**Table 10:** Pixel-space fits of the B03 maps with a combination of a CMB template (from WMAP) and a dust template (from IRAS), see Eq. (39). For the three upper rows, the fit has been performed in the deep survey region ( $74\hbox {$^\circ $ }<\rm RA < 90\hbox {$^\circ $ }$ ; $-50\hbox {$^\circ $ }< {\rm Dec} < -40\hbox {$^\circ $ }$ , $\langle \vert b\vert \rangle \sim 32\hbox{$^\circ$ }$ , for a total of 2172 15 $^\prime$ 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 ( $90\hbox {$^\circ $ }< {\rm RA} < 105\hbox {$^\circ $ }$ ; $-50\hbox {$^\circ $ }< {\rm Dec} < -40\hbox {$^\circ $ }$ , $\langle \vert b\vert \rangle \sim 23\hbox{$^\circ$ }$ , 2027 pixels of 15 $^\prime$ ). 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.
Frequency	R(A)	R(B)	$B[\mu {\rm K}/\rm (MJy/sr)]$	$\langle \Delta T_{\rm dust}^2 \rangle^{1/2} (\mu \rm K)$
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	$(202 \pm 18)$	$50 \pm 5$
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	$(183 \pm 24)$	$104 \pm 14$

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