning as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1020fig3.eps} \end{figure}$	Figure 3: Influence of the temperature on the synthetic ¹²CO band emission spectra. Clear band head structures form for $T_{\rm CO} \ge 2000$ K.
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$\begin{figure} \par\includegraphics[width=18.4cm,clip]{1020fig4.eps} \end{figure}$	Figure 4: Synthetic, optically thin ¹²CO plus ¹³CO first-overtone band spectra computed for $T_{\rm CO} = 3500$ K. The individual panels are for increasing spectral resolutions ( from top to bottom) and for decreasing ¹²C/¹³C ratios ( from left to right).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1020fig5.eps} \end{figure}$	Figure 5: CO Band structure for increasing CO column density ( from bottom to top), i.e., increasing optical thickness.
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