All Figures

$\begin{figure} \par\includegraphics[width=14cm,clip]{4968fig1} \end{figure}$ Figure 1: $\log\epsilon$ (X) vs. atmospheric parameters ([Fe/H], $T_{\rm eff}$ , $\log~ g$ ) for normal stars. Symbols indicate different references: open squares: Gratton & Sneden (1994); open circles: Burris et al. (2000); open triangles: Tomkin & Lambert (1999); filled triangles: Jehin et al. (1999); crosses: Edvardsson et al. (1993) and Woolf et al. (1995); filled squares: Smith et al. (2000); open pentagon Mashonkina & Gehren (2001). Uncertainties were taken from the respective references; otherwise, the values of $\pm$ 0.1 for [Fe/H] and $\pm$ 0.05 for $\log\epsilon$ (X) were used. These values were also attributed to Jehin et al. (1999), given that their uncertainties seem underestimated.
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In the text

$\begin{figure} \par\includegraphics[width=13.5cm,clip]{4968fig2} \end{figure}$ Figure 2: Same as Fig. 1 for other elements.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4968fig3} \end{figure}$ Figure 3: Total abundances of heavy elements for the barium ( $\log\epsilon(X)$ ) and normal ( $\log\epsilon_{\rm nor}(X)$ ) stars with the same metallicities. Solid lines indicate $\log\epsilon_{\rm nor}(X) = \log\epsilon(X)$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fig4} \end{figure}$ Figure 4: Abundance fraction of heavy elements due to all processes except the s-process main component ( $\log\epsilon_{\rm o}(X)$ ) vs. total abundance of barium stars ( $\log\epsilon(X)$ ). Solid lines indicate $\log\epsilon_{\rm o}(X) = \log\epsilon(X)$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fig5} \end{figure}$ Figure 5: Abundances corresponding to the s-process main component for heavy elements of barium stars ( $\log\epsilon_{\rm s} (X)$ ) vs. normal stars ( $\log\epsilon_{\rm s}(X)_{\rm nor}$ ) with the same metallicities. Solid lines indicate $\log\epsilon_{\rm s} (X)_{\rm nor} = \log\epsilon_{\rm s}(X)$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fig6} \end{figure}$ Figure 6: $\log\epsilon_{\rm s} (X)$ vs. [Fe/H], where $\log\epsilon_{\rm s} (X)$ are the abundances corresponding to the s-process main component of heavy elements in barium stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4968fig7} \end{figure}$ Figure 7: $\log\epsilon$ (X) vs. [Fe/H] for present sample of barium stars and post-AGBs from Reyniers et al. (2004) and van Winckel & Reyniers (2000). Filled symbols indicate barium stars; squares: $\log g \ge 3.7$ ; triangles: $2.4 < \log g < 3.7$ ; circles: $\log g \le 2.4$ . Open circles are post-AGBs.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{4968fig8} \end{figure}$ Figure 8: $\log\epsilon$ (Eu) vs. $\log\epsilon(X)$ for normal, post-AGB, and barium stars. Normal stars from the literature are represented by symbols as in Fig. 1. Starred squares are the present sample of barium stars. Starred triangles are post-AGB from Reyniers et al. (2004) and van Winckel & Reyniers (2000). Solid lines in the Ba panel represent r-only production of Ba (upper line) and solar [Ba/Eu] (lower line).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fig9} \end{figure}$ Figure 9: $\log\epsilon_{\rm r}$ (Eu) vs. $\log\epsilon_{\rm s} (X)$ , where $\log\epsilon_{\rm r}$ (Eu) is the abundance fraction due to r-process for Eu and $\log\epsilon_{\rm s} (X)$ is that due to s-process main component for other heavy elements in barium stars.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fi10} \end{figure}$ Figure 10: $\log\epsilon_{\rm r}$ (Eu) vs. $\log\epsilon_{\rm r}(X)$ , where $\log\epsilon_{\rm r}$ (Eu) and $\log\epsilon_{\rm r}(X)$ are the abundance fractions due to r-process for Eu and other heavy elements in barium stars, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fi11} \end{figure}$ Figure 11: Abundance ratios involving s- and r-processes, light and heavy s-elements. Uncertainties indicated are the highest values of Table 7 for each panel. Symbols are the same as in Fig. 7.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4968fi12} \end{figure}$ Figure 12: Fittings of observed data to theoretical predictions by Malaney (1987b,a).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4968fi13} \end{figure}$ Figure 13: Same as Fig. 12 for 6 other sample stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4968fi14} \end{figure}$ Figure 14: Same as Fig. 12 for 6 other sample stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4968fi15} \end{figure}$ Figure 15: Same as Fig. 12 for 8 other sample stars.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{4968fi16} \end{figure}$ Figure 16: Example of the fit of parameters G and $\tau _{\rm o}$ for the barium star HD 123585. Open symbols correspond to the use of ${\partial \chi \over \partial G}=0$ and filled symbols, ${\partial \chi \over \partial \tau _{\rm o}}=0$ . From left to right the plot is zoomed in order to visualise the crossing of the two functions better.
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In the text

