All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig1.eps} \end{figure}$ Figure 1: [el/Fe] versus [Fe/H] for several $\alpha$ - elements compared to a large compilation of data (see text). The black dots represent the new data of Cayrel et al. (2004). Here we have adopted the yields of WW95 for massive stars and N97 for type Ia SNe taken as per their models.The model predictions are normalized to the predicted solar abundances, namely those predicted at 4.5 Gyr ago. In a corner of each panel we show our predicted solar abundance ratios. In some cases we fit the behavior of [el/Fe] vs. [Fe/H] but not the solar value, as it is the case for Mg.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig2.eps} \end{figure}$ Figure 2: The same as in Fig. 1 for several Fe- peak elements. The yields are taken at as per their models.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig3.eps} \end{figure}$ Figure 3: The same as in Fig. 1 for several Fe- peak elements. The yields are taken as per their models.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig4.eps} \end{figure}$ Figure 4: [el/Fe] versus [Fe/H] for several $\alpha$ -elements, as predicted by adopting the corrected yields, compared with a large data sample (Table 1). The model predictions are normalized to the predicted solar abundances, namely those predicted for the gas at 4.5 Gyr ago. As one can see, the model reproduces now both the behavior of abundance ratios and the solar abundances.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig5.eps} \end{figure}$ Figure 5: The same as Fig. 2 for some Fe-peak elements.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig6.eps} \end{figure}$ Figure 6: The same as Fig. 2 for some Fe-peak elements.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig7.eps} \end{figure}$ Figure 7: Ratios between the yields we adopted to obtain the best fit to the data and the yields of WW95 for massive stars and those of Iwamoto et al. (1999) for the nucleosynthesis in type Ia SNe. Notice that the oxygen yields are those of WW95 as a function of metallicity whereas all the other yields of WW95 refer to the solar chemical composition.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig8.eps} \end{figure}$ Figure 8: Ratios between the yields we adopted to obtain the best fit to the data and the yields of N97 for massive stars and those of Iwamoto et al. (1999) for type Ia SNe.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig9.eps} \end{figure}$ Figure 9: Ratios between the yields we adopted to obtain the best fit to the data and the yields of LC03 for massive stars and those of Iwamoto et al. (1999) for the nucleosynthesis in type Ia SNe.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig2.eps} \end{figure}$	Figure 2: The same as in Fig. 1 for several Fe- peak elements. The yields are taken at as per their models.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig3.eps} \end{figure}$	Figure 3: The same as in Fig. 1 for several Fe- peak elements. The yields are taken as per their models.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig4.eps} \end{figure}$	Figure 4: [el/Fe] versus [Fe/H] for several $\alpha$ -elements, as predicted by adopting the corrected yields, compared with a large data sample (Table 1). The model predictions are normalized to the predicted solar abundances, namely those predicted for the gas at 4.5 Gyr ago. As one can see, the model reproduces now both the behavior of abundance ratios and the solar abundances.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig5.eps} \end{figure}$	Figure 5: The same as Fig. 2 for some Fe-peak elements.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig6.eps} \end{figure}$	Figure 6: The same as Fig. 2 for some Fe-peak elements.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig7.eps} \end{figure}$	Figure 7: Ratios between the yields we adopted to obtain the best fit to the data and the yields of WW95 for massive stars and those of Iwamoto et al. (1999) for the nucleosynthesis in type Ia SNe. Notice that the oxygen yields are those of WW95 as a function of metallicity whereas all the other yields of WW95 refer to the solar chemical composition.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig8.eps} \end{figure}$	Figure 8: Ratios between the yields we adopted to obtain the best fit to the data and the yields of N97 for massive stars and those of Iwamoto et al. (1999) for type Ia SNe.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fig9.eps} \end{figure}$	Figure 9: Ratios between the yields we adopted to obtain the best fit to the data and the yields of LC03 for massive stars and those of Iwamoto et al. (1999) for the nucleosynthesis in type Ia SNe.
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