Astronomy & Astrophysics

All Figures

$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{0849fig1.eps} } \end{figure}$ Figure 1: Top: design of the integrated optics two-beam combiner. Bottom: the connected combiner in its box at ESO.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0849fig2.eps} \end{figure}$ Figure 2: Diagram of the coherence factor data processing. The numbers in brackets refer to the steps detailed in the text (see Sect. 3.2.2).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0849fig3.eps} \end{figure}$ Figure 3: Cross-correlation of $\kappa _a'$ with the estimator of injection: the flux ( left) and normalized temporal derivative of the flux ( right). The solid line is the vertical average of the diagram. Note the smaller dispersion of the data with the UTs ( top) than with the siderostats ( bottom) due to the smaller photon noise. Each figure corresponds to a BEAM A calibration file of 20 scans (10 840 points) on $\alpha$ Aql.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0849fig4.eps} \end{figure}$ Figure 4: Long time fluctuations of the $\kappa$ ratio on $\alpha$ Aql. Each point represents one observation and vertical lines separate the different nights. The last night was carried out on the Unit Telescopes UT1 and UT2. With the BEAM-B file, $\kappa _b'$ is the average ratio of interferometric on photometric flux. With the ON-SOURCE file, $\kappa _a$ and $\kappa _b$ are estimated at the same time by a linear fit of the interferometric flux with the two photometric ones (see Sect. 3.2.1). The estimated error bars are plotted at the bottom left corner for the siderostats and at the bottom right for the UTs.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0849fig5.eps} \end{figure}$ Figure 5: Instrumental visibility with the IONIC component during the different observation nights on 3 calibrators stars ( $\alpha$ Aql, $\alpha$ Ind, $\alpha$ Psa) and on the internal light LEONARDO. The last night (31) was carried out with the UTs. The dotted line is the average instrumental visibility on the sky with the siderostats. The histogram is plotted in the left sub-figure. The instrumental visibility is computed with the Fourier visibility estimator. The correlation between the Direct and Fourier estimator is plotted in the right sub-figure. We assume an effective wavelength of $1.63~\mu$ m and the uniform disk angular diameters of Table 4.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0849fig6.eps} \end{figure}$ Figure 6: Visibility obtained on different stars corrected for the instrumental visibility ( $87\%$ ) and fitted with the theoretical visibility derived from Table 5 (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0849fig7.eps} \end{figure}$ Figure 7: Relative error in % of the mean visibility with the IONIC combiner versus the total coherent flux collected during the acquisition. X-axis units have normalized by the flux obtained on the best siderostat file (100 scans on $\alpha$ Aql with a visibility of 0.7). The dash line represents a linear fit. The marker used are the same as for Fig. 4.
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In the text

$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{0849fig1.eps} } \end{figure}$	Figure 1: Top: design of the integrated optics two-beam combiner. Bottom: the connected combiner in its box at ESO.
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$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0849fig2.eps} \end{figure}$	Figure 2: Diagram of the coherence factor data processing. The numbers in brackets refer to the steps detailed in the text (see Sect. 3.2.2).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0849fig6.eps} \end{figure}$	Figure 6: Visibility obtained on different stars corrected for the instrumental visibility ( $87\%$ ) and fitted with the theoretical visibility derived from Table 5 (solid line).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0849fig7.eps} \end{figure}$	Figure 7: Relative error in % of the mean visibility with the IONIC combiner versus the total coherent flux collected during the acquisition. X-axis units have normalized by the flux obtained on the best siderostat file (100 scans on $\alpha$ Aql with a visibility of 0.7). The dash line represents a linear fit. The marker used are the same as for Fig. 4.
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