$\begin{figure} \par\includegraphics[width=6.5 cm,clip]{Gj211_f1.ps} \end{figure}$ Figure 1: Spectra of the three most probable CMa stars, in the region of the Mg b triplet. [Fe/H], $\log(g)$ and $T_{\rm eff}$ all increase from bottom to top. The spectra are normalized to one, stars 30077 and 6631 are shifted vertically for display purposes (continuum is at 2.5 for 30077 and at 4 for 6631).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{Gj211_f2.ps} \end{figure}$ Figure 2: Alpha elements abundances for the three sample stars, plotted against [Fe/H]. Triangles are Mg I, squares Si I, and open circles are Ca I. Error bars for single elements removed for clarity. Filled circles with error bars represent weighted means of Mg, Si, and Ca. Increasing in metallicity from left we have EIS 7873, 30077 and 6631.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{Gj211_f3.ps} \end{figure}$ Figure 3: Abundances for n-capture elements La (triangles), Ce (squares) and Nd (circles) plotted against metallicity.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{Gj211_f4.ps} \end{figure}$ Figure 4: Synthesis for the Cu I 510.5 nm line in EIS 6631 (thick line) with superimposed the observed spectrum. Hyperfine splitting is taken into account, [Cu/Fe] = +0.25 in the synthesis.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.5 cm,clip]{Gj211_f1.ps} \end{figure}$	Figure 1: Spectra of the three most probable CMa stars, in the region of the Mg b triplet. [Fe/H], $\log(g)$ and $T_{\rm eff}$ all increase from bottom to top. The spectra are normalized to one, stars 30077 and 6631 are shifted vertically for display purposes (continuum is at 2.5 for 30077 and at 4 for 6631).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{Gj211_f2.ps} \end{figure}$	Figure 2: Alpha elements abundances for the three sample stars, plotted against [Fe/H]. Triangles are Mg I, squares Si I, and open circles are Ca I. Error bars for single elements removed for clarity. Filled circles with error bars represent weighted means of Mg, Si, and Ca. Increasing in metallicity from left we have EIS 7873, 30077 and 6631.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{Gj211_f3.ps} \end{figure}$	Figure 3: Abundances for n-capture elements La (triangles), Ce (squares) and Nd (circles) plotted against metallicity.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{Gj211_f4.ps} \end{figure}$	Figure 4: Synthesis for the Cu I 510.5 nm line in EIS 6631 (thick line) with superimposed the observed spectrum. Hyperfine splitting is taken into account, [Cu/Fe] = +0.25 in the synthesis.
Open with DEXTER