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$\begin{figure} \par\resizebox{16.6cm}{!}{\includegraphics{0265fig1.eps}} \end{figure}$ Figure 1: Evolution of [Eu/Fe] and [Ba $^{\rm r}$ /Fe] abundances as a function of metallicity [Fe/H]. Lower-mass SNe II (8- $10 ~ {M}_{\odot}$ , Model SN810) are assumed to be the dominating r-process sources. Black dots denote model stars, observations are marked by filled squares and diamonds (see text). Average ISM abundances are marked by a continuous line. Filled circles with error bars denote average abundances of model stars and their standard deviation in [Fe/H] bins with binsize 0.1 dex.
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In the text

$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics{0265fig2.eps}} \end{figure}$ Figure 2: Evolution of [Eu/Fe] and [Ba $^{\rm r}$ /Fe] abundances as a function of metallicity [Fe/H]. Higher-mass SNe II (20- $25 ~ {M}_{\odot}$ , Model SN2025) are assumed to be the dominating r-process sources. Symbols are as in Fig. 1.
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In the text

$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics{0265fig3.eps}} \end{figure}$ Figure 3: Evolution of [Eu/Fe] and [Ba $^{\rm r}$ /Fe] abundances as a function of metallicity [Fe/H]. Higher-mass SNe II (20- $50 ~ {M}_{\odot}$ , Model SN2050) are assumed to be the dominating r-process sources. Symbols are as in Fig. 1.
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In the text

$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics{0265fig4.eps}} \end{figure}$ Figure 4: Evolution of [Eu/Fe] and [Ba $^{\rm r}$ /Fe] abundances as a function of metallicity [Fe/H]. NSM with a rate of $2 \times 10^{-4} ~ {\rm yr}^{-1}$ , a coalescence timescale of 10⁶ yr and $10^{-3} ~ {M}_{\odot}$ of ejected r-process matter are assumed to be the dominating r-process sources. Symbols are as in Fig. 1. The right-hand panel of this figure is reproduced in the upper right panel of Fig. 5.
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In the text

$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics{0265fig5.eps}} \end{figure}$ Figure 5: [Ba $^{\rm r}$ /Fe] vs. [Fe/H] for the NSM rates $2 \times 10^{-3} ~ {\rm yr}^{-1}$ , $2 \times 10^{-4} ~ {\rm yr}^{-1}$ , $2 \times 10^{-5} ~ {\rm yr}^{-1}$ and $2 \times 10^{-6} ~ {\rm yr}^{-1}$ (from left to right and top to bottom). The coalescence timescale adopted in these cases is $t_{\rm c}=10^6$ yr.
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In the text

$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics{0265fig6.eps}} \end{figure}$ Figure 6: Same as Fig. 5 but with $t_{\rm c} = 10^8$ yr.
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In the text

$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics{0265fig7.eps}} \end{figure}$ Figure 7: $\log \epsilon ( {\rm Ba}^{\rm r} )$ vs. [Fe/H] of model SN2050 ( left panel) and NSM occurring at a rate of $2 \times 10^{-5}$ yr^-1 ( right panel). Symbols are as in Fig. 1. Additionally, numbered circles in the left panel give $\log \epsilon ( {\rm Ba}^{\rm r} )$ of SNe II with the indicated progenitor mass, when mixed with $5 \times 10^4 ~ {M}_{\odot}$ of primordial ISM. Similarly, the labelled circle in the right panel indicates $\log \epsilon ( {\rm Ba}^{\rm r} )$ of NSM when mixed with $5 \times 10^4 ~ {M}_{\odot}$ of enriched ISM (at [Fe/H] =-2).
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In the text

$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics{0265fig2.eps}} \end{figure}$	Figure 2: Evolution of [Eu/Fe] and [Ba $^{\rm r}$ /Fe] abundances as a function of metallicity [Fe/H]. Higher-mass SNe II (20- $25 ~ {M}_{\odot}$ , Model SN2025) are assumed to be the dominating r-process sources. Symbols are as in Fig. 1.
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$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics{0265fig3.eps}} \end{figure}$	Figure 3: Evolution of [Eu/Fe] and [Ba $^{\rm r}$ /Fe] abundances as a function of metallicity [Fe/H]. Higher-mass SNe II (20- $50 ~ {M}_{\odot}$ , Model SN2050) are assumed to be the dominating r-process sources. Symbols are as in Fig. 1.
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$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics{0265fig5.eps}} \end{figure}$	Figure 5: [Ba $^{\rm r}$ /Fe] vs. [Fe/H] for the NSM rates $2 \times 10^{-3} ~ {\rm yr}^{-1}$ , $2 \times 10^{-4} ~ {\rm yr}^{-1}$ , $2 \times 10^{-5} ~ {\rm yr}^{-1}$ and $2 \times 10^{-6} ~ {\rm yr}^{-1}$ (from left to right and top to bottom). The coalescence timescale adopted in these cases is $t_{\rm c}=10^6$ yr.
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$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics{0265fig6.eps}} \end{figure}$	Figure 6: Same as Fig. 5 but with $t_{\rm c} = 10^8$ yr.
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