All Figures

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{2877_f1.eps} \end{figure}$ Figure 1: A comparison between observations (thick dashed line) and synthetic spectrum (single line) in the region of two Fe II lines at 6147.74 Å (blend of lines characterized by small effective Landé factors) and 6149.26 Å (marginally blended line). The synthetic spectrum calculations were performed with a stratified Fe abundance and with a magnetic field of 5.7 kG. Note a resolved magnetic splitting of the second line.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{2877_f2.eps} \end{figure}$ Figure 2: Comparison between observed and calculated spectra in the region of the Fei line at 6336.824 Å ( $g_{\rm eff}=2.00$ ). Thick dashed line - observations. Dash-dotted line - the feature calculated without magnetic field. Single line - synthetic spectrum with a mean magnetic field modulus of 5.7 kG.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2877_vgl.eps} \end{figure}$ Figure 3: The spectral region around 6148 Å is shown for the stars of Table 1. Single line - synthetic spectrum; double line - observed spectrum. For the first star (HD 208217) two calculations are shown: the single line corresponds to $\vert\vec{B}\vert=7.3$ kG, the dashed line to $\vert\vec{B}\vert=6.5$ kG. A spectrum of the star 10 Aql (HD 176232), where no Zeeman splitting can be seen at our resolution, is plotted at the bottom of the plot.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{2877_f2.eps} \end{figure}$	Figure 2: Comparison between observed and calculated spectra in the region of the Fei line at 6336.824 Å ( $g_{\rm eff}=2.00$ ). Thick dashed line - observations. Dash-dotted line - the feature calculated without magnetic field. Single line - synthetic spectrum with a mean magnetic field modulus of 5.7 kG.
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