All Figures

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{ABPicfig1.ps}\end{figure}$ Figure 1: $K_{\rm s}$ -band coronagraphic image of AB Pic A and b acquired on 17 March 2003 with an occulting mask of diameter 1.4''.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{ABPicfig2.ps}\end{figure}$ Figure 2: Top: differences of separation between AB Pic A and b on 17 March 2003, 5 March 2004, and 25 September 2004. Bottom: differences of position angle for AB Pic A and b. The expected evolutions with their uncertainties for bound (solid line) and stationary background (dashed line) objects are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ABPicfig3.ps}\end{figure}$ Figure 3: K-band spectrum of AB Pic b acquired on 3 December 2004 with the low resolution ( ${R}_{\lambda }=550$ ) grism of NACO, the 86 mas slit and the S54 camera (54 mas/pixel). The best $\chi ^2$ adjustment is found with the L1 dwarf 2MASSJ0345+2540 (Geballe et al. 2002).
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{ABPicfig1.ps}\end{figure}$	Figure 1: $K_{\rm s}$ -band coronagraphic image of AB Pic A and b acquired on 17 March 2003 with an occulting mask of diameter 1.4''.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{ABPicfig2.ps}\end{figure}$	Figure 2: Top: differences of separation between AB Pic A and b on 17 March 2003, 5 March 2004, and 25 September 2004. Bottom: differences of position angle for AB Pic A and b. The expected evolutions with their uncertainties for bound (solid line) and stationary background (dashed line) objects are indicated.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ABPicfig3.ps}\end{figure}$	Figure 3: K-band spectrum of AB Pic b acquired on 3 December 2004 with the low resolution ( ${R}_{\lambda }=550$ ) grism of NACO, the 86 mas slit and the S54 camera (54 mas/pixel). The best $\chi ^2$ adjustment is found with the L1 dwarf 2MASSJ0345+2540 (Geballe et al. 2002).
Open with DEXTER