Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{a_Ori_UD_vs_lamb... ...cludegraphics[angle=-90,width=7.8cm,clip]{a_Her_UD_vs_lambda.eps} \end{figure}$ Figure 1: Uniform disk diameters measured for $\alpha$ Orionis and $\alpha$ Herculis. Values are reported in Benson et al. (1991), Mozurkewich et al. (1991), Dyck et al. (1992), Tuthill et al. (1997), Burns et al. (1997), Mennesson et al. (1999), Young et al. (2000), Weiner et al. (2000), Chagnon et al. (2002).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{transfert.eps} \end{figure}$ Figure 2: Instrumental visibility on November 9, 1996 for the two interferometric channels (full circles). Open circles are the interpolated instrumental visibilities at the time Betelgeuse was observed.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{a_Ori_UD_2.eps} \end{figure}$ Figure 3: K band visibilities for $\alpha$ Orionis. The $\chi ^{2}$ is computed with first lobe visibilities only.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{a_Her_UD_2.eps} \end{figure}$ Figure 4: K band visibilities for $\alpha$ Herculis. The $\chi ^{2}$ is computed with first lobe visibilities only.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{a_Ori_LD_2.eps} \end{figure}$ Figure 5: Fit of $\alpha$ Orionis data by a limb darkened disk model.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{a_Her_LD_2.eps} \end{figure}$ Figure 6: Fit of 1997 $\alpha$ Herculis data by a limb darkened disk model.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14.3cm,clip]{a_Ori_KLN_2.eps} \end{figure}$ Figure 7: Fit of $\alpha$ Orionis K, L and 11.15 $\mu$ m data by a photosphere plus layer model. The 11.15 $\mu$ m data have been rescaled to eliminate the contribution of dust (see text). Fits of the K, L and 11.15 $\mu$ m data are respectively the continuous, dotted and dashed lines. Low frequency data in the L band around 18 cycles/arcsec poorly contribute to the fit which is more constrained by the better calibrated data at 26 cycles/arcsec.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{a_Ori_UD_vs_lamb... ...cludegraphics[angle=-90,width=7.8cm,clip]{a_Her_UD_vs_lambda.eps} \end{figure}$	Figure 1: Uniform disk diameters measured for $\alpha$ Orionis and $\alpha$ Herculis. Values are reported in Benson et al. (1991), Mozurkewich et al. (1991), Dyck et al. (1992), Tuthill et al. (1997), Burns et al. (1997), Mennesson et al. (1999), Young et al. (2000), Weiner et al. (2000), Chagnon et al. (2002).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{transfert.eps} \end{figure}$	Figure 2: Instrumental visibility on November 9, 1996 for the two interferometric channels (full circles). Open circles are the interpolated instrumental visibilities at the time Betelgeuse was observed.
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$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{a_Ori_UD_2.eps} \end{figure}$	Figure 3: K band visibilities for $\alpha$ Orionis. The $\chi ^{2}$ is computed with first lobe visibilities only.
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$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{a_Her_UD_2.eps} \end{figure}$	Figure 4: K band visibilities for $\alpha$ Herculis. The $\chi ^{2}$ is computed with first lobe visibilities only.
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$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{a_Ori_LD_2.eps} \end{figure}$	Figure 5: Fit of $\alpha$ Orionis data by a limb darkened disk model.
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$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{a_Her_LD_2.eps} \end{figure}$	Figure 6: Fit of 1997 $\alpha$ Herculis data by a limb darkened disk model.
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