\begin{table}%t3
\caption{\label{tab: results WW Cha}Overview of the results for WW~Cha.}
%\centerline
{ \small \begin{tabular}{lcccc}
 \hline \hline
Obs. date & Wavelength & Flux$^{a}$ & rms$^{a}$ & Beam size$^{b}$	\\
& (mm)  & (mJy) & (mJy/beam) & (arcsec)			\\
 \hline
 \multicolumn{5}{c}{ATCA 7 mm band} \\
% \hline
 5 Oct 2007	& 7.0		& $5.41\pm0.32$			& $0.313$	& $11 \times 11$		\\
 5 Oct 2007	& 7.3		& $3.93\pm0.29$			& $0.350$	& $11 \times 11$		\\
 31 Mar 2008	& 7.0		& $5.10\pm0.19$			& $0.231$	& $5.8 \times 5.3$		\\
 31 Mar 2008	& 7.3		& $5.19\pm0.17$			& $0.194$	& $6.1 \times 5.6$		\\
 \hline	
 \multicolumn{5}{c}{ATCA 12 mm band}\\
 %\hline
 8 May 2006 & 16.1 & $1.16\pm0.31$ & $0.329$ & $23 \times 6$\\
 8 May 2006 & 16.2 & $1.04\pm0.30$ & $0.158$ & $23 \times 6$\\
 13 Oct. 2006 & 16.1 & $<$0.921	 & $0.307$ & $25 \times 9$\\
 13 Oct. 2006	& 16.2 & $1.08\pm0.21$ & $0.217$ & $26 \times 9$ \\
 18 Oct. 2006	& 16.1 & $0.81\pm0.20$& $0.222$& $38 \times 7$\\
 18 Oct. 2006	& 16.2 & $1.23\pm0.19$ & $0.110$	& $39 \times 7$\\
 24 Oct. 2007 	& 15.4 & $1.01\pm0.16$ & $0.209$	& $12 \times 8$\\
 24 Oct. 2007 	& 16.2 & $0.95\pm0.13$& $0.181$	& $13 \times 9$\\
 2 Nov. 2007	& 15.4 & $0.55\pm0.20^{c}$ & $0.125$ & $1.9 \times 1.3$\\
 2 Nov. 2007	& 16.2 & $0.48\pm0.13^{c}$ & $0.089$ & $2.0 \times 1.4$\\
 31 Mar. 2008  & 15.4 & $0.88\pm0.12$ & $0.232$ & $14 \times 13$ \\
 31 Mar. 2008	 & 16.2 & $1.07\pm0.10$& $0.227$& $15 \times 13$\\
 \hline
 \multicolumn{5}{c}{ATCA 3~cm band}\\
 %\hline
 18 Oct. 2006& 34.7& $<$0.222& $0.074$	& $71 \times 20$	 \\
 9 June 2007	& 34.7 & $0.63\pm0.06$ & $0.076$ & $53 \times 16$\\
 \hline
 \multicolumn{5}{c}{ATCA 6 cm band}\\
% \hline
 18 Oct. 2006	& 62.5 & $<$0.202	 & $0.067$ & $125 \times 32$\\
 9 June 2007	& 62.5 & $<$0.399	 & $0.133$ & $91 \times 26$\\
\hline
\end{tabular}}
\medskip
$^{a}$ Continuum fluxes are from point-source fits in the ($u, v$) plane. If the source was not detected at  3$\sigma$, a 3$\sigma$ upper limit is quoted. rms calculated from the cleaned image; $^{b}$~restored beam, using natural weighting. Note that the exact beam size depends 		on frequency and location of the source in the sky, as well as on the time of the observations,
 over which time range the data were taken, and exactly which data/baselines were included; 
$^{c}$~the 16~mm values from the 2~November 2007 data were obtained with antenna 6~included, causing the significantly lower point-source flux. Note that a Gaussian fit recovers the full flux, indicating that the source is probably extended.
\end{table}