All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=15cm,clip]{3241_f1a.ps}\par\vspace*{2mm} \includegraphics[angle=-90,width=15cm,clip]{3241_f1b.ps} \end{figure}$ Figure 1: Spectra of 36 WR CSPNe stars (see Tables 1a and 3) ordered according to the evolutive sequence. The 5200-5670 Å range has been zoomed, in order to better distinguish the different emission lines. Nebular lines are shown at the top of the figures.
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In the text

$\begin{figure}\par\includegraphics[angle=-90,width=16cm,clip]{3241_f1c.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f2.eps} \end{figure}$ Figure 2: Comparison of the dereddened line strengths relative to C IV-5806 = 100 given in this work and in CMB98. The resulting correlation seems to be linear: this work $= 1.05\times {\rm CMB98}$ with R²=0.91 (solid line). An alternative fit gives: this work $= 0.98\times {\rm CMB98} + 0.16$ (dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f3.eps} \end{figure}$ Figure 3: Upper panels: variation along the [WO] and [WC] types of the O VI-5290/C IV-5806 (early-types) and C III-5696/C IV-5806 (late-types) dereddened line ratios. Lower panels: variation of the C IV-5470/C IV-5806 and He II(C II?)-5412/C IV-5806 dereddened line ratios. The numbers 1 to 42 on the abscissa correspond to the observed stars (see Table 3). All line intensities are relative to C IV-5806 = 100.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f4.eps} \end{figure}$ Figure 4: Correlation between the C IV-5470/C IV-5806 and He II-5410/C IV-5806 dereddened line ratios. All line intensities are relative to C IV-5806 = 100. See symbol legend in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{3241_f5a.eps}\par\vspace*{2mm} \includegraphics[width=6.8cm,clip]{3241_f5b.eps} \end{figure}$ Figure 5: For hot [WO] stars, top panels: relative variation versus O VI -5290 of the O VII+VI-5666, O VIII-6068, O VI-3822, O V-5590, He II-5412 and C IV-4650 dereddened line intensities. Bottom panels: relative variation versus O VI-3822/O V-5590 of the O VI-3822/C IV-5806 and O VI-3822/He II-5412 dereddened line intensities. All line intensities are relative to C IV-5806 = 100. See symbol legend in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3241_f6.eps} \end{figure}$ Figure 6: For [WC] stars, relative variation versus C III-5696 of the C III-4649, C II-4267,-6461,-7235, C IV(C II?)-5470, He II(C II?)-5412 and O III-5592 dereddened line intensities, and of the C III-5696/O III-5592 ratio. All line intensities are relative to C IV-5806 = 100. See symbol legend in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3241_f7.ps} \end{figure}$ Figure 7: C IV-5801/12 superimposed line profiles of the four [WO4]pec stars. The thick profile corresponds to M 1-51 (20.9-1.1), and the thin solid line to Cn 1-5 (2.2-9.4). M 1-32 (11.9+4.2) and PM 1-89 (324.0+3.5) are represented with a dashed and dashed-dotted line respectively. For comparison, the C IV line profile of the wels star M 1-61 (19.4-5.3) has been added (dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f8a.eps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{3241_f8b.eps} \end{figure}$ Figure 8: Upper panel: variation of the FWHM of C IV-5806 and C III-5696 along the spectral sequence, averaged from Table 1a. Middle and lower panels: variation of the mean terminal wind velocity and the stellar temperature ( $T_{\rm eb}$ ), respectively, through the spectral sequence from the [WO1-4] to [WC4-11] subtypes. The fits (solid line) include the [WO4]pec point.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f9.eps} \end{figure}$ Figure 9: 42 CSPNe plotted on the tracks from Pauldrach et al. (1988). See the symbol legend in Fig. 8. The data points from Pauldrach et al. (1988) are also shown with the symbols "+'' and " $\times$ ''.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f10.eps} \end{figure}$ Figure 10: Positions of the stars on the HR diagram, using symbol legend from Fig. 8. Four evolutionary tracks from Blöcker (1995), for the masses 0.546, 0.565, 0.696 and 0.940 $M_{\odot }$ , are shown in solid lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f11.eps} \end{figure}$ Figure 11: Histogram of the distribution of our sample (42 stars, solid line), similar to the distribution of the whole well-classified sample (50 stars, dotted line).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15cm,clip]{3241_f1a.ps}\par\vspace*{2mm} \includegraphics[angle=-90,width=15cm,clip]{3241_f1b.ps} \end{figure}$	Figure 1: Spectra of 36 WR CSPNe stars (see Tables 1a and 3) ordered according to the evolutive sequence. The 5200-5670 Å range has been zoomed, in order to better distinguish the different emission lines. Nebular lines are shown at the top of the figures.
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$\begin{figure}\par\includegraphics[angle=-90,width=16cm,clip]{3241_f1c.ps}\end{figure}$	Figure 1: continued.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f2.eps} \end{figure}$	Figure 2: Comparison of the dereddened line strengths relative to C IV-5806 = 100 given in this work and in CMB98. The resulting correlation seems to be linear: this work $= 1.05\times {\rm CMB98}$ with R²=0.91 (solid line). An alternative fit gives: this work $= 0.98\times {\rm CMB98} + 0.16$ (dotted line).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f4.eps} \end{figure}$	Figure 4: Correlation between the C IV-5470/C IV-5806 and He II-5410/C IV-5806 dereddened line ratios. All line intensities are relative to C IV-5806 = 100. See symbol legend in Fig. 3.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3241_f6.eps} \end{figure}$	Figure 6: For [WC] stars, relative variation versus C III-5696 of the C III-4649, C II-4267,-6461,-7235, C IV(C II?)-5470, He II(C II?)-5412 and O III-5592 dereddened line intensities, and of the C III-5696/O III-5592 ratio. All line intensities are relative to C IV-5806 = 100. See symbol legend in Fig. 3.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3241_f7.ps} \end{figure}$	Figure 7: C IV-5801/12 superimposed line profiles of the four [WO4]pec stars. The thick profile corresponds to M 1-51 (20.9-1.1), and the thin solid line to Cn 1-5 (2.2-9.4). M 1-32 (11.9+4.2) and PM 1-89 (324.0+3.5) are represented with a dashed and dashed-dotted line respectively. For comparison, the C IV line profile of the wels star M 1-61 (19.4-5.3) has been added (dotted line).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f8a.eps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{3241_f8b.eps} \end{figure}$	Figure 8: Upper panel: variation of the FWHM of C IV-5806 and C III-5696 along the spectral sequence, averaged from Table 1a. Middle and lower panels: variation of the mean terminal wind velocity and the stellar temperature ( $T_{\rm eb}$ ), respectively, through the spectral sequence from the [WO1-4] to [WC4-11] subtypes. The fits (solid line) include the [WO4]pec point.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f9.eps} \end{figure}$	Figure 9: 42 CSPNe plotted on the tracks from Pauldrach et al. (1988). See the symbol legend in Fig. 8. The data points from Pauldrach et al. (1988) are also shown with the symbols "+'' and " $\times$ ''.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f10.eps} \end{figure}$	Figure 10: Positions of the stars on the HR diagram, using symbol legend from Fig. 8. Four evolutionary tracks from Blöcker (1995), for the masses 0.546, 0.565, 0.696 and 0.940 $M_{\odot }$ , are shown in solid lines.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3241_f11.eps} \end{figure}$	Figure 11: Histogram of the distribution of our sample (42 stars, solid line), similar to the distribution of the whole well-classified sample (50 stars, dotted line).
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