Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1034fig1.ps} \end{figure}$ Figure 1: The position in the diagram dereddened c₁ vs. b-y is shown as proof of the similar evolutionary stage of the stars. Filled squares represent stars with measurements of Fe II lines and thus spectroscopic estimate of log(g). Empty squares are used for stars with no Fe II measurements.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1034fig2.ps} % \end{figure}$ Figure 2: Calibration of the spectroscopic log(g) vs. the gravity sensitive dereddened c₁ photometric index. The empty square represents the star LP635-14 that was rejected from the fit by a 2 $\sigma$ clipping procedure.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1034fig3.ps} \end{figure}$ Figure 3: A comparison between the Fe estimates of this study and the 1 Å (filled squares) and literature (empty squares) estimates respectively. Overplotted are the two linear fits.
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In the text

$\begin{figure} \par\includegraphics[width=13.5cm,clip]{1034fig4.ps} \end{figure}$ Figure 4: Abundances are shown as [el/Fe] vs. [Fe/H]. Empty squares are stars with no Fe II measurements. In the case of Mg and Ca, we show the results of a linear fit (thick line) and the $\pm 1\sigma$ region. This is not shown for Ti and Cr because of the small number of stars with Ti and Cr measurements.
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{1034fig5.ps} \end{figure}$ Figure 5: The standard deviation of the dispersion in [Mg/Fe] predicted by the model of Argast et al. (2002, their Fig. 1), in the case of SN II yields adopted from Thielemann et al. (1996). The dotted, small dashed and the dashed lines show the standard deviation over the metallicity range of our observations, -3.4 < [Fe/H] < -2.2, respectively for Argast et al. (2002), Cayrel et al. (2003) and this work.
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{1034fig6.ps} \end{figure}$ Figure 6: The standard deviation of the dispersion in [Mg/Fe] predicted by the model of Argast et al. (2002, their Fig. 14), in the case of their H1 model. The dotted, small dashed and the dashed lines show the standard deviation over the metallicity range of our observations, -3.4 < [Fe/H] < -2.2, respectively for Argast et al. (2002), Cayrel et al. (2003) and this work.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1034fig1.ps} \end{figure}$	Figure 1: The position in the diagram dereddened c₁ vs. b-y is shown as proof of the similar evolutionary stage of the stars. Filled squares represent stars with measurements of Fe II lines and thus spectroscopic estimate of log(g). Empty squares are used for stars with no Fe II measurements.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1034fig2.ps} % \end{figure}$	Figure 2: Calibration of the spectroscopic log(g) vs. the gravity sensitive dereddened c₁ photometric index. The empty square represents the star LP635-14 that was rejected from the fit by a 2 $\sigma$ clipping procedure.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1034fig3.ps} \end{figure}$	Figure 3: A comparison between the Fe estimates of this study and the 1 Å (filled squares) and literature (empty squares) estimates respectively. Overplotted are the two linear fits.
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$\begin{figure} \par\includegraphics[width=13.5cm,clip]{1034fig4.ps} \end{figure}$	Figure 4: Abundances are shown as [el/Fe] vs. [Fe/H]. Empty squares are stars with no Fe II measurements. In the case of Mg and Ca, we show the results of a linear fit (thick line) and the $\pm 1\sigma$ region. This is not shown for Ti and Cr because of the small number of stars with Ti and Cr measurements.
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$\begin{figure} \par\includegraphics[width=8.35cm,clip]{1034fig6.ps} \end{figure}$	Figure 6: The standard deviation of the dispersion in [Mg/Fe] predicted by the model of Argast et al. (2002, their Fig. 14), in the case of their H1 model. The dotted, small dashed and the dashed lines show the standard deviation over the metallicity range of our observations, -3.4 < [Fe/H] < -2.2, respectively for Argast et al. (2002), Cayrel et al. (2003) and this work.
Open with DEXTER