\begin{table}%t2
\caption{\label{table2}Flux measurements at 92~cm (unless otherwise noted) for detections and nondetections of GCRT~J1745-3009 at~$\alpha$~$=$ ${\rm 17h45m5.15s}$,\protect $\delta$~$=$ $-30\degr09\arcmin52.7\arcsec$ \citep{Kaplan}. Corrections for primary beam attenuation and bandwidth smearing have been applied where appropiate.}
\small%\centerline
 {
\begin{tabular}{c c c c c c c}
\hline \hline
No. & Date             & Telescope & Peak flux density  & Error on fit & rms noise & Resolution \\
    & (yymmdd)         & (+conf.)  & (mJy/beam)         & (mJy/beam)   & (mJy/beam)& ($\arcsec\times \arcsec$) \\
\hline
1   & 860329           &  VLA A    &   --49              & 27           & 18        &  $10\times 4$ \\
2   & 860805           &  VLA B    & --19                & 20           & 100$^{{\rm 1}}$       & $44\times 33$  \\   
3   & 861226           &  VLA C    & --26                & 29           & 100$^{{\rm 1}}$        & $105\times 54$ \\
4   & 881203           &  VLA A    & --18                &  15          & 15        &  $12\times 6$ \\
5   & 890318           & VLA B     & 41                 & 19           & 8         & $27\times 14$  \\
6   & 020930           & VLA CnB   & 110$^{{\rm 2}}$& 8$^{{\rm 2}}$          & 8$^{{\rm 3}}$        & $44\times 36$ \\
7   & 050324           & WSRT      & 5                  & 4            & 4         & $148\times 27$ \\
8   & 050514           & WSRT (21 cm)&--0.3               & 0.2          & 0.2       & $68\times 9$  \\
\hline
\end{tabular}}
\medskip
$^{{\rm 1}}$ The formal rms noise levels in these two maps are 19~mJy~${\rm beam^{-1}}$ and 69~mJy~${\rm beam^{-1}}$ for the 1986~August~5 and December~26 observations respectively, (much) lower than the indicated value of 100~mJy~${\rm beam^{-1}}$. However, many bright compact sources that should be detectable in these maps, are not due to the very poor uv coverage of this observation. We accounted for this by replacing the rms~noise by a higher number, in this way giving a very crude representation of these missing sources. \\
$^{{\rm 2}}$~Here we did not tie the clean beam fit to the position from \citet{Kaplan}, but set the AIPS task ``IMFIT'' to solve for peak flux density as well as position in the residual image. \\
$^{{\rm 3}}$~This is the average noise in the residual image.
\end{table}