Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5410fi01.ps} \end{figure}$ Figure 1: Raw absolute visibilities of calibration stars corrected for their angular diameters and averaged over the [2.13-2.21] $\mu$ m window, allowing us to monitor the instrumental+atmospheric transfer function (points respectively around 1h in red and 7 h in blue). For comparison we have overplotted the raw visibilities of $\kappa$ CMa (around 3 h in green). The $\kappa$ CMa visibilities have the same value as the instrumental+atmospheric transfer function within the error bars, leading to a calibrated visibility of 1, i.e. a non resolved or poorly resolved object on all baselines.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{5410fi02.eps} \end{figure}$ Figure 2: From top to bottom: Pa $\beta$ line profile from the Observatorio do Pico dos Dias, Brazil (dotted line) with our best model fit (plain line), Br $\gamma$ line profile, differential visibilities and differential phases for the three baselines. For each plot, the dots with errors bars are AMBER/VLTI data and the solid line is from our best SIMECA model (see Sect. 4).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,height=5.5cm,clip]{5410fi03.eps} \end{figure}$ Figure 3: $\kappa$ CMa's Spectral Energy Distribution (SED) from SIMBAD CDS (triangles). Dotted line: emission from the central star assuming a black body with $R_\star = 6~R_\odot$ , $T_{\rm eff}=22~500$ K and d=230 pc. Dashed line: free-free and free-bound envelope contribution from the SIMECA code between 0.3 and 100 $\mu$ m. Plain line: Central star emission + envelope contribution.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5410fi04.ps} \end{figure}$ Figure 4: $\kappa$ CMa diameters in the Br $\gamma$ line, assuming an unresolved star + uniform disk models, as a function of the baseline position angle (in mas). The length of each plot corresponds to the error bar measurement whereas diameters are given by the center of each error bar.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.2cm,height=3.2cm,clip]{5410fi05.eps}... ...m} \includegraphics[width=6.5cm,height=3.2cm,clip]{5410fi06.eps} \end{figure}$ Figure 5: Upper picture: $\kappa$ CMa Pa $\beta$ line profile observed in December 2005 at the Observatorio do Picos dos Dias, Brazil (solid line). Estimated symmetric part of the Pa $\beta$ profile (dotted line) using an axi-symmetric model. The asymmetric residue corresponds to the emission of "one-armed'' over-density (dashed line). Bottom picture: differential phase variation measured along the B₁ baseline (dots with errors bars) and theoretical phase from the SIMECA code.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5410fi07.ps} \end{figure}$ Figure 6: Intensity map in the continuum at 2.15 $\mu$ m obtained with SIMECA for our best model parameters. The inclination angle is 60 $\hbox {$^\circ $ }$ , the central black dot represents the $\kappa$ CMa photosphere (0.25 mas); the bright part in the equatorial disk is produced by the over-density which is oriented along the B₁ baseline. This over-density is also responsible for a 30% emission excess in the asymmetric V part of the Br $\gamma$ line.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5410fi08.ps} \end{figure}$ Figure 7: V/R variations obtained from the literature between 1965 and 2003, from Jaschek (1965), Slettebak (1982), Banerjee (2000) and this work.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{5410fi02.eps} \end{figure}$	Figure 2: From top to bottom: Pa $\beta$ line profile from the Observatorio do Pico dos Dias, Brazil (dotted line) with our best model fit (plain line), Br $\gamma$ line profile, differential visibilities and differential phases for the three baselines. For each plot, the dots with errors bars are AMBER/VLTI data and the solid line is from our best SIMECA model (see Sect. 4).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,height=5.5cm,clip]{5410fi03.eps} \end{figure}$	Figure 3: $\kappa$ CMa's Spectral Energy Distribution (SED) from SIMBAD CDS (triangles). Dotted line: emission from the central star assuming a black body with $R_\star = 6~R_\odot$ , $T_{\rm eff}=22~500$ K and d=230 pc. Dashed line: free-free and free-bound envelope contribution from the SIMECA code between 0.3 and 100 $\mu$ m. Plain line: Central star emission + envelope contribution.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{5410fi04.ps} \end{figure}$	Figure 4: $\kappa$ CMa diameters in the Br $\gamma$ line, assuming an unresolved star + uniform disk models, as a function of the baseline position angle (in mas). The length of each plot corresponds to the error bar measurement whereas diameters are given by the center of each error bar.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{5410fi08.ps} \end{figure}$	Figure 7: V/R variations obtained from the literature between 1965 and 2003, from Jaschek (1965), Slettebak (1982), Banerjee (2000) and this work.
Open with DEXTER