Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2556fig1} \end{figure}$ Figure 1: (u,v) tracks corresponding to the observations of FU Orionis. Left panel: H data; right panel: K data. The (u,v) points have been labeled with the interferometer and the baseline used.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2556fig2} \end{figure}$ Figure 2: Calibrated squared visibilities of FU Orionis as function of hour angle in H ( left column) and K band ( right column). Rows from top to bottom display data obtained with the 6 interferometric baselines.
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In the text

$\begin{figure} \par\parbox{6.7cm}{ \includegraphics[width=6.65cm,clip]{2556fig3... ...parbox{7.75cm}{ \includegraphics[width=7.75cm,clip]{2556fig3b} } \end{figure}$ Figure 3: Accretion disk model with baseline-averaged data corresponding to parameters listed in Table 4. Lines correspond to the model and symbols to measurements. The dotted line corresponds to an unresolved object. For the sake of clarity, data have been binned in the figure, but the model fit was performed using individual measurements. Top-left panel: spectral energy distribution and best fit model. Right panel: visibility data versus hour angle in H and K. Bottom-left panel: synthetic images in H and K in logarithmic scale. East is left and North is up.
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In the text

$\begin{figure} \par\parbox{6.7cm}{ \includegraphics[width=6.65cm,clip]{2556fig5... ...parbox{7.75cm}{ \includegraphics[width=7.75cm,clip]{2556fig5b} } \end{figure}$ Figure 4: Disk-spot model corresponding to parameters of Table 5. Lines corresponds to the best model fit and markers to visibilities from Fig. 2 in binned form. Top-left panel: spectral energy distribution and best fit model. The solid line stands for the whole model and the dashed one for the spot. Right panel: visibility data vs. hour angle for each baseline in H and K. The contribution of the disk is displayed in dashed lines. Bottom-left panel: synthetic image in logarithmic scale. East is left and North is up.
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In the text

$\begin{figure} \includegraphics[width=7.65cm,clip]{2556fig4a}\hspace*{6mm} \in... ...6fig4c}\hspace*{6mm} \includegraphics[width=7.6cm,clip]{2556fig6c} \end{figure}$ Figure 5: $\chi ^2$ distribution of the disk alone ( left column) and disk-spot ( right column) models around the best fit (marked with a square). The white solid line draws the 3- $\sigma$ limit ("goodness-of-fit'' > 0.25%). Top: inclination vs. temperature. Middle: temperature law exponent vs. minimum radius. Bottom left: inclination vs. position angle of the disk. Bottom right: position angle of the spot vs. projected distance to the centre. Left subpanels: $\chi ^2$ determined with both visibility and SED data. Middle subpanels: $\chi ^2$ determined with the SED only. Right subpanels: $\chi ^2$ determined with the visibilities only.
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In the text

$\begin{figure} \par\includegraphics[width=7.75cm,clip]{2556fig7} \end{figure}$ Figure 6: Predicted squared visibility curve of the disk+spot model for FU Ori through the infrared spectrum with the triplet of VLTI 8 m telescopes U2-U3-U4.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2556fig1} \end{figure}$	Figure 1: (u,v) tracks corresponding to the observations of FU Orionis. Left panel: H data; right panel: K data. The (u,v) points have been labeled with the interferometer and the baseline used.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2556fig2} \end{figure}$	Figure 2: Calibrated squared visibilities of FU Orionis as function of hour angle in H ( left column) and K band ( right column). Rows from top to bottom display data obtained with the 6 interferometric baselines.
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$\begin{figure} \par\includegraphics[width=7.75cm,clip]{2556fig7} \end{figure}$	Figure 6: Predicted squared visibility curve of the disk+spot model for FU Ori through the infrared spectrum with the triplet of VLTI 8 m telescopes U2-U3-U4.
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