Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=12cm,clip]{0913fig1.eps}\end{figure}$ Figure 1: Spectra of UV copper and zinc lines in metal-poor dwarfs.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0913fig2.ps}\end{figure}$ Figure 2: Expanded plots of the solar spectral regions ( dotted lines) fitted with the synthetic spectrum ( solid lines).
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In the text

$\begin{figure} \par\includegraphics[width=8.65cm,clip]{0913fig3.eps}\end{figure}$ Figure 3: Comparison of the $T_{\rm eff}$ obtained in this study with spectroscopic $T_{\rm eff}$ from Fulbright ( triangles) and Mishenina & Kovtyukh ( squares).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0913fig4.eps}\end{figure}$ Figure 4: Comparison of the log g obtained in this study with spectroscopic log g from Fulbright ( triangles) and Mishenina & Kovtyukh ( squares).
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0913fig5.ps}\end{figure}$ Figure 5: Synthetic spectral fits to the copper and zinc lines in the spectra of several metal-poor stars of our sample.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{0913fig6.eps}\end{figure}$ Figure 6: [Cu/Fe] and [Zn/Fe] ratios vs. [Fe/H]. The upper limits of Zn abundances are represented by the arrows, the Cu abundance in the giant BD -18 $\hbox {$^\circ $ }$ 5550 by the square and the fit to the Cu data obtained by Mishenina et al. by the dotted line. The solid lines represent the predictions of the Prantzos model and the horizontal lines represent the elapsed time since the beginning of the halo formation.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0913fig7.ps}\end{figure}$ Figure 7: [Zn/Fe] ratios vs. [Fe/H] from our measurements ( filled dots), from Cayrel et al. ( filled triangles), from Mishenina et al. ( asterisks) and Gratton et al. ( crossed squares). The [Zn/Fe] values of Gratton et al. are decreased by 0.09 dex for normalization to meteoritic rather than to solar abundances.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0913fig8.eps}\end{figure}$ Figure 8: [Cu/Zn] ratios vs. [Zn/H]. The solid line represents the predictions of the Prantzos model.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{0913fig1.eps}\end{figure}$	Figure 1: Spectra of UV copper and zinc lines in metal-poor dwarfs.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{0913fig2.ps}\end{figure}$	Figure 2: Expanded plots of the solar spectral regions ( dotted lines) fitted with the synthetic spectrum ( solid lines).
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$\begin{figure} \par\includegraphics[width=8.65cm,clip]{0913fig3.eps}\end{figure}$	Figure 3: Comparison of the $T_{\rm eff}$ obtained in this study with spectroscopic $T_{\rm eff}$ from Fulbright ( triangles) and Mishenina & Kovtyukh ( squares).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0913fig4.eps}\end{figure}$	Figure 4: Comparison of the log g obtained in this study with spectroscopic log g from Fulbright ( triangles) and Mishenina & Kovtyukh ( squares).
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$\begin{figure} \par\includegraphics[width=14cm,clip]{0913fig5.ps}\end{figure}$	Figure 5: Synthetic spectral fits to the copper and zinc lines in the spectra of several metal-poor stars of our sample.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0913fig7.ps}\end{figure}$	Figure 7: [Zn/Fe] ratios vs. [Fe/H] from our measurements ( filled dots), from Cayrel et al. ( filled triangles), from Mishenina et al. ( asterisks) and Gratton et al. ( crossed squares). The [Zn/Fe] values of Gratton et al. are decreased by 0.09 dex for normalization to meteoritic rather than to solar abundances.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0913fig8.eps}\end{figure}$	Figure 8: [Cu/Zn] ratios vs. [Zn/H]. The solid line represents the predictions of the Prantzos model.
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