$\begin{figure} \par\includegraphics[width=13.7cm,clip]{4968fi17} \end{figure}$ Figure 17: Solar $\sigma N$ curve. Abundances related to s-process main component were taken from Arlandini et al. (1999).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4968fi22} \end{figure}$ Figure 22: [hs/ls], [ls/Fe], [hs/Fe], and [s/Fe] vs. [Fe/H]. Filled symbols indicate barium stars, as in Fig. 7; open circles are post-AGBs; crosses are data from Junqueira & Pereira (2001); open squares are data from Luck & Bond (1991); open triangles are data from North et al. (1994). The uncertainties indicated are the higher values shown in Table 9.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4968fi23} \end{figure}$ Figure 23: [hs/ls] vs. [s/Fe]. Symbols are the same as in Fig. 7. Error bars in the bottom right corner show the largest uncertainties.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fi24} \end{figure}$ Figure 24: [hs/ls] vs. $\tau _{\rm o}$ ( upper panel), and $\tau _{\rm o}$ vs. [Fe/H] ( lower panel). Crosses are post-AGBs from Reyniers et al. (2004) and van Winckel & Reyniers (2000). Circles, triangles, and squares represent the sample of barium stars according to log g, as in Fig. 7. Open symbols correspond to $\tau _{\rm o}$ values derived from theoretical predictions by Malaney (1987b,a) and filled symbols are those from $\sigma N$ curves. The solid line is the least-square fitting with $\tau _{\rm o}$ from $\sigma N$ curves and dotted, with $\tau _{\rm o}$ from theoretical predictions.
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In the text

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{4968fi18} \end{figure}$ Figure 18: The $\sigma N$ curves for the sample of barium stars. Open squares represent the solar distribution of abundances (Col. 18 of Table 6) and filled squares represent the distribution taking the overabundance of barium stars into account (Col. 16 of Table 6). Error bars in the HD 749 panel at A=190 and A=195 indicate the typical errors in each region of the logarithmic scale.
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In the text

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{4968fi19} \end{figure}$ Figure 19: Same as Fig. 18 for 6 other sample stars.
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In the text

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{4968fi20} \end{figure}$ Figure 20: Same as Fig. 18 for 6 other sample stars.
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In the text

$\begin{figure} \par\includegraphics[width=17.3cm,clip]{4968fi21} \end{figure}$ Figure 21: Same as Fig. 18 for 8 other sample stars.
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In the text

