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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1419f1.ps}\par\end{figure}$ Figure 1: Difference between the theoretical radial velocity curves measured by the profile minimum method ( $v_{\rm rad\vert min}$ ) and the Gaussian fitting method ( $v_{\rm rad\vert gauss}$ ). The small difference induces a bias in the determination of the p-factor. The horizontal line is the zero velocity in the stellar rest frame.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1419f2.ps}\par\end{figure}$ Figure 2: Pulsation velocities vs. phase. The dashed curve shows the velocity of the photospheric layer ( $\tau =2/3$ in the continuum), the dot-dashed curve the velocity of the layer corresponding to $\tau =2/3$ in the spectral center of the line and the dotted curve the gas velocity corresponding to $\tau =2/3$ in the line. The horizontal line is the zero velocity in the stellar rest frame.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1419f3.ps}\par\end{figure}$ Figure 3: Radial velocity curve deduced from the theoretical line profiles by the Gaussian method together with a) the gas velocity corresponding to $\tau =2/3$ in the line forming region according to Eq. (1), b) the $\tau =2/3$ "optical layer'' velocity according to Eq. (2), c) the velocity of the photospheric layer ( $\tau =2/3$ in the continuum, see Eq. (3)).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1419f4.ps}\par\end{figure}$ Figure 4: The quantity $v_{\rm puls}-1.35*v_{\rm rad}$ versus the phase in the case of Fig. 3a: $v_{\rm puls}$ is the gas velocity corresponding to $\tau =2/3$ in the line formation region according to Eq. (1), and $v_{\rm rad}$ is the radial velocity curve deduced from the theoretical line profiles by the Gaussian method. p=1.35 is the optimum value obtained from the estimator 1, as described in Sect. 4.2
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1419f5.ps}\par\end{figure}$ Figure 5: Simulated angular diameter points deduced from Eq. (9) with $R_{\rm puls_{(ic)}}=R(\tau _{\rm c}=2/3)$ . Each point is shown with its arbitrary theoretical error bar of 0.01 mas. This curve simulates interferometric observations used in the IBW method.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1419f1.ps}\par\end{figure}$	Figure 1: Difference between the theoretical radial velocity curves measured by the profile minimum method ( $v_{\rm rad\vert min}$ ) and the Gaussian fitting method ( $v_{\rm rad\vert gauss}$ ). The small difference induces a bias in the determination of the p-factor. The horizontal line is the zero velocity in the stellar rest frame.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1419f3.ps}\par\end{figure}$	Figure 3: Radial velocity curve deduced from the theoretical line profiles by the Gaussian method together with a) the gas velocity corresponding to $\tau =2/3$ in the line forming region according to Eq. (1), b) the $\tau =2/3$ "optical layer'' velocity according to Eq. (2), c) the velocity of the photospheric layer ( $\tau =2/3$ in the continuum, see Eq. (3)).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1419f5.ps}\par\end{figure}$	Figure 5: Simulated angular diameter points deduced from Eq. (9) with $R_{\rm puls_{(ic)}}=R(\tau _{\rm c}=2/3)$ . Each point is shown with its arbitrary theoretical error bar of 0.01 mas. This curve simulates interferometric observations used in the IBW method.
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