\begin{table}%t4
\caption{Properties of intermediate-mass outflows.}
\label{toutflows}
%\centerline
{\begin{tabular}{lcccc}
\hline\hline 
&\multicolumn{1}{c}{$M$}&
\multicolumn{1}{c}{$P$}&
\multicolumn{1}{c}{$E$}&
\multicolumn{1}{c}{$\dot P$}
\\
\multicolumn{1}{c}{Outflow}&
\multicolumn{1}{c}{($M_\odot$)}&
\multicolumn{1}{c}{($M_\odot$ \kms)}&
\multicolumn{1}{c}{($10^{45}$ erg)}&
\multicolumn{1}{c}{($M_\odot ~ \mbox{km s}^{-1}$~yr$^{-1}$)}
\\
\hline\noalign{\smallskip}
 IRAS 20050+2720$^{a}$ &1.7 &25.4\phantom{1} &7.7 &${\sim} 5.0\times10^{-3}\phantom{13}$\\
 IRAS 21391+5802$^{b}$ &\phantom{1}0.14 &3.6 &1.2 &$1.4\times10^{-3}$ \\
 HH288$^{c}$ &11 &385 &6.7 &$1.4\times10^{-2}$ \\
 L1641S$^{d}$ &1.4 &37 &0.3 &$5.3\times10^{-4}$ \\
 NGC 2071$^{e}$ &10 &81 &8.5 &$5.1\times10^{-3}$ \\
\hline
\end{tabular}}
\medskip
\par
$^a$ The parameters correspond to the whole emission of the different outflow lobes detected in 
IRAS~20050+2720 (Bachiller et~al.~\cite{bachiller95}). 
$^b$ Beltr\'an et~al.~(\cite{beltran02}). 
$^c$ Because of the difficulty of treating each outflow separately, the parameters correspond to the whole
emission, thus including the two outflows detected in HH228 (Gueth et~al.~\cite{gueth01}). 
$^d$ Anglada~(\cite{anglada95}) and Wu et~al.~(\cite{wu04}).
$^e$ Snell et~al.~(\cite{snell84}).
\end{table}