$\begin{figure} \par\includegraphics[width=13.5cm,clip]{4968fig2} \end{figure}$	Figure 2: Same as Fig. 1 for other elements.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4968fig3} \end{figure}$	Figure 3: Total abundances of heavy elements for the barium ( $\log\epsilon(X)$ ) and normal ( $\log\epsilon_{\rm nor}(X)$ ) stars with the same metallicities. Solid lines indicate $\log\epsilon_{\rm nor}(X) = \log\epsilon(X)$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fig4} \end{figure}$	Figure 4: Abundance fraction of heavy elements due to all processes except the s-process main component ( $\log\epsilon_{\rm o}(X)$ ) vs. total abundance of barium stars ( $\log\epsilon(X)$ ). Solid lines indicate $\log\epsilon_{\rm o}(X) = \log\epsilon(X)$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fig5} \end{figure}$	Figure 5: Abundances corresponding to the s-process main component for heavy elements of barium stars ( $\log\epsilon_{\rm s} (X)$ ) vs. normal stars ( $\log\epsilon_{\rm s}(X)_{\rm nor}$ ) with the same metallicities. Solid lines indicate $\log\epsilon_{\rm s} (X)_{\rm nor} = \log\epsilon_{\rm s}(X)$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fig6} \end{figure}$	Figure 6: $\log\epsilon_{\rm s} (X)$ vs. [Fe/H], where $\log\epsilon_{\rm s} (X)$ are the abundances corresponding to the s-process main component of heavy elements in barium stars.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4968fig7} \end{figure}$	Figure 7: $\log\epsilon$ (X) vs. [Fe/H] for present sample of barium stars and post-AGBs from Reyniers et al. (2004) and van Winckel & Reyniers (2000). Filled symbols indicate barium stars; squares: $\log g \ge 3.7$ ; triangles: $2.4 < \log g < 3.7$ ; circles: $\log g \le 2.4$ . Open circles are post-AGBs.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fig9} \end{figure}$	Figure 9: $\log\epsilon_{\rm r}$ (Eu) vs. $\log\epsilon_{\rm s} (X)$ , where $\log\epsilon_{\rm r}$ (Eu) is the abundance fraction due to r-process for Eu and $\log\epsilon_{\rm s} (X)$ is that due to s-process main component for other heavy elements in barium stars.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fi10} \end{figure}$	Figure 10: $\log\epsilon_{\rm r}$ (Eu) vs. $\log\epsilon_{\rm r}(X)$ , where $\log\epsilon_{\rm r}$ (Eu) and $\log\epsilon_{\rm r}(X)$ are the abundance fractions due to r-process for Eu and other heavy elements in barium stars, respectively.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4968fi11} \end{figure}$	Figure 11: Abundance ratios involving s- and r-processes, light and heavy s-elements. Uncertainties indicated are the highest values of Table 7 for each panel. Symbols are the same as in Fig. 7.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4968fi12} \end{figure}$	Figure 12: Fittings of observed data to theoretical predictions by Malaney (1987b,a).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4968fi13} \end{figure}$	Figure 13: Same as Fig. 12 for 6 other sample stars.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4968fi14} \end{figure}$	Figure 14: Same as Fig. 12 for 6 other sample stars.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4968fi15} \end{figure}$	Figure 15: Same as Fig. 12 for 8 other sample stars.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{4968fi16} \end{figure}$	Figure 16: Example of the fit of parameters G and $\tau _{\rm o}$ for the barium star HD 123585. Open symbols correspond to the use of ${\partial \chi \over \partial G}=0$ and filled symbols, ${\partial \chi \over \partial \tau _{\rm o}}=0$ . From left to right the plot is zoomed in order to visualise the crossing of the two functions better.
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$\begin{figure} \par\includegraphics[width=13.7cm,clip]{4968fi17} \end{figure}$	Figure 17: Solar $\sigma N$ curve. Abundances related to s-process main component were taken from Arlandini et al. (1999).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4968fi22} \end{figure}$	Figure 22: [hs/ls], [ls/Fe], [hs/Fe], and [s/Fe] vs. [Fe/H]. Filled symbols indicate barium stars, as in Fig. 7; open circles are post-AGBs; crosses are data from Junqueira & Pereira (2001); open squares are data from Luck & Bond (1991); open triangles are data from North et al. (1994). The uncertainties indicated are the higher values shown in Table 9.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4968fi23} \end{figure}$	Figure 23: [hs/ls] vs. [s/Fe]. Symbols are the same as in Fig. 7. Error bars in the bottom right corner show the largest uncertainties.
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$\begin{figure} \par\includegraphics[width=17.4cm,clip]{4968fi18} \end{figure}$	Figure 18: The $\sigma N$ curves for the sample of barium stars. Open squares represent the solar distribution of abundances (Col. 18 of Table 6) and filled squares represent the distribution taking the overabundance of barium stars into account (Col. 16 of Table 6). Error bars in the HD 749 panel at A=190 and A=195 indicate the typical errors in each region of the logarithmic scale.
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$\begin{figure} \par\includegraphics[width=17.4cm,clip]{4968fi19} \end{figure}$	Figure 19: Same as Fig. 18 for 6 other sample stars.
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$\begin{figure} \par\includegraphics[width=17.4cm,clip]{4968fi20} \end{figure}$	Figure 20: Same as Fig. 18 for 6 other sample stars.
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$\begin{figure} \par\includegraphics[width=17.3cm,clip]{4968fi21} \end{figure}$	Figure 21: Same as Fig. 18 for 8 other sample stars.
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