All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{4333f1.eps} \end{figure}$ Figure 1: Spectral line evolution of $\beta$ Dor together with the modelled bi-Gaussian (bold). Line asymmetry is clear. The vertical line at the top corresponds to a differential flux of 0.3. Pulsation phases are given on the right of each profile.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4333f2.eps} \end{figure}$ Figure 2: $\beta$ Dor radial velocities obtained with different method: $RV_{\rm m}$ (points), $RV_{\rm g}$ (squares), and $RV_{\rm c}$ (crosses). Statistical uncertainties at $\pm$ $1 \sigma$ are indicated but too small to be visualized. We can therefore see the impact of the choice of the method in the case of a very asymmetric line (Fig. 1).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4333f3.eps} \end{figure}$ Figure 3: Radial velocity curves ( $RV_{\rm m}$ ). Curves have been arbitrarily shifted vertically. The horizontal lines are the zero velocity in the stellar rest frame. Largest velocities are for receding motion.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4333f4.eps} \end{figure}$ Figure 4: FWHM versus phase for all stars. Curves have been arbitrarily shifted vertically. The horizontal lines correspond to a zero FWHM. Note the particular case of RS Pup, which may present the signature of an important compression or shock wave. RS Pup has the longest period of our sample.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4333f5.eps} \end{figure}$ Figure 5: FeI 6056.005 Å spectral line evolution of RS Pup. The vertical line at the top corresponds to a differential flux of 0.2. We note the broadening of the line at $\phi =0.83$ which could be the signature of a strong velocity gradient (compression or shock wave).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4333f6.eps}\end{figure}$ Figure 6: Asymmetry against phase for all stars. Curves have been arbitrarily shifted vertically. The horizontal lines correspond to an asymmetry of zero.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4333f7.eps} \end{figure}$ Figure 7: Difference between the radial velocity obtained with the line minimum and the Gaussian fit methods as a function of the asymmetry in the case of $\ell$ Car and RS Pup. Statistical uncertainties are provided for each point. Arrows indicate the direction and the origin $\phi =0$ of the curves. These relations are not linear and certainly affected by star characteristics (rotation, FWHM, velocity gradients...).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4333f8.eps} \end{figure}$ Figure 8: The weighting or the synthetic spectral line profile in different cases, considering a) the pulsation velocity, b) the limb-darkening, c) the rotation and, d) an intrinsic width for the line ( $\sigma _{\rm C}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4333f9.eps} \end{figure}$ Figure 9: The projection factor corresponding to the centroid velocity ( $p_{\rm c}$ ) as a function of the limb-darkening parameter (u_V). Dots are the results from the toy model and the solid line corresponds to the linear approximation ( $\chi ^2 \simeq 10^{-5}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{4333f10.eps} \end{figure}$ Figure 10: Results of the geometric model of pulsating star. a), b) The radial velocity-asymmetry correlation curves for different $\sigma _{\rm C}$ , with no rotation and no limb-darkening (uniform disk). Points, squares and crosses correspond respectively to the $RV_{\rm m}$ , $RV_{\rm g}$ and $RV_{\rm c}$ radial velocities. For clarity $RV_{\rm g}$ and $RV_{\rm m}$ are represented only for $\sigma _{\rm C}=0.1$ Å. The solid lines are the interpolated curves using a cubic spline function. The corresponding projection factors are represented on diagram b). c), d) Same plots but for different values of the rotation. The $\sigma _{\rm C}$ and the limb-darkening are respectively of 0.25 Å and 0.7. These RV-A plot are used to interpret HARPS observations.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{4333f11.eps} \end{figure}$ Figure 11: Radial velocity ( $RV_{\rm c}$ ) - asymmetry correlation curves for R TrA, S Cru, Y Sgr, $\beta$ Dor, $\zeta$ Gem, Y Oph, RZ Vel and $\ell$ Car. Dots and bold curves correspond respectively to observations and models. The statistical uncertainties are indicated. Note that RV-A plot deduced from the model have been shifted in asymmetry. The small plot on each diagram correspond to the comparison of the observational (dots) and model (bold curve) FWHM.