Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{Hb091_f1.ps}\end{figure}$ Figure 1: Upper panel: the SFR for the halo and the thick disk ( dotted and dashed curves, respectively), plotted as function of [Fe/H]. Lower panel: [O/Fe] vs. [Fe/H] diagram for our sample stars ( filled squares: dissipative component; empty squares: accretion component). An asterisk denotes the position of the chemically peculiar star HD 74000, belonging to the accretion component. The median absolute abundance error bar is given. Note that the uncertainty in the relative abundances will be smaller. The abundance ratios predicted by our model for the halo and the thick disk are shown by the dotted and dashed curves, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=6.1cm,clip]{Hb091_f2.ps}\end{figure}$ Figure 2: Upper panel: the SFR for the halo and the thick disk ( dotted and dashed curves, respectively) as function of $\log~ ({\rm Be/H})$ . Lower panel: [O/Fe] vs. $\log~ ({\rm Be/H})$ diagram for our sample stars (same symbols and line types as in Fig. 1). Notice the good agreement between the thick disk model and the dissipative component.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{Hb091_f3.ps}\end{figure}$ Figure 3: Diagram of [ $\alpha$ /Fe] vs. [Fe/H] and $\log~ ({\rm Be/H})$ , where $\alpha$ is the average of the abundances of Mg, Ca, Si, and Ti (same symbols as in Figs. 1 and 2).
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In the text

$\begin{figure} \par\includegraphics[width=6.1cm,clip]{Hb091_f2.ps}\end{figure}$	Figure 2: Upper panel: the SFR for the halo and the thick disk ( dotted and dashed curves, respectively) as function of $\log~ ({\rm Be/H})$ . Lower panel: [O/Fe] vs. $\log~ ({\rm Be/H})$ diagram for our sample stars (same symbols and line types as in Fig. 1). Notice the good agreement between the thick disk model and the dissipative component.
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$\begin{figure} \par\includegraphics[width=6.2cm,clip]{Hb091_f3.ps}\end{figure}$	Figure 3: Diagram of [ $\alpha$ /Fe] vs. [Fe/H] and $\log~ ({\rm Be/H})$ , where $\alpha$ is the average of the abundances of Mg, Ca, Si, and Ti (same symbols as in Figs. 1 and 2).
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