\begin{table}%t5
%\centering
\par
\caption {\label{TabCoverStats}Sky coverage (15~months survey, average per frequency).} 
\begin{tabular}{lccccc}
 \hline\hline  \noalign{\smallskip}
Frequency & Mean\tablefootmark{a} &
Low\tablefootmark{b} &
High\tablefootmark{c}&
Deep\tablefootmark{d} &
Pol. Stat.\tablefootmark{e}  \\
(GHz) &(s/sq. deg.) & (\%) & (\%) & (\%) & (\%) \\
 \hline
30  & 953 & 4.5 & 1.7 & 0.42 & 0.8 \\
44  & 953  & 3.3   & 1.5  & 0.28  & 3.7  \\
100  & 953 & 4.3 & 1.5 & 0.41 & 0.61 \\
353  & 953 & 4.3 & 1.2 & 0.37 & 0.10 \\
\hline
\end{tabular}
\tablefoot{\tablefoottext{a}{Integration time per square degree for typical channels.}\tablefoottext{b}{Fraction of the sky with integration time lower than one-half the mean value.}\tablefoottext{c}{Fraction of the sky with integration time higher than four times the mean value.}\tablefoottext{d}{Fraction of the sky with integration time higher than nine times the mean value.}\tablefoottext{e}{Fraction of the sky which has a high spread of scanning angles, for all detectors at each frequency. The value is based on dividing the 2$\pi$ range of angles into 
16~bins; for a pixel on the sky, the spread is considered high if there are samples in at least 5~bins. More details are
available in Dupac \& Tauber (\cite{Dupac05}).}}
\vspace*{-2mm}\end{table}