\begin{table}%t1 \def\zero{\phantom{0}} \caption {\label{tab:1}The average value of foreground stars found in the various complexes.} %\centerline {\tiny \begin{tabular}{lccccc} \hline\hline \noalign{\smallskip} Complex & $N_{\rm fg}$ & Area & $\rho_{\rm fg}$ & Distance & VLBI Distance \\ & & $\mbox{deg}^2$ & $\mbox{deg}^{-2}$ & pc & pc \\ \hline Taurus & \zero75 & 1.829 & $\zero41 \pm 4\zero$ & $153 \pm 8\zero$ & $147.6 \pm 0.6$ \\ Perseus & \zero71 & 0.638 & $ 111 \pm 13 $ & $240 \pm 13 $ & $235 \pm 18$ \\ Perseus North & \zero45 & 0.336 & $ 134 \pm 20 $ & $260 \pm 18 $ \\ Perseus South & \zero26 & 0.302 & $\zero86 \pm 17 $ & $212 \pm 18 $ \\ California & 119 & 0.270 & $ 440 \pm 30 $ & $450 \pm 23 $ & --\\ \hline \end{tabular}} \tablefoot {The fourth column reports the measured distance and its 1-$\sigma$ error, as estimated from a comparison of the density of foreground stars with the \citet{2003AetA...409..523R} Galactic model (see Fig.~\ref{fig:10}); the last column reports the two VLBI distances known from the literature (\citealp{2007ApJ...671..546L}, for Taurus and \citealp{2008PASJ...60...37H}, for Perseus).} \vspace*{3mm} \end{table}