\begin{table}%t3
%\centering
 {\small
    \caption {{\label{scaling}Scaling parameters of NGC~6266, 47~Tuc, M~28, M~4, M~71, NGC~6366, M~55, and NGC~288.}}
\begin{tabular}{lccccc cccccc}
    \hline \hline
    \noalign{\smallskip}
      (1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9) & (10) & (11) & (12) \\
      Cluster &
      log $\rho_0$ &
      $r_{\rm c}$ &
      $d$ &
      $M_{\rm V}$ &
      $\Gamma$ &
      $M_{\rm h}$ &
      Source & 
      Background &
      Member & 
      IDs. &
      Reference\tablefootmark{a} \\
      &
      ($L_\odot ~{\rm pc}^{-3}$) &
      (\arcsec) &
      (kpc) &&&&&&&&\\
\hline
    NGC~6266  & 5.14  & 10.8 & 6.9 & $-$9.19 &  37.07 & 8.24 & 51 & 2--3 & 48--49 & 2\tablefootmark{c} & 1, 2, 3 \\
    47~Tuc       & 4.81 & 24.0 & 4.5 & $-$9.4 & 24.91 & 10.0 & 79 & $\sim$16 & $63\pm4$ & 53-63 & 4 \\
    M~28         &  4.75 & 14.4 & 5.6 & $-$8.33 & 11.29 & 3.73 & 26 & 2--3 & 23--24 & 2\tablefootmark{c} & 1, 5 \\ 
    M~4           & 4.01 & 49.8 & 1.73 & $-$6.9 & 1.0 & 1.0 & 6 & 1--3 & 3--5 & 5 & 1, 6 \\
    M~71           & 3.05 & 37.8 & 4.0 & $-$5.6 & 0.11 & 0.30 & 14 & 1--7 & 10~$\pm$~3 & 4--9 & 7  \\
    NGC~6366 & 2.42 & 109.8 & 3.6 & $-$5.77 & 0.08 & 0.33 & 5 & 2--5 & $1^{+2}_{-1}$ & $\sim$1 & 8 \\
    M~55         & 2.15 & 169.8 & 5.3 & $-$7.6  & 0.18 & 1.82 & 16 & 5--12 & $8^{+3}_{-4}$ & 2--4 & 8 \\ 
    NGC~288\tablefootmark{b}   & 1.80 & 85.0 & 8.4 & $-$6.7 & 0.03 & 0.83 & 11 & 4-11 & $4^{+3}_{-4}$ & 2-5 & 9 \\
\hline
\end{tabular}}
\par
\tablefoot {Columns~2--5 give the values for central density ($\rho_0$), core-radius
      ($r_{\rm c}$), distance ($d$), and absolute visual magnitude
      ($M_{\rm V}$) come from \citet[ version of February 2003]{1996harris}. 
      For M~4, the values of $\rho_0$ and $M_{\rm V}$ are computed for
      the distance and reddening of Richer et~al.~(1997). Columns~6 and~7 are the 
      collision number, which is computed from $\Gamma \equiv \rho_0^{1.5}\
      r_{\rm c}^2$ and the half mass from $M_{\rm h} \propto
      10^{-0.4M_V}$ \citep{2006kong}. Values for $\Gamma$ and $M_{\rm h}$
      are normalized to the value of M~4. Column~8 shows the total number of sources detected within 
      the half-mass radius. Column~9 is the number of expected fore/background sources. 
      Column~10 gives the number of expected cluster members plus error.
      Column~11 shows the number of X-ray sources (with $L_{\rm X,0.5{-}6.0~keV} > 4\times10^{30}$~erg~s$^{-1}$) 
      which have optical or/and radio counterparts associated with the cluster, or spectrally confirmed qLMXBs.
      The last column gives the reference paper. These globular clusters are ordered 
      on the central density. \\
\noindent
\tablefoottext{a}{For each cluster, the basic data for this table were extracted from: 1. \citet{2003pooley}; 2. \citet{2008cocozza}; 
3. \citet{2007trepl}; 4. \citet{2005heinke}; 5. \citet{2003becker}; 6. \citet{2004bassa}; 7. this work; 8. \citet{2008bassa}; 
9. \citet{2006kong}.}
\tablefoottext{b}{NGC~288 was not observed long enough to reach this luminosity limit of $L_{\rm X} \sim 4.0 \times 10^{30}$ 
erg~s$^{-1}$ in the 0.5--6.0~keV range. Its limiting luminosity is $\sim$$ 5.7 \times 10^{30}$~erg~s$^{-1}$. 
However, we keep this cluster's data, as a lower limit, since we have so few constraints on low-density clusters.}
\tablefoottext{c}{No information about the optical counterparts to X-ray sources.}}
\end{table}