\begin{table}%t1
   \caption{\label{tab:sources}\label{tab1}Class~0 source sample.}
   \small%\centering
\par
\begin{tabular}{lccccccc}
\hline
\hline\noalign{\smallskip}
 {Source}  & $\alpha$ (J2000)& $\delta$ (J2000)& SFR\tablefootmark{1} & Distance\tablefootmark{2} & $M_{\rm{env}}$ & $L_{\rm{bol}}$ & Ref.\tablefootmark{3}\\
 {} & {} & {} & {} & (pc) & ($M_{\odot}$) & ($L_{\odot}$) & \\
% {} & {} & {} &  &  & & & \\
\hline
{L1448-C} & 03:25:38.87 & $+$30:44:05.4  & Perseus & 250 & 1.6 & 5 & (a) \\
{NGC~1333-IRS2A}& 03:28:55.58 & $+$31:14:37.1 & Perseus & 250 & 1.7 & 10 & (b)\\
{IRAM~04191}& 04:21:56.91 & $+$15:29:46.1 & Taurus & 140 & 0.5--1.5 & 0.1 & (c) \\
{L1527}& 04:39:53.90 & $+$26:03:10.0 & Taurus & 140 & 0.8--1.7 & 1.6& (a), (d) \\
{L1521-F} & 04:28:38.99 & $+$26:51:35.6 & Taurus & 140 & 0.7--4 & 0.1 & (e), (f)\\
\hline
\end{tabular}
\tablefoot{\tablefoottext{1}{Star Forming Region with which the Class~0 object is associated.}
\tablefoottext{2}{Recent estimates of the distance to Perseus range from 220 to~350~pc. 
Throughout this paper, we adopt a distance of~250~pc for the Perseus molecular cloud \citep{Enoch06}.} 
\tablefoottext{3}{References for the adopted values of $M_{\rm{env}}$ and $L_{\rm{bol}}$: (a)~\citet{Motte01a}; (b)~\citet{Jorgensen07b}; (c)~\citet{Andre99}; (d)~\citet{Ohashi97a}; (e)~\citet{Bourke06}; (f)~\citet{Crapsi04}.}}\vspace{4mm}
\end{table}