All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{4164f1.ps} \end{figure}$ Figure 1: Light curves for the 2002 B dataset (Loiano). Note that $\delta B=B_{\rm VAR}-B_{\rm COMP}$ . The solid line represents the fit to the data including the six significant frequencies found for this dataset (see Sect. 3).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4164f2.ps}\hspace*{4mm} \includegraphics[width=8.5cm,clip]{4164f3.ps} \end{figure}$ Figure 2: Left panels: light curves for the 2003 V dataset. Note that $\delta V=V_{\rm VAR}-V_{\rm COMP}$ . Right panels: light curves for the 2003 B dataset. Note that $\delta B=B_{\rm VAR}-B_{\rm COMP}$ .
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In the text

$\begin{figure} \includegraphics[width=7cm,clip]{4164f4.ps}\end{figure}$ Figure 3: Data collected in Loiano with the TTCP (V filter) during Nov./Dec. 2003 (dots). The solid line show the fit to the data with 9 frequencies obtained from the period analysis (see Sect. 3).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4164f5.ps} \end{figure}$ Figure 4: Spectral window in amplitude for the three datasets analysed in this paper (see labels in the figure). Note in particular that the 1 c/d alias is reduced to about 50% for the 2003 V dataset.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4164f6.ps} \end{figure}$ Figure 5: Frequency analysis for the 2002 B dataset. The solid, dashed and dotted lines show respectively the 99.9%, 99% and 90% significant levels. In each panel, one peak (i.e. the labelled frequency) is selected and removed from the time series and a new spectrum is obtained. The last panel shows the periodogram after the prewithening with all the significant frequencies.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4164f7.ps} \end{figure}$ Figure 6: As in Fig. 5 but for the 2003 B dataset.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{4164f8.ps} \end{figure}$ Figure 7: As in Fig. 5 but for the 2003 V dataset.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4164f9.ps} \end{figure}$ Figure 8: Position in the HR diagram of the best-fit radial pulsation model. The shaded region is the predicted instability strip by Marconi & Palla (1998) with solar chemical composition (Z=0.02, Y=0.28). Solid lines are the PMS evolutionary tracks computed for the labelled stellar masses with the FRANEC stellar evolution code (Chieffi & Straniero 1989; Castellani et al. 1999). The dashed lines represent the 1.77 $M_{\odot }$ PMS track with solar chemical composition.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4164f10.ps} \end{figure}$ Figure 9: Position of the instability strip for the first three radial modes at Z=0.008 (dashed lines) compared with the one at solar metallicity (solid lines). The long dashed line represent the birthline by Palla & Stahler (1993).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4164f11.ps} \end{figure}$ Figure 10: Best fit radial pulsation model for Z=0.008 in the HR diagram (filled triangle) as compared with the spectroscopic measurement by Miroshnichenko et al. (2001). The corresponding PMS evolutionary track and instability strip are overplotted. The track for 1.77 $M_{\odot }$ , Z=0.008 is shown for comparison with Fig. 8.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4164f1.ps} \end{figure}$	Figure 1: Light curves for the 2002 B dataset (Loiano). Note that $\delta B=B_{\rm VAR}-B_{\rm COMP}$ . The solid line represents the fit to the data including the six significant frequencies found for this dataset (see Sect. 3).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4164f2.ps}\hspace*{4mm} \includegraphics[width=8.5cm,clip]{4164f3.ps} \end{figure}$	Figure 2: Left panels: light curves for the 2003 V dataset. Note that $\delta V=V_{\rm VAR}-V_{\rm COMP}$ . Right panels: light curves for the 2003 B dataset. Note that $\delta B=B_{\rm VAR}-B_{\rm COMP}$ .
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$\begin{figure} \includegraphics[width=7cm,clip]{4164f4.ps}\end{figure}$	Figure 3: Data collected in Loiano with the TTCP (V filter) during Nov./Dec. 2003 (dots). The solid line show the fit to the data with 9 frequencies obtained from the period analysis (see Sect. 3).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4164f5.ps} \end{figure}$	Figure 4: Spectral window in amplitude for the three datasets analysed in this paper (see labels in the figure). Note in particular that the 1 c/d alias is reduced to about 50% for the 2003 V dataset.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4164f6.ps} \end{figure}$	Figure 5: Frequency analysis for the 2002 B dataset. The solid, dashed and dotted lines show respectively the 99.9%, 99% and 90% significant levels. In each panel, one peak (i.e. the labelled frequency) is selected and removed from the time series and a new spectrum is obtained. The last panel shows the periodogram after the prewithening with all the significant frequencies.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4164f7.ps} \end{figure}$	Figure 6: As in Fig. 5 but for the 2003 B dataset.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{4164f8.ps} \end{figure}$	Figure 7: As in Fig. 5 but for the 2003 V dataset.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{4164f10.ps} \end{figure}$	Figure 9: Position of the instability strip for the first three radial modes at Z=0.008 (dashed lines) compared with the one at solar metallicity (solid lines). The long dashed line represent the birthline by Palla & Stahler (1993).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{4164f11.ps} \end{figure}$	Figure 10: Best fit radial pulsation model for Z=0.008 in the HR diagram (filled triangle) as compared with the spectroscopic measurement by Miroshnichenko et al. (2001). The corresponding PMS evolutionary track and instability strip are overplotted. The track for 1.77 $M_{\odot }$ , Z=0.008 is shown for comparison with Fig. 8.
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