EDP Sciences
Free Access
Issue
A&A
Volume 510, February 2010
Article Number A22
Number of page(s) 21
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361/200913120
Published online 02 February 2010

Online Material

Table 5:   List of log gf values for the Si II-IV lines considered in this study (from Atomic Line List v2.05). For the O II lines we refer to Simón-Díaz et al. (2006).

Table 6:   Results from the abundance analysis of HD 36512 (B0 V).

Table 7:   Results from the abundance analysis of HD 37020 (B0.5 V).

Table 8:   Results from the abundance analysis of HD 36960 (B0.5 V).

Table 9:   Results from the abundance analysis of HD 37042 (B0.7 V).

Table 10:   Results from the abundance analysis of HD 36591 (B1 V).

Table 11:   Results from the abundance analysis of HD 36959 (B1 V).

Table 12:   Results from the abundance analysis of HD 37744 (B1.5 V).

Table 13:   Results from the abundance analysis of HD 35299 (B1.5 V).

Table 14:   Results from the abundance analysis of HD 36285 (B2 V).

Table 15:   Results from the abundance analysis of HD 35039 (B2 V).

Table 16:   Results from the abundance analysis of HD 36629 (B2 V).

Table 17:   Results from the abundance analysis of HD 36430 (B2 V).

Table 18:   Results from the abundance analysis of HD 35912 (B2 V).

\begin{figure}
\par\includegraphics[angle=180,scale=0.85]{13120f8a.eps}
\end{figure} Figure 8:

The complete atlas of FIES@ NOT spectra (part 1 of 3). The Si II-IV and O II lines used for the abundance analysis are indicated as solid and dashed vertical lines, respectively.

Open with DEXTER

\begin{figure}
\par\includegraphics[angle=180,scale=0.85]{13120f8b.eps}
\end{figure} Figure 8:

continued.

Open with DEXTER

\begin{figure}
\par\includegraphics[angle=180,scale=0.85]{13120f8c.eps}
\end{figure} Figure 8:

continued.

Open with DEXTER

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