Online Material

Table 3: Error sources for the abundances of the chemical elements in HD 49933.

Table 4: Comparison between the line abundances obtained for a set of Fe I lines calculated from equivalent widths measured with direct integration and a Gaussian approximation.

$\begin{figure} \par\includegraphics[width=8cm,clip]{11871f4.eps} \end{figure}$	Figure 4: Samples of the first spectrum obtained February 11th, the last obtained February 13th and the final co-added spectrum (from top to bottom) around the strong Fe II line at $\sim$ 5018 Å.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{11871f5.eps} \end{figure}$	Figure 5: ionFei individual line abundances vs. equivalent widths. Abundances are derived for the preferred model parameters, $T_{{\rm eff}}$ = 6500 K, $\ensuremath{\log g}$ = 4.00, $\upsilon _{{\rm mic}}$ = 1.5 ${\rm km~s}^{-1}$ .
Open with DEXTER