All Figures

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5440fig1.eps} \end{figure}$ Figure 1: Observed (crosses) and synthetic spectra (lines) of CS 31080-095, CS 22958-042, and CS 29528-041 in the region of the Li I 670.7 nm doublet. Li is not detected in CS 22958-042.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5440fig2.eps} \end{figure}$ Figure 2: Observed and synthetic spectra of our stars around the 388.3 nm CN band (symbols as in Fig. 1). The strong CN bands in CS 22958-042 indicate a larger N excess than in CS 31080-095. In CS 29528-041 the CN bands are weak, but the derived [N/H] is high because [C/H] is low and $T_{\rm eff}$ is high. The 336 nm NH bands are also detected in CS 29528-041 and CS 22958-042 (not shown).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5440fig3.eps} \end{figure}$ Figure 3: Observed spectra (crosses) for the two stars with meaningful measurements or limits on the ¹²C/¹³C ratio. Solid, dotted, dashed, and dash-dotted lines show our synthetic spectra for ¹²C/¹³C = 99, 40, 9, and 3, respectively. For CS 29528-041 all ¹²C/¹³C ratios between 3 and 99 are within a 2 $\sigma$ detection limit; hence, no ¹²C/¹³C is given for this star.
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In the text

$\begin{figure} \includegraphics[width=11cm,clip]{5440fig4.eps} \end{figure}$ Figure 4: [N/Fe] vs. [C/Fe] for CEMP stars from the recent literature (Table 4). The $\times$ and $\triangle$ symbols represent the mixed and unmixed giants from Spite et al. (2005); the + and $\diamond$ signs represent stars with log g < 3.5 and log g > 3.5, respectively. Stars with significant Li detections are surrounded by a $\sq$ (filled symbols: this paper). The AGB model predictions by Herwig (2004) for [Fe/H] = -2.3 and initial masses 6 $M_\odot$ (HBB) and 2 $M_\odot$ (non-HBB) are shown by $\triangledown$ symbols. HE 0107-5240 and HE 1327-2326 are the two known HMP stars.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5440fig5.eps} \end{figure}$ Figure 5: [Sr/Fe] vs. [Ba/Sr] for the CEMP stars in Table 4 (filled symbols: this paper). [Ba/Sr] ratios for CS 31080-095 and CS 29528-041 falls in between CEMP-s stars and CEMP-no stars.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=11cm,clip,origin=rb]{5440fig6.eps} \end{figure}$ Figure 6: Top: element enhancements in VMP AGB model ejecta ([Fe/H] = -2.3; Z = 0.0001). Bottom: observed abundances in our stars (open symbols: upper limits). The abundances of CS 29528-041 agree well with HBB model predictions for an AGB mass of 4-6 $M_\odot$ , but the other two stars are better matched by lower-mass AGB models. However, the observed high N abundances require enhanced mixing, and the observed Na may differ more than expected from current models.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5440fig7.eps} \end{figure}$ Figure 7: ¹²C/¹³C vs. A(Li) for the CEMP stars in Table 4 (symbols as in Fig. 4; arrows indicate limits). The Li-rich CEMP stars tend to have high ¹²C/¹³C ratios.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5440fig1.eps} \end{figure}$	Figure 1: Observed (crosses) and synthetic spectra (lines) of CS 31080-095, CS 22958-042, and CS 29528-041 in the region of the Li I 670.7 nm doublet. Li is not detected in CS 22958-042.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{5440fig2.eps} \end{figure}$	Figure 2: Observed and synthetic spectra of our stars around the 388.3 nm CN band (symbols as in Fig. 1). The strong CN bands in CS 22958-042 indicate a larger N excess than in CS 31080-095. In CS 29528-041 the CN bands are weak, but the derived [N/H] is high because [C/H] is low and $T_{\rm eff}$ is high. The 336 nm NH bands are also detected in CS 29528-041 and CS 22958-042 (not shown).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{5440fig3.eps} \end{figure}$	Figure 3: Observed spectra (crosses) for the two stars with meaningful measurements or limits on the ¹²C/¹³C ratio. Solid, dotted, dashed, and dash-dotted lines show our synthetic spectra for ¹²C/¹³C = 99, 40, 9, and 3, respectively. For CS 29528-041 all ¹²C/¹³C ratios between 3 and 99 are within a 2 $\sigma$ detection limit; hence, no ¹²C/¹³C is given for this star.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{5440fig5.eps} \end{figure}$	Figure 5: [Sr/Fe] vs. [Ba/Sr] for the CEMP stars in Table 4 (filled symbols: this paper). [Ba/Sr] ratios for CS 31080-095 and CS 29528-041 falls in between CEMP-s stars and CEMP-no stars.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{5440fig7.eps} \end{figure}$	Figure 7: ¹²C/¹³C vs. A(Li) for the CEMP stars in Table 4 (symbols as in Fig. 4; arrows indicate limits). The Li-rich CEMP stars tend to have high ¹²C/¹³C ratios.
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