**Table 4:** Upper limits for the relative brightness of undetected companions to both components of the binaries in our survey, measured at 0 $\hbox{$.\!\!^{\prime\prime}$ }$ 07, 0 $\hbox{$.\!\!^{\prime\prime}$ }\!$ 15 and 0 $\hbox{$.\!\!^{\prime\prime}$ }$ 5, as well as the limiting magnitudes at large separations.
$\begin{displaymath}{ { \begin{tabular}{l@{\hspace{2mm}}r@{~$\pm$~}l@{\hspace{2mm... ..... & & ... & ... & ... && 14.6 & ... \\ \hline \end{tabular}}}\end{displaymath}$ ^a Assumes as for the triples/quadruples that the primary is the brightest component in Br $\gamma$ and [FeII], for respectively the first and second data set. ^b Components inverted with respect to RZ93, given the above assumption. Notes: Separations and PAs are computed from aperture photometry and the uncertainties combine the rms variations over the individual frames and the uncertainties due to the plate scale and detector orientation.

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