\begin{table}%t2
\caption{\label{sources}Photometric and derived properties of candidate
  clusters in~NGC~6872.  The complete list is available in electronic form
at the CDS.
 }
%\centerline
{{
\begin{tabular}{c c c c c c c c c c c c c c c c}    
\hline\hline
id & $x$ & $y$ & $U^{a}$ & d$U $& $B^{a}$ & d$B$ & $V^{a}$ & d$V$ & $I^{a}$ & d$I$ & $\chi^{2}_{\nu}$$^{b}$ & $A_{\rm V}$$^{c}$ & log (Age/yr)$^{c}$ & log Mass/$M_{\odot}$$^{c}$ & $M_{\rm V}$$^{d}$ \\ 
\hline
  2  &    120.6  &    164.0  &    23.25  &     0.17  &    23.05  &     0.04  &    22.27  &     0.03  &    21.37  &     0.04  &     2.00  &     0.00  &     9.48  &     6.89  &   --11.63  \\
  6  &    189.0  &    178.2  &    22.55  &     0.11  &    23.34  &     0.07  &    23.58  &     0.09  &    22.90  &     0.10  &     7.60  &     0.19  &     7.20  &     5.11  &   --10.51  \\
 10  &    215.5  &    197.7  &    22.05  &     0.09  &    22.58  &     0.05  &    22.73  &     0.07  &    22.50  &     0.09  &     1.80  &     0.06  &     6.64  &     4.59  &   --11.23  \\
 14  &     40.4  &    236.0  &    20.94  &     0.03  &    20.89  &     0.01  &    20.46  &     0.01  &    19.77  &     0.03  &     0.80  &     0.00  &     8.96  &     7.20  &   --13.44  \\
 16  &     71.0  &    240.8  &    21.83  &     0.07  &    22.21  &     0.03  &    22.28  &     0.04  &    21.96  &     0.06  &     6.80  &     0.25  &     6.62  &     4.79  &   --11.87  \\
 19  &    201.0  &    265.4  &    22.09  &     0.08  &    22.54  &     0.03  &    22.61  &     0.04  &    22.13  &     0.06  &     9.20  &     0.19  &     6.88  &     4.95  &   --11.48  \\
 20  &    159.4  &    273.8  &    22.75  &     0.17  &    23.14  &     0.08  &    23.07  &     0.09  &    22.15  &     0.07  &     3.10  &     0.74  &     7.30  &     5.52  &   --11.57  \\
\hline
\end{tabular}}}
\smallskip
$^{{a}}$ Magnitudes have only been corrected for foreground extinction.\\
$^{{b}}$ The reduced $\chi^{2}$ value for the best fitting model.\\
$^{{c}}$ Derived extinction, age, and mass using the {\it 3DEF} method.  Sources with ages greater than~1~Gyr are most likely foreground stars.\\
$^{{d}}$ Absolute magnitue of the source, correcting for the derived extinction.
\end{table}