\begin{table}%t2
\caption{\label{tab:lmc_sampling}LMC globular cluster structural and photometric properties.}
%\centering
 \small \begin{tabular}{c c c c c c c c c c}
\hline  \hline \noalign {\smallskip}
Name & $r_{h}$    & $r_{t}$ &$K_{r_{t}}$ & $K_{20}$ &
$L_{\rm mosaic}$ & $R_{\rm int}$ & $K_{M06}$ & $(J-K)_{M06}$ & $(H-K)_{M06}$\\ 
(1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9) & (10)\\
\hline \noalign{\smallskip}
NGC~1754 & 11\farcs2  &  142\farcs9 & 9.01 & 10.21 & $2.7 \times10^{4}$ &  20$\arcsec$ & -- & -- & --\\
NGC~2005 &  8\farcs65 & 98\farcs8   & 8.92 &  9.80 & $3.9\times10^{4}$ &  20$\arcsec$ & -- & -- & --\\
NGC~2019 &  9\farcs72 & 121\farcs6  & 8.31 &  9.21 & $6.7\times10^{4}$ &  20$\arcsec$ & -- & -- & --\\
NGC~1806 &  -- &  -- & 7.57 &  9.19 & $3.4\times10^{4}$ & 100$\arcsec$ & 7.076 & 1.055 & 0.271\\ 
NGC~2162 & 21\farcs37 & 197\farcs2  & 9.65 & 11.18 & $0.5\times10^{4}$ & 120$\arcsec$ & 9.071 & 1.253 & 0.372\\ 
NGC~2173 & 34\farcs35 & 393\farcs5  & 8.86 & 10.69 & $0.9\times10^{4}$ &  60$\arcsec$ & 9.050 & 1.033 & 0.297\\
\hline
\end{tabular}
\tablefoot{(1) Cluster name; (2) half-light radius and; (3)~tidal radius of the King-model cluster fit from the catalogue of \citet{mclaughlin05};
(4)~\mbox{$K$-band} integrated magnitude within the tidal radius from
\citet{pessev06}. For NGC~1806, where $r_{t}$ is unknown, we list the
magnitude within 200$\arcsec$ radius. The same applies for NGC~2173,
because aperture equal to the tidal radius does not exist; (5)~\mbox{$K$-band} magnitude from \citet{pessev06} with aperture radius 20$\arcsec$, which matches reasonably well our central SINFONI mosaics; (6)~sampled bolometric luminosity within the clusters central mosaics in $L_{\sun}$, computed following Eq.~(\ref{eq:puzia}); (7)~integration radius, to which we have added stars from the additional bright AGB star sample; (8), (9) and (10)~photometry with the fixed aperture radius of 90$\arcsec$ of \citet{muc06}.}\vspace*{3mm}
\end{table}