All Figures

$\begin{figure} \includegraphics[width=9cm,clip]{0614fig1.eps} \end{figure}$ Figure 1: Left: names, lengths, and PA for each baseline of the two triplets of observation. Note that the two measurements from January 8 with A0-K0-G1 are merged into B₁, B₂, and B₃ baselines, since the projected baseline length and PA does not vary significantly between them. B₄, B₅, and B₆ baselines correspond to the E0-G0-H0 triplets. Right: (u, v) plane coverage obtained during the $\delta$ Cen observing run. Fortunately, the largest projected baseline is aligned with the shorter ones.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,height=4.3cm,clip]{0614fig2.ps}\end{figure}$ Figure 2: $\delta$ Cen Spectral Energy Distribution (SED) reconstructed from various sources in the literature: Morel (1978), 2MASS, IRAS magnitude and flux measurements (diamonds), IUE spectra (solid line in the UV), and ISO spectra (solid line in the IR). The dashed line is a Kurucz model for $T_{\rm eff}=21~000$ K, $R_\star=5.9~R_\odot$ , $\log g=4$ , and d=121 pc.
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In the text

$\begin{figure} \includegraphics[width=3.8cm,clip]{0614fig3.ps}\hspace*{2mm} \i... ...5.ps}\hspace*{2mm} \includegraphics[width=3.5cm,clip]{0614fig6.ps} \end{figure}$ Figure 3: Left: LR K (dark) and H (gray) bands visibilities for the January 8, 2008 baselines (B₄, B₅, and B₆) as a function of the spatial frequency. Second picture from the left to the right: MR visibilities for the January 5, 2008 baselines (B₁, B₂, and B₃) as a function of the spatial frequency. For all figures, measurements are given by the error bars, whereas the solid line corresponds to our best-fit binary + uniform disk circumstellar envelope modeled using parameters from Table 2.
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In the text

$\begin{figure} \par\includegraphics[width=4cm,clip]{0614fig7.ps}\hspace*{2mm} \includegraphics[width=3.75cm,clip]{0614fig8.ps}\end{figure}$ Figure 4: Observed and modeled closure phase for the B₄B₅B₆ ( left) and B₁B₂B₃ ( right) triplets plotted as a function of the average spatial frequency. For all figures, the measurements are represented by the error bars whereas the solid line corresponds to our best binary + uniform disk circumstellar envelope modeled using parameters from Table 2.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,height=4.3cm,clip]{0614fig2.ps}\end{figure}$	Figure 2: $\delta$ Cen Spectral Energy Distribution (SED) reconstructed from various sources in the literature: Morel (1978), 2MASS, IRAS magnitude and flux measurements (diamonds), IUE spectra (solid line in the UV), and ISO spectra (solid line in the IR). The dashed line is a Kurucz model for $T_{\rm eff}=21~000$ K, $R_\star=5.9~R_\odot$ , $\log g=4$ , and d=121 pc.
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$\begin{figure} \par\includegraphics[width=4cm,clip]{0614fig7.ps}\hspace*{2mm} \includegraphics[width=3.75cm,clip]{0614fig8.ps}\end{figure}$	Figure 4: Observed and modeled closure phase for the B₄B₅B₆ ( left) and B₁B₂B₃ ( right) triplets plotted as a function of the average spatial frequency. For all figures, the measurements are represented by the error bars whereas the solid line corresponds to our best binary + uniform disk circumstellar envelope modeled using parameters from Table 2.
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