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$\begin{figure} \par\includegraphics[width=18cm]{0605fig1.eps} \end{figure}$ Figure 1: NACO H-band images.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{0605fig2.eps} \end{figure}$ Figure 2: Lick Ks-band images. The spike South of 2MASS J1626 is much narrower than the point-spread function and cannot be stellar.
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In the text

$\begin{figure} \includegraphics[width=9cm,clip]{0605fig3.eps} \end{figure}$ Figure 3: Limits of sensitivity $\Delta$ Mag vs. separation of the adaptive optics observations performed with VLT/NACO (J and H bands) and Lick/AO (Ks band).
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{0605fig4.eps} \end{figure}$ Figure 4: Close binary fraction vs. spectral type. The short thick lines show the new binary fraction for each L and T spectral type. The longer dashed lines indicate the published fraction, averaged over four groups of subtypes (Burgasser 2007), while the thick lines give the updated average fraction including our results. The bottom numbers indicate the numbers of resolved binaries and total numbers of observed brown dwarfs. The 90% confidence levels for statistical noise are reported as vertical thin lines. We include the results of the Duquennoy & Mayor (1991) survey for G stars and Reid & Gizis (1997). We point out again the different survey sensitivities, in particular Duquennoy & Mayor (1991) is based on the radial-velocity method.
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In the text

$\begin{figure} \par\includegraphics[width=18cm]{0605fig1.eps} \end{figure}$	Figure 1: NACO H-band images.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{0605fig2.eps} \end{figure}$	Figure 2: Lick Ks-band images. The spike South of 2MASS J1626 is much narrower than the point-spread function and cannot be stellar.
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$\begin{figure} \includegraphics[width=9cm,clip]{0605fig3.eps} \end{figure}$	Figure 3: Limits of sensitivity $\Delta$ Mag vs. separation of the adaptive optics observations performed with VLT/NACO (J and H bands) and Lick/AO (Ks band).
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