All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4771fig1.eps} \end{figure}$ Figure 1: Coverage of the (u,v) plane for the VINCI observations of Achernar. The K band observations (MONA beam combiner) are represented using circles (open for siderostat observations, solid for the Unit Telescopes), and the H band observations are represented using crosses. The scales are in units of $B/\lambda$ , expressed in cycles/arcsec.
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In the text

$\begin{figure} \par\includegraphics[width=16.6cm,clip]{4771fig2.eps} \end{figure}$ Figure 2: Left: squared visibilities V² measured on Achernar and corresponding to projected baseline azimuth angles around the polar direction (values between 10 $^\circ$ and 70 $^\circ$ ). Right: V² corresponding to projected baseline azimuth angles around the equatorial direction (values between 100 $^\circ$ and 160 $^\circ$ ). The solid squares and crosses represent K and H band data, respectively. The solid curves represent theoretical V² along the pole ( left) and the equator ( right) obtained from the 2D fit of our two-component model (Sect. 3) to all measured V²(Tables 3a-d. Note also the V² outliers along the polar direction, which were not included in the fit (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4771fig3.eps} \end{figure}$ Figure 3: Graphical representation of the best-fit model intensity distribution of Achernar. The relative flux contributions from the star and the envelope are not to scale. This illustration should not be considered as a true image of the star.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{4771fig4a.eps}\par\vspace*... ...\par\vspace*{2mm} \includegraphics[width=6.8cm,clip]{4771fig4c.eps} \end{figure}$ Figure 4: Residuals of the visibility fit in units of V² standard deviation $\sigma$ , as a function of azimuth angle, for a uniform disk ( top), a uniform ellipse ( middle), and our uniform ellipse with CSE model ( bottom). The H band data are shown with crosses. The four outliers (open diamonds) were not included in the fit. The dashed and dot-dashed lines represent, respectively, the polar and equatorial directions of the models, including a uniform ellipse.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4771fig5a.eps}\par\vspace*{2mm} \includegraphics[width=7cm,clip]{4771fig5b.eps} \end{figure}$ Figure 5: Residuals of the visibility fit as a function of projected baseline length ( top) and date of observation ( bottom). The symbols are the same as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4771fig1.eps} \end{figure}$	Figure 1: Coverage of the (u,v) plane for the VINCI observations of Achernar. The K band observations (MONA beam combiner) are represented using circles (open for siderostat observations, solid for the Unit Telescopes), and the H band observations are represented using crosses. The scales are in units of $B/\lambda$ , expressed in cycles/arcsec.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{4771fig3.eps} \end{figure}$	Figure 3: Graphical representation of the best-fit model intensity distribution of Achernar. The relative flux contributions from the star and the envelope are not to scale. This illustration should not be considered as a true image of the star.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{4771fig5a.eps}\par\vspace*{2mm} \includegraphics[width=7cm,clip]{4771fig5b.eps} \end{figure}$	Figure 5: Residuals of the visibility fit as a function of projected baseline length ( top) and date of observation ( bottom). The symbols are the same as in Fig. 4.
Open with DEXTER