EDP Sciences
Free Access
Issue
A&A
Volume 508, Number 1, December II 2009
Page(s) L17 - L20
Section Letters
DOI https://doi.org/10.1051/0004-6361/200913038
Published online 12 November 2009

Online Material

\begin{figure}
\par\includegraphics[width=16.8cm,clip]{13038f1.ps}\end{figure} Figure 1:

Abundance ratios as a function of iron abundance for full sample of 64 stars. Dotted lines denote solar values.

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Table 1:   Derived stellar parameters, average abundance ratios [X/Fe] of volatile elements ( $T_{\rm C}<900$ K), and slope of the [X/Fe] vs. $T_{\rm C}$ relation for refractory elements ( $T_{\rm C}>900$ K). Errors in ${\rm [Fe/H]}$ correspond to the 1-$\sigma $ scatter of the line-by-line abundances.

Table 2:   Abundance ratios [X/Fe] for C, O, Na, Al, Si, and S. Errors correspond to the 1-$\sigma $scatter of the line-by-line abundances. A conservative value of 0.050 for the error was assumed when only one line was available.

Table 3:   Abundance ratios [X/Fe] for Ca, Sc, Ti, V, Cr, and Mn. Errors correspond to the 1-$\sigma $ scatter of the line-by-line abundances. A conservative value of 0.050 for the error was assumed when only one line was available.

Table 4:   Abundance ratios [X/Fe] for Ni, Cu, Zn, Y, Zr, and Ba. Errors correspond to the 1-$\sigma $ scatter of the line-by-line abundances. A conservative value of 0.050 for the error was assumed when only one line was available.


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