All Figures

$\begin{figure} \par\includegraphics[width=7.35cm,clip]{5545fig1.ps}\end{figure}$ Figure 1: Distribution of separations/orbital semimajor axes of the wide binaries of our sample.
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In the text

$\begin{figure} \par\includegraphics[width=16.35cm,clip]{5545fg2a.eps}\vspace*{0.5cm}\ \includegraphics[width=16.35cm,clip]{5545fg2b.eps}\end{figure}$ Figure 2: Already known and candidate triple ( upper panel) and quadruple ( lower panel) systems detected in our VLT/NACO survey. These systems are the only apparent high-order multiple systems found in our sample, physical systems will be identified in Sect. 4.5. North is up, east is left.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5545fig3.ps}\end{figure}$ Figure 3: Relative motion in RA and Dec between the RZ93 positions and those measured in this study (NACO-RZ93). Green triangles are pairs with projected separations <150 AU.
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{5545fig4.ps}\end{figure}$ Figure 4: Results of our survey in a plot of flux ratio or magnitude difference in H and K vs. pair separation. The circle symbol refers to pairs in triple systems while square symbols are for pairs in quadruple systems. The lines represent the completeness of our observations as derived from the sensitivity limit for undetected companions of the only binaries of the sample (see Sect. 4.2). The lines are, from top to bottom, 99%, 90%, 70%, 50%, 30%, 10% and 1% completeness.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{5545fg5a.ps}\hspace*{7.5m... ...g5c.ps}\hspace*{8mm} \includegraphics[width=7.5cm,clip]{5545fg5d.ps}\end{figure}$ Figure 5: Upper left: J-H/H-K color-color diagram for all sources with reliable 2MASS magnitudes, i.e. detected in all three bands, in the FOV of our targets. Blue small dot symbols denote sources detected in our survey while green triangle symbols are those non or marginally detected. Upper right: J-H/H-K color-color diagram for the new (PH $\alpha$ 30, CGH $\alpha$ 5/6, ESO H $\alpha$ 283) and unconfirmed (LkH $\alpha$ 336 and Sz 41) systems. Filled squares represent component(s) included in the $\sim$ 2 arcsec beam of 2MASS along with the main component, filled circles are possible companions linked to the latter by dotted lines. The loci of unreddened dwarf and giant stars are shown as the solid lines (Bessel & Brett 1988), as well as the locus of unreddened classical T Tauri stars (CTTS) as the dashed line (Meyer et al. 1997). A reddening vector for a standard reddening law is shown (E(J-H) = 0.11 $A_{\rm V}$ , E(H-K) = 0.065 $A_{\rm V}$ , Meyer et al. 1997). Lower left: H-K/M_k color-magnitude diagram for all resolved components in the FOV of our targets for which we have a H-K color. As above, blue small dot symbols denote sources detected in our survey while green triangle symbols are those non-detected. The distribution of component is relative to the ZAMS, to the beginning of the giant branch (GB), and to a 1 Myr isochrone for PMS stars from 0.08 to 1.4 $M_{\odot }$ (with [M/H] = 0, Y = 0.275 and $L_{\rm mix}$ = $H_{\rm p}$ , Baraffe et al. 1998). Lower right: H-K/M_k color-magnitude diagram for all resolved components of the new and unconfirmed systems above. Absolute magnitudes M_K are computed using the adopted distances shown in Table 1 and assuming 10% relative error. The reddening vector assumes A_K = 0.11 $A_{\rm V}$ . All data are in the CIT system.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{5545fig6.eps}\end{figure}$ Figure 6: Locus of new and poorly studied companions in the ( $T_{{\rm eff}}$ , $M_{{\rm H}}$ ) plane together with the PMS evolutionary tracks and isochrones of Baraffe et al. (1998). The components are placed in the diagram using their $M_{{\rm H}}$ and assuming coevality with the closest component of the system.
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In the text

$\begin{figure} \par\includegraphics[width=2.4cm,clip]{5545fa1a.ps}\hspace*{3mm} ... ...a1e.ps}\hspace*{3mm} \includegraphics[width=2.4cm,clip]{5545fa1f.ps}\end{figure}$ Figure A.1: Result of the PSF-subtraction of RW Aur B in Br $\gamma$ ( top) and [FeII] ( bottom). From left to right: primary and secondary (1/3 power stretch display) and secondary minus primary (linear stretch, upper cut is 10-sigma of the residual noise). FOV is 1 $\hbox{$.\!\!^{\prime\prime}$ }$ 4 $\times$ 1 $\hbox{$.\!\!^{\prime\prime}$ }$ 4.

In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5545fga2.ps}\end{figure}$ Figure A.2: Astrometric measurements of SR 24 C. Offset positions are shown with respect to SR 24 B. The expected position of a background star at the time of the NACO measurements (May 2004) is shown assuming it was located at the position measured by Simon et al. in August 1991.

In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{5545fga3.eps}\end{figure}$ Figure A.3: Locus of the components of the LkH $\alpha$ 346 system in the ( $T_{{\rm eff}}$ , $M_{{\rm H}}$ ) plane together with the PMS evolutionary tracks and isochrones of Baraffe et al. (1998). The components B and C are placed using their $M_{{\rm H}}$ and the assumption of coevality with either component A or D.

In the text

$\begin{figure} \par\includegraphics[width=7.35cm,clip]{5545fig1.ps}\end{figure}$	Figure 1: Distribution of separations/orbital semimajor axes of the wide binaries of our sample.
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$\begin{figure} \par\includegraphics[width=16.35cm,clip]{5545fg2a.eps}\vspace*{0.5cm}\ \includegraphics[width=16.35cm,clip]{5545fg2b.eps}\end{figure}$	Figure 2: Already known and candidate triple ( upper panel) and quadruple ( lower panel) systems detected in our VLT/NACO survey. These systems are the only apparent high-order multiple systems found in our sample, physical systems will be identified in Sect. 4.5. North is up, east is left.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5545fig3.ps}\end{figure}$	Figure 3: Relative motion in RA and Dec between the RZ93 positions and those measured in this study (NACO-RZ93). Green triangles are pairs with projected separations <150 AU.
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$\begin{figure} \par\includegraphics[width=7.5cm]{5545fig6.eps}\end{figure}$	Figure 6: Locus of new and poorly studied companions in the ( $T_{{\rm eff}}$ , $M_{{\rm H}}$ ) plane together with the PMS evolutionary tracks and isochrones of Baraffe et al. (1998). The components are placed in the diagram using their $M_{{\rm H}}$ and assuming coevality with the closest component of the system.
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