Online Material

$\begin{figure} \par\includegraphics[width=12cm,clip]{11561fig8.ps}\end{figure}$	Figure 8: Same as Fig. 2, but also for H $\gamma$ and H $\alpha$ .
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$\begin{figure} \par\includegraphics[width=12cm,clip]{11561fig9.ps}\end{figure}$	Figure 9: Same as Fig. 8, but for HD 145788.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{11561fig10.ps}\end{figure}$	Figure 10: Same as Fig. 8, but for $\pi$ Cet.
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$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{11561fig11.ps}\end{figure}$

Figure 11:

Comparison between LLMODELS theoretical fluxes calculated with the fundamental parameters and abundances derived for HD 145788, taking into account a reddening of E(B-V)=0.20 (full black line) and without taking into account reddening (dashed black line), with IUE calibrated fluxes (full blue line), Johnson UBV photometry (green squares), Geneva photometry (red circles) and 2MASS photmetry (violet triangles). The model fluxes were convolved to have approximately the same spectral resolution of the IUE fluxes ( R $\sim$ 900).

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$\begin{figure} \par\includegraphics[width=12cm,clip]{11561fig12.ps}\end{figure}$	Figure 12: Comparison between the observed spectrum of the He I line at $\lambda \sim 4471$ Å for 21 Peg (black thick line) and three synthetic profiles calculated with three different $T_{{\rm eff}}$ for the model atmosphere: 10 200 K (green line), the adopted 10 400 K (red line) and 10 600 K (blue line).
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Table 6: Comparison of the derived abundances with previous determinations for 21 Peg.

Table 7: Comparison of the derived abundances with previous dterminations for $\pi$ Cet.

Table 8: A collection of the experimental and theoretical transition probabilities and Stark widths for the observed Si II lines. Errors are given in parenthesis.