\begin{table}%t10
%\centering
\small 
\caption{Pixel-space fits of the \bk\ maps with a
combination of a CMB template (from \wmap) and a dust template
(from IRAS), see Eq.~(\ref{eq:bestfit}). For the three upper rows,
the fit has been performed in the deep survey region ($74\degr <\rm  RA
< 90\degr$; $-50\degr < {\rm Dec} < -40\degr$, $\langle |b| \rangle \sim 32\degr$,
for a total of 2172 15\arcmin\ pixels). In this region, the rms
fluctuation of the IRAS/DIRBE map is 0.25~MJy/sr. For the three
lower rows, the fit has been done in the part of the Shallow
Survey closer to the Galactic Plane ($90\degr < {\rm RA} < 105\degr$; 
$-50\degr < {\rm Dec} < -40\degr$, $\langle |b| \rangle \sim 23\degr$, 2027 pixels of~15\arcmin). Here the rms fluctuation of the IRAS/DIRBE map is 0.57~MJy/sr. $R(A)$ is the 
correlation coefficient for the CMB
template, while~$R(B)$ is the correlation coefficient for the dust
template. The last column gives the estimated brightness
fluctuation due to the ISD component correlated to the IRAS/DIRBE
map, in CMB temperature units. \label{tab:fitwmapiras} }
\begin{tabular}{ccccc}
\hline\hline
\noalign{\smallskip}
Frequency & $R(A)$ & $R(B)$  & $B[\mu {\rm K}/\rm (MJy/sr)]$ & $ \langle \Delta T_{\rm dust}^2 \rangle^{1/2} (\mu \rm K) $ \\[-3mm]\\
\hline 
145 GHz & 0.634 &  0.074 & $(18 \pm 23) $ & $< $10         \\
245 GHz & 0.452 &  0.173 & $(49 \pm 21) $ & $12 \pm 5$   \\
345 GHz & 0.331 &  0.452 & $(202 \pm 18)$ & $50 \pm 5$   \\
\hline
145 GHz & 0.588 & --0.085 & $(-5 \pm 9)  $ & $< $5        \\
245 GHz & 0.273 &  0.143 & $(37 \pm 11)  $ & $21 \pm 6$    \\
345 GHz & 0.123 &  0.380 & $(183 \pm 24)$ & $ 104 \pm 14 $\\
\hline
\end{tabular}
\end{table}