Astronomy & Astrophysics

$\begin{figure} \par\resizebox{7cm}{!}{\includegraphics{2257fig1.eps}}\end{figure}$ Figure 1: Schematic layout of the VLTI interferometer, showing the baselines used for the calibrators observations as listed in Table 3. North is up.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fig6.eps}}\end{figure}$ Figure 6: Histogram of the number of nights according to the number of OBs (observation blocks) carried out on candidate calibrators. The maximum number of OBs ever observed in one night was 97.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fig7.eps}}\end{figure}$ Figure 7: Calibrators observations on the night of 2 June 2002, using the E0-G1 baseline. See the text for a discussion on the rejection of discrepant visibility points.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fig8.eps}}\end{figure}$ Figure 8: Same as Fig. 7, for the night of 23 July 2001. The baseline used was E0-G0. No measurements were rejected, as explained in the text.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fig9.eps}}\end{figure}$ Figure 9: Calibrators observations on the night of 14 November 2001, using the E0-G0 baseline. The weighted average transfer function is 0.384 with a relative error of only 0.5%. This can be considered as an example of a good night at the VLTI.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fi10.eps}}\end{figure}$ Figure 10: Calibrators observations on the night of 20 April 2003, using the B3-M0 baseline. The weighted average transfer function is 0.574 with a large relative error of 15.8%. This can be considered as an example of a very bad night at the VLTI. Note the large scatter in the measurements of each star.
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In the text

$\begin{figure} \par\resizebox{14cm}{!}{\includegraphics{2257fi11.eps}}\end{figure}$ Figure 11: Long term plot of the night-average VLTI transfer function, as computed from the nominal diameters of the candidate calibrators. Changes of baseline are marked by the vertical segments at the top (short for SID, long for UT baselines). At this scale, the error bars are barely visible.
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In the text

$\begin{figure} \par\resizebox{7cm}{!}{\includegraphics{2257fig1.eps}}\end{figure}$	Figure 1: Schematic layout of the VLTI interferometer, showing the baselines used for the calibrators observations as listed in Table 3. North is up.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fig2.eps}}\end{figure}$	Figure 2: K magnitude distribution of the observed candidate calibrators.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fig3.eps}}\end{figure}$	Figure 3: Angular diameter distribution of the observed candidate calibrators.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fig4.eps}}\end{figure}$	Figure 4: Diameter accuracy distribution of the observed candidate calibrators.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fig5.eps}}\end{figure}$	Figure 5: Sky distribution of the observed candidate calibrators.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fig6.eps}}\end{figure}$	Figure 6: Histogram of the number of nights according to the number of OBs (observation blocks) carried out on candidate calibrators. The maximum number of OBs ever observed in one night was 97.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fig7.eps}}\end{figure}$	Figure 7: Calibrators observations on the night of 2 June 2002, using the E0-G1 baseline. See the text for a discussion on the rejection of discrepant visibility points.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fig8.eps}}\end{figure}$	Figure 8: Same as Fig. 7, for the night of 23 July 2001. The baseline used was E0-G0. No measurements were rejected, as explained in the text.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fig9.eps}}\end{figure}$	Figure 9: Calibrators observations on the night of 14 November 2001, using the E0-G0 baseline. The weighted average transfer function is 0.384 with a relative error of only 0.5%. This can be considered as an example of a good night at the VLTI.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2257fi10.eps}}\end{figure}$	Figure 10: Calibrators observations on the night of 20 April 2003, using the B3-M0 baseline. The weighted average transfer function is 0.574 with a large relative error of 15.8%. This can be considered as an example of a very bad night at the VLTI. Note the large scatter in the measurements of each star.
Open with DEXTER

$\begin{figure} \par\resizebox{14cm}{!}{\includegraphics{2257fi11.eps}}\end{figure}$	Figure 11: Long term plot of the night-average VLTI transfer function, as computed from the nominal diameters of the candidate calibrators. Changes of baseline are marked by the vertical segments at the top (short for SID, long for UT baselines). At this scale, the error bars are barely visible.
Open with DEXTER