Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.5cm]{3924-fig1} \end{figure}$ Figure 1: Short-exposure image of the MWC 297 signal on the AMBER detector. X-axis corresponds to the spatial extension of the beams and Y-axis to the wavelength. First column (Dk) corresponds to the dark, the second (P1) and third (P2) ones are the beams from the first and second telescope resp., and finally the last column (IF) shows the fringes obtained by superposition of the two beams. The bright row is the $\ensuremath {\text {Br}\gamma }$ line at $2165.6~\ensuremath{\text{nm}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{3924-fig2} \end{figure}$ Figure 2: Spectral dependence of the visibility as measured with AMBER for MWC 297 around the $\ensuremath {\text {Br}\gamma }$ line.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3924-fig3} \end{figure}$ Figure 3: Comparison of $\ensuremath {\text {Br}\gamma }$ observed with AMBER (solid line) and ISAAC (dotted line). The dashed line corresponds to the ISAAC spectrum convolved by the response function of AMBER.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3924-fig4} \end{figure}$ Figure 4: Sketch of the model including an optically thick disk and an outflowing wind (edge-on view). The receding part of the wind is only partly visible because of the screen made by the optically thick disk.
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In the text

$\begin{figure} \mbox{ \includegraphics[width=7.4cm]{3924-fig5a} \includegraphics[width=7.4cm]{3924-fig5b} } \end{figure}$ Figure 5: Result from the optically thick disk model. Left panel: observed and modeled SED for MWC 297. The full dots are the continuum measurements taken from Pezzuto et al. (1997), also included are the ISO SWS/LWS spectra. Dotted line is the star, dashed line the accretion disk, and the full line the resulting total flux of the model. Right panel: resulting best-fit model radial squared visibilities compared with continuum squared visibilities observed with AMBER, IOTA and PTI. Full line and IOTA data are in the H-band, dashed line and AMBER/PTI are in the K-band. PTI values are upper limits.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{3924-fig6} \end{figure}$ Figure 6: Double peaked $\ensuremath {\text {Br}\gamma }$ profile observed by ISAAC (full line) and modeled with the outflowing wind model (dotted line). We have also plotted the cumulative contribution of the accretion disk (dashed line) and of the star (dashed-dotted).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3924-fig7} \end{figure}$ Figure 7: The visibility observed with AMBER (points with error bars) and the one obtained from the outflowing wind model (full line).
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In the text

$\begin{figure} \par\includegraphics[width=17cm]{3924-fig8} \end{figure}$ Figure 8: Edge-on intensity maps of the wind in the computed $\ensuremath {\text {H}\alpha }$ , $\ensuremath {\text {H}\beta }$ , $\ensuremath {\text {Br}\gamma }$ lines.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{3924-fig9} \end{figure}$ Figure 9: Continuum H-band squared visibilities obtained with the disk model compared to the IOTA visibilities observed during the transit of the object over the sky with the IOTA S15N35 baseline.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=5.6cm,height=6cm]{3924-fig10a} ... ...ce*{8cm} \includegraphics[width=5.6cm,height=6cm]{3924-fig10c} } \end{figure}$ Figure 10: Pole-on intensity maps of the wind $\ensuremath {\text {Br}\gamma }$ emission ( left panel) and of the K-band disk continuum emission ( center panel). Right panel shows a radial cut of these intensity maps with the $\ensuremath {\text {Br}\gamma }$ wind in solid line and the continuum disk in dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{3924-fig2} \end{figure}$	Figure 2: Spectral dependence of the visibility as measured with AMBER for MWC 297 around the $\ensuremath {\text {Br}\gamma }$ line.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3924-fig3} \end{figure}$	Figure 3: Comparison of $\ensuremath {\text {Br}\gamma }$ observed with AMBER (solid line) and ISAAC (dotted line). The dashed line corresponds to the ISAAC spectrum convolved by the response function of AMBER.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3924-fig4} \end{figure}$	Figure 4: Sketch of the model including an optically thick disk and an outflowing wind (edge-on view). The receding part of the wind is only partly visible because of the screen made by the optically thick disk.
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$\begin{figure} \par\includegraphics[width=8.5cm]{3924-fig6} \end{figure}$	Figure 6: Double peaked $\ensuremath {\text {Br}\gamma }$ profile observed by ISAAC (full line) and modeled with the outflowing wind model (dotted line). We have also plotted the cumulative contribution of the accretion disk (dashed line) and of the star (dashed-dotted).
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3924-fig7} \end{figure}$	Figure 7: The visibility observed with AMBER (points with error bars) and the one obtained from the outflowing wind model (full line).
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$\begin{figure} \par\includegraphics[width=17cm]{3924-fig8} \end{figure}$	Figure 8: Edge-on intensity maps of the wind in the computed $\ensuremath {\text {H}\alpha }$ , $\ensuremath {\text {H}\beta }$ , $\ensuremath {\text {Br}\gamma }$ lines.
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$\begin{figure} \par\includegraphics[width=7cm]{3924-fig9} \end{figure}$	Figure 9: Continuum H-band squared visibilities obtained with the disk model compared to the IOTA visibilities observed during the transit of the object over the sky with the IOTA S15N35 baseline.
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$\begin{figure} \par\mbox{ \includegraphics[width=5.6cm,height=6cm]{3924-fig10a} ... ...ce*{8cm} \includegraphics[width=5.6cm,height=6cm]{3924-fig10c} } \end{figure}$	Figure 10: Pole-on intensity maps of the wind $\ensuremath {\text {Br}\gamma }$ emission ( left panel) and of the K-band disk continuum emission ( center panel). Right panel shows a radial cut of these intensity maps with the $\ensuremath {\text {Br}\gamma }$ wind in solid line and the continuum disk in dashed line.
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