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$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{0116fig1a.ps} \includegraphics[angle=90,width=8.3cm,clip]{0116fig1b.ps}\end{figure}$ Figure 1: Synchrotron and dust (effective powerlaw) spectral indices evaluated between 30 and 44 GHz, and 143 and 217 GHz respectively (in $\mu$ K $_{\rm RJ}$ ). A spatially varying spectral index corresponds to a foreground morphology that varies with frequency.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{0116fig2a.ps} \includegraphics[angle=90,width=8.5cm,clip]{0116fig2b.ps} \end{figure}$ Figure 2: Upper panel: hit counts for the 143 GHz channel. The inhomogeneities at the ecliptic poles are characteristic of PLANCK's cycloidal scanning strategy. Lower panel: the masking scheme separating the sky in three regions of different foreground contamination. The grey region at high Galactic latitudes is Zone 1, covering $f_{{\rm sky}}=74\%$ . The darker region at lower Galactic latitudes is Zone 2 and covers $f_{{\rm sky}}=22\%$ . The remaining region (green) along the Galactic ridge is Zone 3. The point source mask (red) covers $4\%$ of Zone 1. The SZ mask (yellow) cuts detected SZ clusters at Galactic latitudes above 20 degrees, covering $1.4\%$ of sky.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0116fig3a.ps} \includegraphics[width=8.5cm,clip]{0116fig3b.ps} \end{figure}$ Figure 3: Spectra of the simulated microwave sky components near the foreground minimum. CMB, noise with the effect of beam deconvolution, and the thermal SZ effect are evaluated on the full sky; point source power is evaluated on Zone 1 + 2 both with and without sources above 200 mJy masked; the galaxy power spectra are evaluated on Zone 1 and on Zone 2. The well-known importance of masking is evident, as is the fact that there is a significant proportion of sky (Zone 2, $f_{{\rm sky}}=22\%$ ) for which Galactic emission is comparable to CMB power.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0116fig4a.ps}\\ [2.5mm] \includegraphics[width=8.5cm,clip]{0116fig4b.ps} \end{figure}$ Figure 4: Upper: rms of the residual error of the CMB map, calculated for each of 18 bands of 10 degrees width in Galactic latitude. For comparison, $\sigma_{{\rm CMB}}=104.5~\mu$ K and $\sigma_{{\rm noise}}=29.3~\mu$ K, for the 143 GHz channel alone (1.7' pixels). Lower: rms of this residual map calculated at 45' resolution. For comparison, $\sigma_{{\rm CMB}}(45')=69.8~\mu$ K and $\sigma_{{\rm noise}}(45')=0.7~\mu$ K for the 143 GHz channel. The corresponding residual maps are shown in Fig. 5.
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In the text

$\begin{figure} \par\begin{tabular}{cc} \includegraphics[angle=90,scale=0.35, wi... ...[angle=90,scale=0.35, width=8.5cm,clip]{0116fig5h} \end{tabular}\par\end{figure}$ Figure 5: CMB reconstruction error smoothed at 45' resolution. These maps are described in Sect. 4.1, and their rms in Galactic latitude strips of $10^{\circ }$ are shown in Fig. 4. Over a large fraction of sky, the typical rms of the residual error is between 2 and 5 $\mu$ K, which can be compared with $\sigma_{{\rm CMB}}(45')=69.8~\mu$ K and $\sigma_{{\rm noise}}(45')=0.7~\mu$ K for the 143 GHz channel. Some contamination from the galactic components and bright clusters remains.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{0116fig6a.ps} }\\ [2mm] {\includegraphics[width=8cm,clip]{0116fig6b.ps} } \end{figure}$ Figure 6: Spectra of the CMB residual maps, evaluated on Zone 1 ( high Galactic latitudes) and Zone 2 ( low Galactic latitudes), both regions with point sources masked. Comparison with Fig. 3 shows the extent to which the Galactic contamination has been removed from the CMB on large angular scales.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{0116fig7a.ps} } {\include... ....ps} }\\ [2.5mm] {\includegraphics[width=8cm,clip]{0116fig7c.ps} } \end{figure}$ Figure 7: Upper: power spectrum estimates (PSE) using Commander on large angular scales. The diamonds show the $C_{\ell }$ of the input CMB realisation. Middle: PSE of the recovered CMB map using the SMICA method. Lower: PSE compared with the estimates derived from the input CMB $C_{\ell }$ , and with the expected PLANCK sensitivity, assuming $f_{\rm sky}=0.8$ . Beyond $\ell =500$ biases in the PSE set in in some of the methods.
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In the text

$\begin{figure} \par\begin{tabular}{cc} \includegraphics[scale=0.5]{0116fig8a} & \includegraphics[scale=0.5]{0116fig8b}\end{tabular}\par\end{figure}$ Figure 8: Patch of the recovered needlet-ILC SZ map and input SZ map. For easier comparison of the two maps ( $12.5\times 12.5$ deg), the input SZ map has been filtered to the same resolution as the output.
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In the text

$\begin{figure} \par\begin{tabular}{cc} \includegraphics[angle=90, scale=0.31]{01... ....5]{0116fig9e} & \includegraphics[scale=0.5]{0116fig9f}\end{tabular}\end{figure}$ Figure 9: Example input and recovered total galaxy emission at 23 GHz, dust at 143 GHz and CMB components.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{0116fig1a.ps} \includegraphics[angle=90,width=8.3cm,clip]{0116fig1b.ps}\end{figure}$	Figure 1: Synchrotron and dust (effective powerlaw) spectral indices evaluated between 30 and 44 GHz, and 143 and 217 GHz respectively (in $\mu$ K $_{\rm RJ}$ ). A spatially varying spectral index corresponds to a foreground morphology that varies with frequency.
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$\begin{figure} \par {\includegraphics[width=8cm,clip]{0116fig6a.ps} }\\ [2mm] {\includegraphics[width=8cm,clip]{0116fig6b.ps} } \end{figure}$	Figure 6: Spectra of the CMB residual maps, evaluated on Zone 1 ( high Galactic latitudes) and Zone 2 ( low Galactic latitudes), both regions with point sources masked. Comparison with Fig. 3 shows the extent to which the Galactic contamination has been removed from the CMB on large angular scales.
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$\begin{figure} \par\begin{tabular}{cc} \includegraphics[scale=0.5]{0116fig8a} & \includegraphics[scale=0.5]{0116fig8b}\end{tabular}\par\end{figure}$	Figure 8: Patch of the recovered needlet-ILC SZ map and input SZ map. For easier comparison of the two maps ( $12.5\times 12.5$ deg), the input SZ map has been filtered to the same resolution as the output.
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$\begin{figure} \par\begin{tabular}{cc} \includegraphics[angle=90, scale=0.31]{01... ....5]{0116fig9e} & \includegraphics[scale=0.5]{0116fig9f}\end{tabular}\end{figure}$	Figure 9: Example input and recovered total galaxy emission at 23 GHz, dust at 143 GHz and CMB components.
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