All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{1765fig1.eps}\end{figure}$ Figure 1: Calibrated interferometric measurements for Aldebaran obtained on 12 January 2002 (squares) and 2 October 2003 (triangles). The solid line is a fit by the combined limb-darkened angular diameter values listed in Table 4. The insets show the data with large magnification, including the error bars and the curves corresponding to a change of one standard deviation in the angular diameter (dotted lines).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1765fig2.eps}\end{figure}$ Figure 2: Previous determinations of the angular diameter of Aldebaran with their error bars, as extracted from the available literature. LO and LBI measurements are shown as triangles and squares, respectively. Solid symbols mark measurements with errors of 0.4 mas or less, open symbols those with errors between 0.4 and 2.0 mas. Measurements with errors larger than 2.0 mas also exist, but are not shown here. For clarity, errorbars are shown only for the best measurements. Our result, as listed in Table 4, is in excellent agreement with the weighted average of these latter.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1765fig3.eps}\end{figure}$ Figure 3: The occultation trace of Aldebaran of February 5, 1998. The fit by a uniform circular disk was quite accurate, yielding the value reported in Table 4. The fit itself is not overplotted since it would be hard to tell from the data. Instead, we show the fit residuals in the lower curve.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{1765fig4.eps}\end{figure}$ Figure 4: Brightness profile of Aldebaran derived from the data of February 5, 1998 using a model-independent analysis. The dashed line refers to the profile after 1000 iterations, the solid line at convergence after about 4000 iterations (see text). The horizontal segment marks the size of the equivalent uniform disk diameter (see Table 4).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1765fig3.eps}\end{figure}$	Figure 3: The occultation trace of Aldebaran of February 5, 1998. The fit by a uniform circular disk was quite accurate, yielding the value reported in Table 4. The fit itself is not overplotted since it would be hard to tell from the data. Instead, we show the fit residuals in the lower curve.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{1765fig4.eps}\end{figure}$	Figure 4: Brightness profile of Aldebaran derived from the data of February 5, 1998 using a model-independent analysis. The dashed line refers to the profile after 1000 iterations, the solid line at convergence after about 4000 iterations (see text). The horizontal segment marks the size of the equivalent uniform disk diameter (see Table 4).
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