All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{8571.F01.eps}\end{figure}$ Figure 1: The SN Ia rate (solid line) and SN II rate (dashed line) in the halo. Note that the rate of SNe Ia is multiplied by ten.
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F02.eps}\end{figure}$ Figure 2: [Eu/Fe] vs. [Fe/H]. The abundances of simulated living stars at the present time are indicated by the blue dots. The red triangles are the observational data from various authors (see Table 1). The dashed line is the prediction of the homogeneous model (Cescutti et al. 2006, model 1).
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F03.eps}\end{figure}$ Figure 3: As in Fig. 2, but for [Ba/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (Cescutti et al. 2006, model 1).
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F04.eps}\end{figure}$ Figure 4: As in Fig. 2, but for [La/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (Cescutti et al. 2007).
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F05.eps}\end{figure}$ Figure 5: As in Fig. 2, but for [Sr/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (Cescutti 2007).
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F06.eps}\end{figure}$ Figure 6: As in Fig. 2, but for [Y/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (Cescutti 2007).
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F07.eps}\end{figure}$ Figure 7: As in Fig. 2, but for [Zr/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (Cescutti 2007).
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F08.eps}\end{figure}$ Figure 8: As in Fig. 2, but for [Si/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (François et al. 2004).
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F09.eps}\end{figure}$ Figure 9: As in Fig. 2, but for [Ca/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (François et al. 2004).
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F10.eps}\end{figure}$ Figure 10: As in Fig. 2, but for [Mg/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (François et al. 2004).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{8571.F11.eps}\end{figure}$ Figure 11: The relative frequency of stars at a given [Si/Fe] ratio for different enrichment phases. In solid line the predictions of the model for the living stars at the present time, in dashed line the observational data. The authors of the observational data are listed in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{8571.F12.eps}\end{figure}$ Figure 12: As in Fig. 11, but for [Eu/Fe]. The authors of the observational data are listed in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F13.eps}\end{figure}$ Figure 13: [Ba/Eu] vs. [Fe/H]. The abundances of simulated living stars at the present time in blue dots, the red triangles are the observational data from Burris et al. (2000); François et al. (2007); Fulbright (2000, 2002); Gilroy et al. (1998); Gratton & Sneden (1994); Honda et al. (2004); Ishimaru et al. (2004); Johnson (2002); Mashonkina & Gehren (2000, 2001); McWilliam et al. (1995); McWilliam & Rich (1994); Prochaska et al. (2000); Ryan et al. (1991, 1996); Stephens (1999); and Stephens & Boesgaard (2002). The dashed line is the prediction of the homogeneous model (Cescutti et al. 2006, model 1).
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F14.eps}\end{figure}$ Figure 14: As in Fig. 13 but for [Ba/Y] vs. [Fe/H]. The data for this elements are from Burris et al. (2000); François et al. (2007); Fulbright (2000, 2002); Gilroy et al. (1998); Gratton & Sneden (1994); Honda et al. (2004); Ishimaru et al. (2004); Johnson (2002); McWilliam et al. (1995); McWilliam & Rich (1994); Nissen & Schuster (1997); Prochaska et al. (2000); and Ryan et al. (1991, 1996). The dashed line is the prediction of the homogeneous model (Cescutti 2007).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8571.F01.eps}\end{figure}$	Figure 1: The SN Ia rate (solid line) and SN II rate (dashed line) in the halo. Note that the rate of SNe Ia is multiplied by ten.
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$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F02.eps}\end{figure}$	Figure 2: [Eu/Fe] vs. [Fe/H]. The abundances of simulated living stars at the present time are indicated by the blue dots. The red triangles are the observational data from various authors (see Table 1). The dashed line is the prediction of the homogeneous model (Cescutti et al. 2006, model 1).
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$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F03.eps}\end{figure}$	Figure 3: As in Fig. 2, but for [Ba/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (Cescutti et al. 2006, model 1).
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$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F04.eps}\end{figure}$	Figure 4: As in Fig. 2, but for [La/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (Cescutti et al. 2007).
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$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F05.eps}\end{figure}$	Figure 5: As in Fig. 2, but for [Sr/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (Cescutti 2007).
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$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F06.eps}\end{figure}$	Figure 6: As in Fig. 2, but for [Y/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (Cescutti 2007).
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$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F07.eps}\end{figure}$	Figure 7: As in Fig. 2, but for [Zr/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (Cescutti 2007).
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$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F08.eps}\end{figure}$	Figure 8: As in Fig. 2, but for [Si/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (François et al. 2004).
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$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F09.eps}\end{figure}$	Figure 9: As in Fig. 2, but for [Ca/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (François et al. 2004).
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$\begin{figure} \par\includegraphics[width=7.85cm,clip]{8571.F10.eps}\end{figure}$	Figure 10: As in Fig. 2, but for [Mg/Fe]. The authors of the observational data are listed in Table 1. The dashed line is the prediction of the homogeneous model (François et al. 2004).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{8571.F11.eps}\end{figure}$	Figure 11: The relative frequency of stars at a given [Si/Fe] ratio for different enrichment phases. In solid line the predictions of the model for the living stars at the present time, in dashed line the observational data. The authors of the observational data are listed in Table 1.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{8571.F12.eps}\end{figure}$	Figure 12: As in Fig. 11, but for [Eu/Fe]. The authors of the observational data are listed in Table 1.
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