Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics*[width=5cm,clip]{4134fig1.eps} \end{figure}$ Figure 1: Projected baselines and corresponding position angles for the AMBER and MIDI observations of CPD $-57\hbox{$^\circ$ }~2874$ (see also Table 1).
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In the text

$\begin{figure} \par\includegraphics[width=11.6cm,clip]{4134fig2.eps} \end{figure}$ Figure 2: AMBER/VLTI observations of CPD $-57\hbox{$^\circ$ }~2874$ obtained around Br $\gamma$ with spectral resolution R=1500. The normalized flux is shown in the top panel and the visibilities Vfor each baseline (30% best frames) are given in the other panels (the corresponding projected baselines $B_{\rm p}$ and position angles PA are indicated). The errors in V are $\simeq$ $\pm$ $5\%$ . The dotted lines are the uniform disk angular diameters $\theta _{\rm UD}$ (to be read from the scales on the right axis), computed from V at each $\lambda$ as a zero-order size estimate. The visibilities obtained from the elliptical Gaussian model fit the observations quite well (smooth solid lines; Eqs. (1) and (2), and Table 4). In contrast to the Br $\gamma$ line, the Mg II and Na I lines do not show any clear signature in the visibilities.
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In the text

$\begin{figure} \par\includegraphics[width=11.6cm,clip]{4134fig3.eps} \end{figure}$ Figure 3: MIDI/VLTI observations of CPD $-57\hbox{$^\circ$ }~2874$ obtained in the mid-IR with spectral resolution R=30. This figure is organized as Fig. 2, but here V and $\theta _{\rm UD}$ are shown as filled and open circles, respectively. The MIDI and ISO-SWS (Sloan et al. 2003) spectra ( top panel) do not show any clear evidence of a silicate feature around $10~\mu{\rm m}$ . The MIDI visibilities are well fitted with an elliptical Gaussian model (solid lines; Eqs. (1) and (2), and Table 4).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4134fig4.eps} \end{figure}$ Figure 4: AMBER/VLTI closure phase for CPD $-57\hbox{$^\circ$ }~2874$ obtained around Br $\gamma$ with spectral resolution R=1500. Within the noise level ( $\simeq$ $\pm$ $10\hbox {$^\circ $ }$ ) the closure phase is zero both in the continuum and in the Br $\gamma$ line. This strongly suggests that the CSE has an approximately centrally-symmetric projected intensity distribution in the near-IR.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{4134fig5.eps} \end{figure}$ Figure 5: Size and orientation of the CSE derived from the fit of an elliptical Gaussian model (Eqs. (1) and (2)) to the AMBER/VLTI and MIDI/VLTI visibilities (the corresponding fit parameters are listed in Table 4). The scale in the right is given in stellar diameters ( $2R_{\star }$ ), where the radius $R_{\star }$ is estimated to be $60\pm15~~{R}_{\odot}$ (Sect. 3).
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In the text

$\begin{figure} \par\includegraphics*[width=5cm,clip]{4134fig1.eps} \end{figure}$	Figure 1: Projected baselines and corresponding position angles for the AMBER and MIDI observations of CPD $-57\hbox{$^\circ$ }~2874$ (see also Table 1).
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$\begin{figure} \par\includegraphics[width=12cm,clip]{4134fig5.eps} \end{figure}$	Figure 5: Size and orientation of the CSE derived from the fit of an elliptical Gaussian model (Eqs. (1) and (2)) to the AMBER/VLTI and MIDI/VLTI visibilities (the corresponding fit parameters are listed in Table 4). The scale in the right is given in stellar diameters ( $2R_{\star }$ ), where the radius $R_{\star }$ is estimated to be $60\pm15~~{R}_{\odot}$ (Sect. 3).
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