All Figures

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5211fig1.ps}\end{figure}$ Figure 1: Observed light variations of HD 239276 in the Strömgren v band during the years 1986 and 1987.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5211fig2.ps}\end{figure}$ Figure 2: Location of HD 239276 (star) in the H-R diagram together with HR 8799 (solid circle) and the sample of $\delta$ Sct-type pulsators from Rodríguez & Breger (2001). The observational $\gamma$ Dor edges (dashed lines) are from Handler & Shobbrook (2002).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.3cm,clip]{5211fig3.eps}\end{figure}$ Figure 3: Spectrum of HD 239276 = SAO 32177.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5211fig4.ps}\end{figure}$ Figure 4: Position of HD 239276 in the HR diagram with associated error bars and evolution tracks for Z=0.01 (solid lines) (Claret & Giménez 1995) and Z=0.02 (dotted lines) (Claret 1995).
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{5211fig5.ps}\end{figure}$ Figure 5: Amplitude spectra of C2 = HD 191096 and C3 = HD 186760 in the b band.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5211fig6.ps}\end{figure}$ Figure 6: Power spectra of HD 239276 in the combined vby band corresponding to the original data and residuals after removing different sets of simultaneously optimized peaks.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{5211fig7.ps}\end{figure}$ Figure 7: Phase diagrams for f₁=2.1066 cd^-1 ( top), f₂=1.8694 cd^-1 ( middle) and f₃=2.2124 cd^-1 ( bottom). In each panel, the data have been prewhitened to remove the other two frequencies.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5211fig8.eps}\end{figure}$ Figure 8: Strömgren photometric amplitude ratios obtained for different values of $f_{\rm T}$ (0.15, 0.25, 0.5, 5), $\psi _{\rm T}=-35\hbox {$^\circ $ }$ , $\log T_{\rm e}=3.85$ , $\log g=4.14$ . The lines are the theoretical predictions for different l and the error bars represent the observations for the frequencies f₁, f₂ and f₃.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5211fig9.eps}\end{figure}$ Figure 9: Position of HD 239276 in the HR diagram with associated error bars and evolution tracks for Z=0.01 (solid lines) and Z=0.02 (dotted lines) using the CLES code. Some of our best models for Z=0.01 ( $\times$ ) and Z=0.02 (+) are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5211fig10.eps}\end{figure}$ Figure 10: Strömgren photometric amplitude ratios obtained with our TDC treatment, for a model with $M=1.5~ M_{\odot}$ and Z=0.02 in the centre of the photometric error box ( $\log T_{\rm e}=3.8508$ ). The lines are the theoretical predictions for l=1 (solid) and l=2 (dashed) modes with frequencies closest to the observed ones. The error bars represent the observations for the frequencies f₁, f₂ and f₃.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5211fig11.eps}\end{figure}$ Figure 11: Strömgren photometric amplitude ratios obtained with our TDC treatment, model with $M=1.3~ M_{\odot}$ , Z=0.01, $\log T_{\rm e}=3.8569$ , $\alpha =2$ . The lines are the theoretical predictions (e.g. f₁ th l=1 means theoretical result for the l=1 mode with frequency closest to f₁). The error bars represent the observations for the frequencies f₁, f₂ and f₃.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5211fig12.eps}\end{figure}$ Figure 12: Theoretical Brunt-Väisälä frequency integral as a function of the effective temperature for representative models with masses in the range of M=1.2-1.6 ${M_\odot }$ and different metallicities [Me/H] = 0.0, -0.2, -0.4, and -0.6. Shaded areas represent uncertainty ( ${\cal I}_{{\rm obs}}$ , ${T_{{\rm eff}}}$ ) boxes for the solutions given in Table 11.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5211fig1.ps}\end{figure}$	Figure 1: Observed light variations of HD 239276 in the Strömgren v band during the years 1986 and 1987.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5211fig2.ps}\end{figure}$	Figure 2: Location of HD 239276 (star) in the H-R diagram together with HR 8799 (solid circle) and the sample of $\delta$ Sct-type pulsators from Rodríguez & Breger (2001). The observational $\gamma$ Dor edges (dashed lines) are from Handler & Shobbrook (2002).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.3cm,clip]{5211fig3.eps}\end{figure}$	Figure 3: Spectrum of HD 239276 = SAO 32177.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5211fig4.ps}\end{figure}$	Figure 4: Position of HD 239276 in the HR diagram with associated error bars and evolution tracks for Z=0.01 (solid lines) (Claret & Giménez 1995) and Z=0.02 (dotted lines) (Claret 1995).
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$\begin{figure} \par\includegraphics[width=6.4cm,clip]{5211fig5.ps}\end{figure}$	Figure 5: Amplitude spectra of C2 = HD 191096 and C3 = HD 186760 in the b band.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5211fig6.ps}\end{figure}$	Figure 6: Power spectra of HD 239276 in the combined vby band corresponding to the original data and residuals after removing different sets of simultaneously optimized peaks.
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{5211fig7.ps}\end{figure}$	Figure 7: Phase diagrams for f₁=2.1066 cd^-1 ( top), f₂=1.8694 cd^-1 ( middle) and f₃=2.2124 cd^-1 ( bottom). In each panel, the data have been prewhitened to remove the other two frequencies.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{5211fig8.eps}\end{figure}$	Figure 8: Strömgren photometric amplitude ratios obtained for different values of $f_{\rm T}$ (0.15, 0.25, 0.5, 5), $\psi _{\rm T}=-35\hbox {$^\circ $ }$ , $\log T_{\rm e}=3.85$ , $\log g=4.14$ . The lines are the theoretical predictions for different l and the error bars represent the observations for the frequencies f₁, f₂ and f₃.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{5211fig9.eps}\end{figure}$	Figure 9: Position of HD 239276 in the HR diagram with associated error bars and evolution tracks for Z=0.01 (solid lines) and Z=0.02 (dotted lines) using the CLES code. Some of our best models for Z=0.01 ( $\times$ ) and Z=0.02 (+) are also shown.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{5211fig11.eps}\end{figure}$	Figure 11: Strömgren photometric amplitude ratios obtained with our TDC treatment, model with $M=1.3~ M_{\odot}$ , Z=0.01, $\log T_{\rm e}=3.8569$ , $\alpha =2$ . The lines are the theoretical predictions (e.g. f₁ th l=1 means theoretical result for the l=1 mode with frequency closest to f₁). The error bars represent the observations for the frequencies f₁, f₂ and f₃.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5211fig12.eps}\end{figure}$	Figure 12: Theoretical Brunt-Väisälä frequency integral as a function of the effective temperature for representative models with masses in the range of M=1.2-1.6 ${M_\odot }$ and different metallicities [Me/H] = 0.0, -0.2, -0.4, and -0.6. Shaded areas represent uncertainty ( ${\cal I}_{{\rm obs}}$ , ${T_{{\rm eff}}}$ ) boxes for the solutions given in Table 11.
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