All Figures

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{8388fig1.eps} \end{figure}$ Figure 1: Observed and synthetic spectra for Me 1-1 a) and S 190 b) displaying broad lines and indicating rotationally broadened profiles. The observed spectra are plotted along with three synthetic spectra computed for three different surface gravities showing the sensitivity of the Fe II (and Ba II to $\log g$ ).
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{8388fig2.eps} \end{figure}$ Figure 2: Observed and synthetic spectra for Me 1-1 ( top panel) and S 190 ( bottom panel) in the spectral regions 6425-6453 Å. The solid lines in each panel correspond to the observed spectra and dotted lines correspond to the synthetic spectra calculated for $\log\epsilon ({\rm Ca})=6.33$ using $T_{\rm eff}=4500$ K and $\log g=2.0$ for Me 1-1 and $T_{\rm eff}=5300$ K and $\log g=3.0$ for S 190.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8388fig3.eps} \end{figure}$ Figure 3: The critical breakup velocity as a function of stellar mass for different values of $\log g$ from 0.0 to 2.0 (solid lines). The dashed horizontal line with arrows shows v sin i for the cool central star in Me 1-1 (90 km s^-1). The arrows indicate that this value is a lower limit to the true equatorial rotational velocity.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8388fig4.eps} \end{figure}$ Figure 4: Line profiles of several emission lines in Me 1-1. The intensity of each line has been normalized to its intensity peak. The H $\alpha$ profile is presented at two different scales in order to show the broad wings of the H $\alpha$ emission.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8388fig5.eps} \end{figure}$ Figure 5: Grey-scale representation of the [N II] image of Me 1-1. The grey leves are linear. The origin (0, 0) corresponds to the position of the central star (labelled).
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{8388fig6.eps} \end{figure}$ Figure 6: The position of Me 1-1 (filled circle) in a $\log g - \log T_{\rm eff}$ diagram along with stellar model evolutionary tracks from Schaerer et al. (1993). The positions of three D $^{\prime }$ -type symbiotic stars is also shown, S 190 (filled square), AS 201 (open circle) and HD 330036 (open square).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{8388fig7.eps} \end{figure}$ Figure 7: [Ba/Fe] vs. effective temperature for D'-type symbiotics and Me 1-1. Symbols have the same meaning as in Fig. 6.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8388fig8.eps} \end{figure}$ Figure 8: Position of planetary nebulae, D'-, D- and S-type symbiotics, in the $\lambda$ 5007/H $\beta$ - $\lambda$ 4363/H $\gamma$ plane. Open squares, planetary nebulae; filled square points, D-type symbiotics; filled triangles, S-type symbiotics; D'-type symbiotics, asterisks; Me 1-1, open circle. Data from Kingsburgh & Barlow (1994), Schmid & Nussbaumer (1993), Gutiérrez-Moreno & Moreno (1996), Schmid & Schild (1990), Pereira (1995), Pereira et al. (1998), Gutiérrez-Moreno et al. (1999).
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{8388fig1.eps} \end{figure}$	Figure 1: Observed and synthetic spectra for Me 1-1 a) and S 190 b) displaying broad lines and indicating rotationally broadened profiles. The observed spectra are plotted along with three synthetic spectra computed for three different surface gravities showing the sensitivity of the Fe II (and Ba II to $\log g$ ).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{8388fig3.eps} \end{figure}$	Figure 3: The critical breakup velocity as a function of stellar mass for different values of $\log g$ from 0.0 to 2.0 (solid lines). The dashed horizontal line with arrows shows v sin i for the cool central star in Me 1-1 (90 km s^-1). The arrows indicate that this value is a lower limit to the true equatorial rotational velocity.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8388fig4.eps} \end{figure}$	Figure 4: Line profiles of several emission lines in Me 1-1. The intensity of each line has been normalized to its intensity peak. The H $\alpha$ profile is presented at two different scales in order to show the broad wings of the H $\alpha$ emission.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8388fig5.eps} \end{figure}$	Figure 5: Grey-scale representation of the [N II] image of Me 1-1. The grey leves are linear. The origin (0, 0) corresponds to the position of the central star (labelled).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6cm,clip]{8388fig6.eps} \end{figure}$	Figure 6: The position of Me 1-1 (filled circle) in a $\log g - \log T_{\rm eff}$ diagram along with stellar model evolutionary tracks from Schaerer et al. (1993). The positions of three D $^{\prime }$ -type symbiotic stars is also shown, S 190 (filled square), AS 201 (open circle) and HD 330036 (open square).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{8388fig7.eps} \end{figure}$	Figure 7: [Ba/Fe] vs. effective temperature for D'-type symbiotics and Me 1-1. Symbols have the same meaning as in Fig. 6.
Open with DEXTER