EDP Sciences
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Free Access
Issue
A&A
Volume 511, February 2010
Article Number L10
Number of page(s) 9
Section Letters
DOI https://doi.org/10.1051/0004-6361/200913877
Published online 16 March 2010

Online Material

\begin{figure}
\par\resizebox{8.8cm}{!}{\includegraphics{13877fig5.eps}}
\end{figure} Figure 5:

[Si/Fe], [Ca/Fe], and [Ti/Fe] as a function of [Fe/H]. The same symbols as in Fig. 1 are used.

Open with DEXTER

\begin{figure}
\par\resizebox{8.8cm}{!}{\includegraphics{13877fig6.eps}}
\end{figure} Figure 6:

[Na/Fe], [Cr/Fe], and [Ni/Fe] as a function of [Fe/H]. The same symbols as in Fig. 1 are used.

Open with DEXTER

\begin{figure}
\par\resizebox{8.8cm}{!}{\includegraphics{13877fig7.eps}}
\end{figure} Figure 7:

UVES spectra of two stars with nearly the same atmospheric parameters $T_{\rm eff}$, log g, and [Fe/H]. The spectrum of the low-$\alpha $ star HD 22879 ( $T_{\rm eff}$ = 5597 K, log g = 4.55, [Fe/H]  = -0.91, [$\alpha $/Fe] = 0.12) is shown with a red line and that of the high-$\alpha $ star HD 22879 ( $T_{\rm eff}$ = 5624 K, log g = 4.37, [Fe/H]  = -0.93, [$\alpha $/Fe] = 0.31) with a green line. The Fe lines have the same strength in the two spectra, but the Na, Mg, Si, and Ni lines are significantly weaker in the spectrum of the low-$\alpha $ star.

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\begin{figure}
\par\resizebox{8.8cm}{!}{\includegraphics{13877fig8.eps}}
\end{figure} Figure 8:

$W_{\rm LSR}$ versus $U_{\rm LSR}$ for stars with $\mbox{\rm [Fe/H]}> -1.4$. The same symbols as in Fig. 3 are used.

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Table 1:   UVES spectra acquired from the ESO/ST-ECF Science Archive.

Table 2:   Stars observed with the NOT/FIES spectrograph.

Table 3:   Atmospheric parameters, abundance ratios, and space velocities for stars with VLT/UVES spectra.

Table 4:   Atmospheric parameters, abundance ratios, and space velocities for stars with NOT/FIES spectra.

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