\begin{table}%tB.1
\caption{Observations in millimetre wavelengths from the Plateau du Bure interferometer 
(compact 6-antenna configuration on all dates). The errors are based on 
point-source fits in the UV~plane to the phase center.}\label{tabB.1}
\small%\centerline
{
\begin{tabular}{c c c c }
\hline\hline
 ($t-t_0$) (days)&Band (GHz)& Flux (mJ)   & 3-$\sigma$ limit (mJy)\\
\hline
 3.23           &  86.789  & 0.0 $\pm$ 0.3 & 0.9          \\
 3.23           & 229.068  & 1.0 $\pm$ 1.6 & 4.8          \\
 5.19           & 115.477  & 0.5 $\pm$ 0.8 & 2.5          \\
 5.19           & 232.295  & 3.3 $\pm$ 1.8 & 5.4          \\
 10.34	        & 86.251   & 0.9 $\pm$ 0.3 & 0.9$^a$ \\
 10.34 	        & 232.171  & 8.4 $\pm$ 2.3 & 6.9$^a$\\
 11.19	        & 108.995  & --1.7 $\pm$ 1.7& 5.2\\
 11.19         	& 228.534  & --9.9 $\pm$ 6.5& 19.5\\
 12.40          & 108.995  & --0.9 $\pm$ 0.7& 2.2           \\
 12.40          & 228.534  & 3.6 $\pm$ 2.7 & 8.2           \\
 14.29          & 111.619  & --0.8 $\pm$ 0.4& 1.3           \\
 14.29          & 224.680  & 1.4 $\pm$ 2.1 & 6.3           \\
\hline
\end{tabular}}
\medskip
$^a$ The faint detections found on this epoch are considered to be due to a~statistical fluctuation or to an~unusual event of interstellar scattering at high galactic latitud, taking into account the 
non detection the next night and the extreme spectral slope.
\end{table}