All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{7539fi1a.eps}\par\includegraphics[width=8cm,clip]{7539fi1b.eps}\end{figure}$ Figure 1: Fe abundances for BQ Ser with optimal atmospheric parameters. The parameters were set as $T_{\rm eff} = 6000$ K, $\log g = 2.0$ , $v_{\rm t} = 3.7$ km s^-1. Open circles denote Fe I lines, filled squares are Fe II lines. Top panel: iron abundance vs. excitation potential; bottom panel: abundance vs. EW.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7539fi2a.eps}\par\includegra... ...lip]{7539fi2b.eps}\par\includegraphics[width=8cm,clip]{7539fi2c.eps}\end{figure}$ Figure 2: The sensitivity of the calculated line abundances to the atmospheric parameters in the case of BQ Ser. The meaning of the symbols is the same as in Fig. 1. Top panel: the effect of setting $T_{\rm eff} = 5500$ K; middle panel: setting incorrect gravity ( $\log g = 3.0$ ); bottom panel: incorrect microturbulence ( $v_{\rm t} = 1.5$ km s^-1).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7539fi3.eps}\end{figure}$ Figure 3: The fitting of the H $\alpha$ profile of BQ Ser. The observed spectrum is shown by continuous curve, while the model spectrum is plotted as a dashed curve. The model shown here was computed assuming $T_{\rm eff} = 6000$ K and $\log g = 2.0$ . The fit was restricted to the wings of H $\alpha$ , since the core cannot be modeled under the LTE assumption.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{7539fi4.eps}\end{figure}$ Figure 4: Comparison of the observed spectrum of EW Scuti (dotted curve) with a model spectrum computed by ATLAS9/SYNTHE (solid curve) with the parameters in Table 2. The solar abundance pattern is scaled to the calculated abundance of EW Sct. Pulsation, as well as the instrumental broadening, has been taken into account (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7539fi5.eps}\end{figure}$ Figure 5: The period ratio - metal abundance relation. The parameters of the dotted line are given in Eq. (3). See text for the correction term on the vertical axis.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7539fi6.eps}\end{figure}$ Figure 6: Comparison of the [Fe/H] data of this paper with values from the literature (see Table 3 for tabulated data). The meaning of the symbols is as follows: filled circles: D'Cruz et al. (2000); open circles: Andrievsky et al. (1994); crosses: Andrievsky et al. (2002); asterisks: Lemasle et al. (2007). The reason for the discrepancy between our values and those by Andrievsky et al. (1994) is described in the text.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7539fi7.eps}\end{figure}$ Figure 7: Period - surface gravity relation from observations and theory. The dots are the averaged, corrected surface gravities of the program stars (see text). The dotted line is the relation predicted by simple pulsation theory (Eq. (4)), while the solid line is the result of a least-square fit (Eq. (5)). The theoretical relation is nicely recovered from the observations.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7539fi1a.eps}\par\includegraphics[width=8cm,clip]{7539fi1b.eps}\end{figure}$	Figure 1: Fe abundances for BQ Ser with optimal atmospheric parameters. The parameters were set as $T_{\rm eff} = 6000$ K, $\log g = 2.0$ , $v_{\rm t} = 3.7$ km s^-1. Open circles denote Fe I lines, filled squares are Fe II lines. Top panel: iron abundance vs. excitation potential; bottom panel: abundance vs. EW.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{7539fi2a.eps}\par\includegra... ...lip]{7539fi2b.eps}\par\includegraphics[width=8cm,clip]{7539fi2c.eps}\end{figure}$	Figure 2: The sensitivity of the calculated line abundances to the atmospheric parameters in the case of BQ Ser. The meaning of the symbols is the same as in Fig. 1. Top panel: the effect of setting $T_{\rm eff} = 5500$ K; middle panel: setting incorrect gravity ( $\log g = 3.0$ ); bottom panel: incorrect microturbulence ( $v_{\rm t} = 1.5$ km s^-1).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{7539fi3.eps}\end{figure}$	Figure 3: The fitting of the H $\alpha$ profile of BQ Ser. The observed spectrum is shown by continuous curve, while the model spectrum is plotted as a dashed curve. The model shown here was computed assuming $T_{\rm eff} = 6000$ K and $\log g = 2.0$ . The fit was restricted to the wings of H $\alpha$ , since the core cannot be modeled under the LTE assumption.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{7539fi4.eps}\end{figure}$	Figure 4: Comparison of the observed spectrum of EW Scuti (dotted curve) with a model spectrum computed by ATLAS9/SYNTHE (solid curve) with the parameters in Table 2. The solar abundance pattern is scaled to the calculated abundance of EW Sct. Pulsation, as well as the instrumental broadening, has been taken into account (see text).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{7539fi5.eps}\end{figure}$	Figure 5: The period ratio - metal abundance relation. The parameters of the dotted line are given in Eq. (3). See text for the correction term on the vertical axis.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{7539fi7.eps}\end{figure}$	Figure 7: Period - surface gravity relation from observations and theory. The dots are the averaged, corrected surface gravities of the program stars (see text). The dotted line is the relation predicted by simple pulsation theory (Eq. (4)), while the solid line is the result of a least-square fit (Eq. (5)). The theoretical relation is nicely recovered from the observations.
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