\begin{table}%t2
\caption{Radio flux densities of the {\it Coronet} sources.}
\small%\centerline
{
\begin{tabular}{lll}
\hline
\hline
\noalign{\smallskip}
Source ID        & 2005 flux density$^1$  & 1998 flux density$^2$\\
                 & [mJy]              & [mJy]                \\
\hline
IRS 2            & $0.49 \pm 0.02$    & 0.29--0.36           \\
Source 5         & $1.14 \pm 0.02$    & 0.40--1.21           \\
IRS 5N           & $0.06 \pm 0.02$    & 0.10$^3$             \\
IRS 5            & $0.68 \pm 0.02$    & 0.75--3.28           \\
IRS 6            & $0.07 \pm 0.02$    & 0.15                 \\
IRS 1            & $0.42 \pm 0.02$    & 0.36--0.59           \\
R CrA            & $0.30 \pm 0.02$    & 0.16--0.26           \\
%Source 9         & $1.61 \pm 0.02$    & 0.86                 \\
IRS 7W$^4$       & $5.33 \pm 0.02$    & 4.11--5.29           \\
IRS 7E           & $1.77 \pm 0.02$    & 1.38--2.10           \\
\hline
\label{vlaresults}
\end{tabular}}
\smallskip
$^1$ Quoted errors are from Gaussian fitting. Our flux scale has an absolute uncertainty of $\sim$$15$\%; \\
$^2$ minima and maxima (if source detected in single epochs), see \citet{for05}; \\
$^3$ note that this source is not called IRS~5N in \citet{for05} but is No. 5 in the tables; \\
$^4$ blended with Source 9. \\
\end{table}