All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5574fig1.eps} \end{figure}$ Figure 1: Normalisation of the spectrum of HD 225125: a) Merged spectrum with incomplete removal of the instrumental signature/response; b) Corrected spectrum and continuum placement (broken line); c) Normalized observed spectrum (black line) compared to the synthetic one (red crosses).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5574fig2.eps} \end{figure}$ Figure 2: The CCF of HD 217860 shown for 3 consecutive exposures.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5574fig3.eps} \end{figure}$ Figure 3: HD 217860 - Comparison between observed (dotted black line) and synthetic spectra (full red line).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{5574fig4.eps} \end{figure}$ Figure 4: Relation between the full base width of the cross-correlation function (WCCF) and the V sin i parameter. The linear least squares relation between the measurements made on single-lined objects (filled circles) is represented by the full line. V sin i values obtained for components member of multiple systems are also plotted (unfilled circles).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip=]{5574fig5a.eps}\par\includ... ...574fig5b.eps}\par\includegraphics[width=7.7cm,clip=]{5574fig5c.eps} \end{figure}$ Figure 5: CCD light curves (filter V or B) obtained for seven targets having an obviously variable cross-correlation function. Magnitude differences (i.e. target minus comparison star and comparison minus check star) are reported as a function of the Julian date. Arbitrary shifts were applied to present the light curves of the target and comparison data in a single panel. In the case of HD 81995, there was no suitable check star available in the field. Small thick lines show the corresponding standard deviations of the reference data obtained under the best conditions.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{5574fig6.eps} \end{figure}$ Figure 6: Successive frequency searches and spectral window of the Fourier analysis (Set All - filter B).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5574fig8.eps} \end{figure}$ Figure 8: Theoretically predicted versus observed frequencies for F1 and F2 in the range 12-20 c/d. Vertical lines represent the observed frequency values.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=270,width=8.5cm,clip=]{5574fig9a... ...} \includegraphics[angle=270,width=8.5cm,clip=]{5574fig9b.eps} } \end{figure}$ Figure 9: Observed and theoretical values in an (amplitude ratio vs. phase difference) diagram for the $\ell$ = 0 (circles), 1 (squares), 2 (triangles), and 3 (stars) modes whose frequency is the closest to the observed frequencies F1 ( left panel) and F2 ( right panel) for the 11 selected models of mass 1.80, 1.85, and 1.90 $M_{\odot }$ . The amplitude ratios and the phase differences corresponding to the extra model #738 of mass 1.80 $M_{\odot }$ correspond to the filled symbols. One $\sigma$ -error boxes are plotted around the observed values.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip=]{5574fig10.eps} \end{figure}$ Figure 10: Radial velocity phase diagram of HD 11190. Full and dashed lines represent the orbital solution assuming a circular orbit. Filled symbols correspond to data collected at NAO Rozhen, unfilled ones to data collected at OHP.
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In the text

$\begin{figure} \includegraphics[width=7.7cm,clip=]{5574fig11.eps} \end{figure}$ Figure 11: Comparison between observed (black line) and synthetic spectra (red line) in the case of the SB2 system HD 11190 at HJD = 2 453 343.4033. The presence of the two components was taken into account in the fit. The significant disagreement between observations and model indicates that both components are Am stars.
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In the text

$\begin{figure} \includegraphics[width=8.5cm,clip=]{5574fig12.eps} \end{figure}$ Figure 12: Location of the targets in the H-R diagram. Open circles are the stars we identified as short-term variables of $\delta$ Scuti type. Squares stand for the components of the SB2 binary HD 11190. Other SB2 systems with inaccurate parameters were not plotted here. Broken lines are the limits of the Cepheid instability strip as computed by Dupret et al. (2005)
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{5574fig7.eps} \end{figure}$ Figure 7: Successive frequency searches and spectral window of the Fourier analysis (Set All - filter V).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5574fig1.eps} \end{figure}$	Figure 1: Normalisation of the spectrum of HD 225125: a) Merged spectrum with incomplete removal of the instrumental signature/response; b) Corrected spectrum and continuum placement (broken line); c) Normalized observed spectrum (black line) compared to the synthetic one (red crosses).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5574fig2.eps} \end{figure}$	Figure 2: The CCF of HD 217860 shown for 3 consecutive exposures.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5574fig3.eps} \end{figure}$	Figure 3: HD 217860 - Comparison between observed (dotted black line) and synthetic spectra (full red line).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{5574fig4.eps} \end{figure}$	Figure 4: Relation between the full base width of the cross-correlation function (WCCF) and the V sin i parameter. The linear least squares relation between the measurements made on single-lined objects (filled circles) is represented by the full line. V sin i values obtained for components member of multiple systems are also plotted (unfilled circles).
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$\begin{figure} \par\includegraphics[width=17cm,clip]{5574fig6.eps} \end{figure}$	Figure 6: Successive frequency searches and spectral window of the Fourier analysis (Set All - filter B).
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5574fig8.eps} \end{figure}$	Figure 8: Theoretically predicted versus observed frequencies for F1 and F2 in the range 12-20 c/d. Vertical lines represent the observed frequency values.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip=]{5574fig10.eps} \end{figure}$	Figure 10: Radial velocity phase diagram of HD 11190. Full and dashed lines represent the orbital solution assuming a circular orbit. Filled symbols correspond to data collected at NAO Rozhen, unfilled ones to data collected at OHP.
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$\begin{figure} \includegraphics[width=7.7cm,clip=]{5574fig11.eps} \end{figure}$	Figure 11: Comparison between observed (black line) and synthetic spectra (red line) in the case of the SB2 system HD 11190 at HJD = 2 453 343.4033. The presence of the two components was taken into account in the fit. The significant disagreement between observations and model indicates that both components are Am stars.
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$\begin{figure} \includegraphics[width=8.5cm,clip=]{5574fig12.eps} \end{figure}$	Figure 12: Location of the targets in the H-R diagram. Open circles are the stars we identified as short-term variables of $\delta$ Scuti type. Squares stand for the components of the SB2 binary HD 11190. Other SB2 systems with inaccurate parameters were not plotted here. Broken lines are the limits of the Cepheid instability strip as computed by Dupret et al. (2005)
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$\begin{figure} \par\includegraphics[width=17cm,clip]{5574fig7.eps} \end{figure}$	Figure 7: Successive frequency searches and spectral window of the Fourier analysis (Set All - filter V).
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