Volume 506, Number 1, October IV 2009
The CoRoT space mission: early results
Page(s) 203 - 211
Section Stellar atmospheres
Published online 15 June 2009

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.

\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.

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\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  ${\rm km~s}^{-1}$.

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