All Figures

$\begin{figure} \par\includegraphics[width=7cm]{9627fig1.eps} \end{figure}$ Figure 1: AMBER calibrated spectrum of 51 Oph around the 2-0 and 3-1 bands of the CO overtone at 2.3 microns. For comparison purposes is plotted (dashed line) the same spectrum measured with the TNG spectrograph (L. Testi, private communication). Note that we did not plot the TNG spectrum between the two bandheads because of irrelevant instrumental artifact.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{9627fig2.eps} \end{figure}$ Figure 2: MR-K calibrated visibilities as a function of the wavelengths for the three baselines and overplotted best model (black thick line), for the ring case.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{9627fig3.eps} \end{figure}$ Figure 3: LR-K calibrated visibilities as a function of the projected baselines, for the three observations, and overplotted best model (lines). In each panel, colors red, blue,and green correspond to baselines G1-D0, D0-H0, and G1-D0 respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{9627fig4.eps} \end{figure}$ Figure 4: Spectral energy distribution of 51 Oph taken from literature (Waters et al. 1988) (crosses) and superimposed best fit model (solid line) using MCFOST dusty disk model. The main parameters that are fitted are the inner radius $R_{\rm dust}=1.2$ AU, the outer radius $R_{\rm out}=400$ AU scale height at 1 AU H₀ = 0.04, the flaring exponent $\beta =1.1$ , the grain size distribution (see text), the surface density exponent p=-1.25 and the total mass of dust $M_{\rm dust} = 10^{-8}~M_{\odot}$ . We refer to Pinte et al. (2006) for a thorough description of the modelling.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{9627fig5.eps} \end{figure}$ Figure 5: MR-K continuum visibilities (top panel) and LR-K visibilities as a function of the baseline and and overplotted MCFOST model arising from SED fitting (lines). The color code is the same than in Figs. 2 and 3. We can see that this model, with inner radius equal to the dust sublimation radius, is incompatible with the interferometric data, with a resulting $\chi ^2$ of $\sim$ 10.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{9627fig1.eps} \end{figure}$	Figure 1: AMBER calibrated spectrum of 51 Oph around the 2-0 and 3-1 bands of the CO overtone at 2.3 microns. For comparison purposes is plotted (dashed line) the same spectrum measured with the TNG spectrograph (L. Testi, private communication). Note that we did not plot the TNG spectrum between the two bandheads because of irrelevant instrumental artifact.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm]{9627fig2.eps} \end{figure}$	Figure 2: MR-K calibrated visibilities as a function of the wavelengths for the three baselines and overplotted best model (black thick line), for the ring case.
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$\begin{figure} \par\includegraphics[width=7cm]{9627fig3.eps} \end{figure}$	Figure 3: LR-K calibrated visibilities as a function of the projected baselines, for the three observations, and overplotted best model (lines). In each panel, colors red, blue,and green correspond to baselines G1-D0, D0-H0, and G1-D0 respectively.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm]{9627fig5.eps} \end{figure}$	Figure 5: MR-K continuum visibilities (top panel) and LR-K visibilities as a function of the baseline and and overplotted MCFOST model arising from SED fitting (lines). The color code is the same than in Figs. 2 and 3. We can see that this model, with inner radius equal to the dust sublimation radius, is incompatible with the interferometric data, with a resulting $\chi ^2$ of $\sim$ 10.
Open with DEXTER