\begin{table}%t3
\par
  %\centering
\par
  \caption {\label{tab:3}The masses of the Taurus, Perseus, and California dark
    complexes. }
 %\centerline
 { \begin{tabular}{lcccc}
 \hline\hline
 \noalign{\smallskip}
    Cloud    & Distance &
    \multicolumn{3}{c}{Mass} \\
    \cline{3-5}
             &          & Total & $A_K > 0.1$ & $A_K > 0.2$ \\
    \hline
    Taurus   & $150 ~\mbox{ pc}$ & $\phantom{0}20~300 ~ { M}_\odot$
    & $\phantom{0}15~500~ \mbox{ M}_\odot$ 
    & $\phantom{0}8~300~  { M}_\odot$ \\
    Perseus  & $240 ~\mbox{ pc}$ & $\phantom{0}27~000~  { M}_\odot$
    & $\phantom{0}19~600 ~ { M}_\odot$ 
    & $\phantom{0}9~300~  { M}_\odot$ \\
    California   & $450 ~\mbox{ pc}$ & $132~000 ~ { M}_\odot$
    & $100~000 ~ { M}_\odot$ & $43~900 ~ { M}_\odot$ \\
    \hline
  \end{tabular}}
  \tablefoot {The small differences with respect to the
    results reported in Table~1 by \citet{2009ApJ...703...52L} are due to the
    different resolution of the extinction maps used.}
    \end{table}