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4333f12.eps}\end{figure}$ Figure 12: Same as Fig. 11 but for RS Pup. RS Pup seems to be a non-rotating star as requested by the shape of its RV-A curve. Note also atypical points in observational RV-A plot, which can certainly be interpreted through the presence of a strong compression or shock wave in the stellar atmosphere.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4333f13.eps} \end{figure}$ Figure 13: Difference of the Observational and Computed asymmetry curves (O-C curves) for each stars. Curves are arbitrarily shifted. The horizontal dotted lines corresponds to a zero asymmetry for each star.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4333f14.eps}\end{figure}$ Figure 14: a) Average values of the observational (black circles) and computed (open squares) asymmetry curves, together with the $\gamma _{\rm O{-}C}$ (filled squares) average values as a function of the pulsation period. b) Dependence of the projected rotation velocity with the pulsation period.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4333f1.eps} \end{figure}$	Figure 1: Spectral line evolution of $\beta$ Dor together with the modelled bi-Gaussian (bold). Line asymmetry is clear. The vertical line at the top corresponds to a differential flux of 0.3. Pulsation phases are given on the right of each profile.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4333f2.eps} \end{figure}$	Figure 2: $\beta$ Dor radial velocities obtained with different method: $RV_{\rm m}$ (points), $RV_{\rm g}$ (squares), and $RV_{\rm c}$ (crosses). Statistical uncertainties at $\pm$ $1 \sigma$ are indicated but too small to be visualized. We can therefore see the impact of the choice of the method in the case of a very asymmetric line (Fig. 1).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4333f3.eps} \end{figure}$	Figure 3: Radial velocity curves ( $RV_{\rm m}$ ). Curves have been arbitrarily shifted vertically. The horizontal lines are the zero velocity in the stellar rest frame. Largest velocities are for receding motion.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4333f4.eps} \end{figure}$	Figure 4: FWHM versus phase for all stars. Curves have been arbitrarily shifted vertically. The horizontal lines correspond to a zero FWHM. Note the particular case of RS Pup, which may present the signature of an important compression or shock wave. RS Pup has the longest period of our sample.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4333f5.eps} \end{figure}$	Figure 5: FeI 6056.005 Å spectral line evolution of RS Pup. The vertical line at the top corresponds to a differential flux of 0.2. We note the broadening of the line at $\phi =0.83$ which could be the signature of a strong velocity gradient (compression or shock wave).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4333f6.eps}\end{figure}$	Figure 6: Asymmetry against phase for all stars. Curves have been arbitrarily shifted vertically. The horizontal lines correspond to an asymmetry of zero.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4333f8.eps} \end{figure}$	Figure 8: The weighting or the synthetic spectral line profile in different cases, considering a) the pulsation velocity, b) the limb-darkening, c) the rotation and, d) an intrinsic width for the line ( $\sigma _{\rm C}$ ).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4333f9.eps} \end{figure}$	Figure 9: The projection factor corresponding to the centroid velocity ( $p_{\rm c}$ ) as a function of the limb-darkening parameter (u_V). Dots are the results from the toy model and the solid line corresponds to the linear approximation ( $\chi ^2 \simeq 10^{-5}$ ).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4333f12.eps}\end{figure}$	Figure 12: Same as Fig. 11 but for RS Pup. RS Pup seems to be a non-rotating star as requested by the shape of its RV-A curve. Note also atypical points in observational RV-A plot, which can certainly be interpreted through the presence of a strong compression or shock wave in the stellar atmosphere.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4333f13.eps} \end{figure}$	Figure 13: Difference of the Observational and Computed asymmetry curves (O-C curves) for each stars. Curves are arbitrarily shifted. The horizontal dotted lines corresponds to a zero asymmetry for each star.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4333f14.eps}\end{figure}$	Figure 14: a) Average values of the observational (black circles) and computed (open squares) asymmetry curves, together with the $\gamma _{\rm O{-}C}$ (filled squares) average values as a function of the pulsation period. b) Dependence of the projected rotation velocity with the pulsation period.
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