$\begin{figure} \par\resizebox{8.8cm}{!} {\includegraphics[angle=-90,clip]{3947.f1}} \end{figure}$ Figure 1: Derived values of q₂/q₁ for a rigidly rotating F0-type star with $\beta = 0.08$ . Different symbols indicate inclination angles as indicated in the figure. The value of q₂/q₁ is determined by $v_{\rm e}$ independent of the values of i and $v~\sin{i}$ . The slope is well approximated by the second order polynomial shown as a solid line.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7.8cm,clip]{3947.f2a}\... ...ace{1cm} \includegraphics[angle=-90,width=7.8cm,clip]{3947.f2d} } \end{figure}$ Figure 2: Derived values of q₂/q₁ vs. equatorial velocity $v_{\rm e}$ for four different stellar models (B0, A0, F0 and G0). For each model different values of the gravity darkening parameter $\beta$ (0.0, 0.08 and 0.25) are indicated using different symbols. The dependence of q₂/q₁ on $v_{\rm e}$ differs for the different cases but is monotonic in $\beta$ and $v_{\rm e}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{3947.f3a}\hspace... ...space*{1cm} \includegraphics[angle=-90,width=7.8cm,clip]{3947.f3d} \end{figure}$ Figure 3: Stars with measured values of $v~\sin{i}$ and q₂/q₁ are seen under an inclination angle i. In the four panels (B0, A0, F0 and G0-type stars) the approximated dependence of i on the ratio q₂/q₁ is shown for values of $v~\sin{i} = 50, 100, 200$ and 300 km s^-1 (solid lines, top to bottom as indicated in the upper left panel). The dashed line marks the lowest ratio of q₂/q₁ consistent with slow rotation and extreme limb darkening, no values of q₂/q₁ > 1.75 are expected.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{3947.f4a}\hspace... ...space*{1cm} \includegraphics[angle=-90,width=7.8cm,clip]{3947.f4d} \end{figure}$ Figure 4: Values of $v~\sin{i}$ as measured from the first zero of the Fourier transformed broadening profiles plotted vs. the real values given as input to the models. The four panels show cases of B0, A0, F0 and G0-type stars, the value of the gravity darkening parameters $\beta$ are chosen according to Claret (1998). In each panel series for four different inclination angles ( $i=90^{\circ }, 70^{\circ }, 50^{\circ }$ and $30^{\circ }$ ) are differentiated, the respective values are connected by solid lines. Dotted lines mark the identity between real and measured values.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!} {\includegraphics[angle=-90,clip]{3947.f1}} \end{figure}$	Figure 1: Derived values of q₂/q₁ for a rigidly rotating F0-type star with $\beta = 0.08$ . Different symbols indicate inclination angles as indicated in the figure. The value of q₂/q₁ is determined by $v_{\rm e}$ independent of the values of i and $v~\sin{i}$ . The slope is well approximated by the second order polynomial shown as a solid line.
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$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7.8cm,clip]{3947.f2a}\... ...ace{1cm} \includegraphics[angle=-90,width=7.8cm,clip]{3947.f2d} } \end{figure}$	Figure 2: Derived values of q₂/q₁ vs. equatorial velocity $v_{\rm e}$ for four different stellar models (B0, A0, F0 and G0). For each model different values of the gravity darkening parameter $\beta$ (0.0, 0.08 and 0.25) are indicated using different symbols. The dependence of q₂/q₁ on $v_{\rm e}$ differs for the different cases but is monotonic in $\beta$ and $v_{\rm e}$ .
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