\begin{table}%[t]%T1
    \caption{Source sample$^a$.}
    \label{tab:samp}
    %\centerline
{
    \begin{tabular}[lccccc]{lccccc}
\hline \hline
Source        & RA\ (1950)& Dec\ (1950) & $L$ & $d$ & $N$(\hh) \\
 &(h m s) & (\degr\ \arcmin\ \arcsec) & ($10^{4}$~\lsol) & (kpc) & ($10^{23}$~\scm)\\
\hline   
W3 IRS5       & 02 21 53.1 & +61 52 20 & 17 & 2.2 & 2.3 \\ 
MonR2 IRS3    & 06 05 21.5 &--06 22 26 & 1.3& 0.95 &1.8 \\
NGC 6334 IRS1 & 17 17 32.0 &--35 44 05 & 11 & 1.7 &11.3 \\
W33A          & 18 11 43.7 &--17 53 02 & 10 & 4   & 6.2 \\
AFGL 2136     & 18 19 36.6 &--13 31 40 &  7 & 2   & 1.2 \\
AFGL 2591     & 20 27 35.8 & +40 01 14 &  2 & 1   & 2.3 \\
S140 IRS1     & 22 17 41.1 & +63 03 42 &  2 & 0.9 & 1.4 \\
NGC 7538 IRS1 & 23 11 36.7 & +61 11 51 & 13 & 2.8 & 6.5 \\
NGC 7538 IRS9 & 23 11 52.8 & +61 10 59 &  4 & 2.8 & 3.3 \\
\hline
    \end{tabular}}
\par
\medskip
$^a$ Luminosity and distance from \citet{henn92} and \citet{gian97}
(MonR2 IRS3) and from \citet{fvdt00} (other sources); \hh\ column
density from this work (MonR2 IRS3) and from \citet{fvdt00} (other
sources). Column densities are 15$''$ averages and strongly beam dependent.
\end{table}