\begin{table}%t1
%\centering
\par
\caption{\label{tdfrac}Summary of the main physical properties of selected cores in IRAS~20293+3952.}
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\begin{tabular}{lcccccccccc}
\hline\hline
\noalign{\smallskip}
& $\alpha$(J2000)& $\delta$(J2000)  &\Tex\tablefootmark{a} & &\Trot\tablefootmark{c}  & $N$(\nhtd)\tablefootmark{d} &$N$(\nh)\tablefootmark{d} &  &\nh/ &Evol.   \\
Core &(h~m~s) &($\degr$ $'$ $''$) &(K) & $\tau_{\rm m}$\tablefootmark{b} &(K)  & ($\times10^{14}$~\cmd) &($\times10^{14}$~\cmd) &$D_{{\rm frac}}$\tablefootmark{e} &\nth\tablefootmark{c}  &stage\tablefootmark{f}  \\
\hline
Western cloud  &20:31:10.70 &40:03:28.2   & $4.8\pm0.2$  &1.5  & $15\pm3$   & \php10~$\pm$~\phnp2 & \php14$\pm$~\phnp2 & $0.8\pm0.2$ &300 &PPC   \\  
BIMA~2-S &20:31:12.34 &40:03:05.7           & $5.4\pm0.3$  &1.1   & $19\pm3$   & $2.8\pm0.6$       & $6.7\pm0.8$ & $0.4\pm0.1$   &\phn90  &PPC \\
Dust ridge  &20:31:12.98 &40:03:08.5          & $4.6\pm0.3$  &1.0   & $16\pm3$  & $2.8\pm0.7$       & $4.9\pm0.9$ & $0.6\pm0.2$  &\phn90  &PPC\\
BIMA~3 &20:31:13.92 &40:03:00.9              & $5.4\pm1.0$   &0.4   & $14\pm2$  & $1.9\pm0.5$        & \php19~$\pm$~\phnp3 & $0.10\pm0.04$ &300 &PPC \\
BIMA~4    &20:31:14.56 &40:03:06.8         & $7.5\pm1.6$     &0.3   & 14$\pm2$  & $1.2\pm0.4$       & $7.4\pm0.8$ & $0.16\pm0.05$  &200  &PPC\\
BIMA~1 &20:31:12.77 &40:03:22.6 &\ldots\  &\ldots\ & $24\pm3$  &${<}1.1$\tablefootmark{g} & $19\pm3$ &${<}0.06$ &\phn50  &O, no IR\\
IRS~5 &20:31:13.41 &40:03:13.7 &\ldots\   &\ldots\  & $24\pm3$ &${<}1.5$\tablefootmark{g} & $11\pm2$ &${<}0.1$ &\phn50  &IR\\
\hline
\end{tabular}
\tablefoot{
\tablefoottext{a}{\Tex\ derived from the output parameters of the \nhtd~$1_{11}{-}1_{01}$ hyperfine fit.}
\tablefoottext{b}{Derived from the fits to the hyperfine structure of \nhtd~$1_{11}{-}1_{01}$.} \tablefoottext{c}{Obtained from \citet{palau2007}.}
\tablefoottext{d}{Column densities derived using the same $uv$ range and convolving the images to a circular beam of $7''$.} 
\tablefoottext{e}{$D_{{\rm frac}}=N$(\nhtd)/$N$(\nh).} 
\tablefoottext{f}{PPC: pre-protostellar core; O: molecular outflow.}
\tablefoottext{g}{3$\sigma$ upper limit estimated adopting $\Delta v$ from \nh\ and \Tex$=5$~K.}}
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\end{table}