\begin{table}%t2
%\centering
\par
\caption {\label{WMAPpeakdata}WMAP peak flux densities in the Magellanic Clouds.}
\begin{tabular}{cccccccccccc}
\hline\hline
\noalign{\smallskip}
         &\multicolumn{8}{c}{LMC}&\multicolumn{3}{c}{SMC}\\
Pos\tablefootmark{a} &1+2+3&4&6&7&8&9&10&12&1&2&3\\
Name\tablefootmark{b} & 30~Dor\tablefootmark{c} & N~206&N~77-94&Bar& N~11 & N~44 & N~48  & N~57  &Wing&NE&SW\\
\noalign{\smallskip}     
\hline
\noalign{\smallskip}
$\nu$ & \multicolumn{11}{c}{Flux densities} \\
(GHz)     & \multicolumn{11}{c}{Jy}\\
\noalign{\smallskip}     
\hline
\noalign{\smallskip}
 23      & 55 (72)  &  3.3 &  6.4 &  5.2 &  6.6 &  4.1 &  3.2 &  4.8 &  2.5 &  7 &  7\\
 31      & 57 (72)  &  3.6 &  6.6 &  5.2 &  7.5 &  4.5 &  2.9 &  5.1 &  3   &  9 &  8\\
 41      & 57 (71)  &  4.2 &  6.9 &  5.5 &  7.9 &  4.9 &  2.8 &  5.3 &  4   & 10 & 10\\
 61      & 58 (74)  &  6.7 &  8.7 &  6.5 & 10.5 &  6.8 &  2.8 &  6.7 &  8   & 16 & 16\\
 93      &101 (198) & 13.1 & 19.1 & 10.5 & 19.3 & 13.3 &  4.0 & 11.5 & 19   & 34 & 35\\
\noalign{\smallskip}
\hline
\end{tabular}
\par
\tablefoot {\tablefootmark{a}{Position numbers correspond to DIRBE position numbers in
Table~\ref{DIRBEpeakdata}, but area covered is not
identical.} 
\tablefootmark{b}{Object identifies the most prominent feature within the
aperture, usually an HII region complex.} 
\tablefootmark{c}{Numbers in the first
column are flux densities with local background level subtracted;
numbers in the second column, between parentheses, are flux densities
as measured by integrating over the aperture without background
subtraction.}} 
\end{table}