\begin{table}%t1
%\centering
\par
\caption{\label{table1}Properties of the brightest compact W43~sources.}
\tiny \begin{tabular}{lcccccccc}
\hline\hline \noalign{\smallskip}
Source & $S_{70}$ & $S_{160}$ & $S_{250}$ & $S_{350}$ & $S_{500}$ & $T$(K)\tablefootmark{a} & $L / {[{10^4~L_{\odot}}]}$\tablefootmark{b}   &  $M/{[{10^3~M_{\odot}}]}$\tablefootmark{c} \\
\hline
MM1          &  128  &  1943   & 1000  &  340   & 136   & 25 & 3.0  &   2.6--4.0 \\
MM2          &  154  &  1400   &   700  &  246   & 164   & 23  & 1.5  &  3.5--5.3  \\
MM3          &  277  &  1255   & (400)  & 153   &   89   &  27 & 2.0   & 1.5--2.3 \\
MM4          &  670  &  1148   &   205   & 131   &  53    &  28  & 2.0  & 0.9--1.3 \\
\hline
\end{tabular}
\tablefoot{\tablefoottext{a}{Temperatures are determined from single grey body fits assuming an emissivity $\beta = 2$, and excluding the 70~$\mu$m data points.}
\tablefoottext{b}{Fluxes are in Jy.  Luminosities only include flux from  60~$\mu$m to 600~$\mu$m and are based on fluxes within a Hi-GAL resolution element.}
\tablefoottext{c}{Masses estimated from $\lambda$ = 500 $\mu$m in a 37\arcsec\ beam,  assuming  OH94 opacities at $t = 10^5$~years, $n = 10^6$~cm$^{-3}$ for thin ice mantles  (first number) and un-evolved MRN dust with no mantles (second number).}}
\vspace*{-2mm}
\end{table}