All Figures

$\begin{figure} \par\includegraphics[height=8.8cm,width=4.7cm,angle=90,clip]{8435f01.ps} \end{figure}$ Figure 1: Angular power spectra of the Galactic plane cut-offs ( $\vert b_{\rm gal}\vert \ge b_{\rm cut}$ ) at radio frequencies. Each line refers to a certain $b_{\rm cut}$ ( from the bottom: black $\to 40^{\circ }$ , fuchsia $\to 50^{\circ }$ , green $\to 60^{\circ }$ ).
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm,height=8.5cm,angle=90,clip]{8435f02.ps}\end{figure}$ Figure 2: Comparison between the cut-off angular power spectra of the original (fuchsia lines at the top) and destriped (blue) version of the 408 MHz map. The cut-off angular power spectra of the difference map are also shown (green lines at the bottom).
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In the text

$\begin{figure} \par\begin{tabular}{c} \includegraphics[width=4.5cm,angle=90]{84... ...ncludegraphics[width=4.5cm,angle=90]{8435f03b.ps}\\ \end{tabular} \end{figure}$ Figure 3: Mollweide projection of the HEALPix maps produced at 408 MHz ( top) and 1420 MHz ( bottom) by subtracting the discrete sources. The maps are in Galactic coordinates. The center of the maps is l = 0 , b = 0. The Galactic longitude increases toward the left up to $180^{\circ }$ .
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In the text

$\begin{figure} \par\begin{tabular}{cc} \includegraphics[width=2.3cm,angle=90,cl... ... & \includegraphics[width=3cm,clip]{8435f04f.ps}\\ \end{tabular} \end{figure}$ Figure 4: HEALPix maps of the Galactic plane cut-offs extracted from the 1.4 GHz all-sky map after DS subtraction. A mollweide projection is displayed for the cuts with $\vert b_{\rm cut}\vert\le 20^{\circ }$ and a gnomonic view (centered on a Galactic pole) for those with $\vert b_{\rm cut}\vert\ge 40^{\circ }$ .
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In the text

$\begin{figure} \par\begin{tabular}{cc} \includegraphics[width=2.3cm,angle=90,cl... ... & \includegraphics[width=3cm,clip]{8435f05f.ps}\\ \end{tabular} \end{figure}$ Figure 5: As in Fig. 4, but at 408 MHz.
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm,height=8.8cm,angle=90,clip]{8435f06.ps} \end{figure}$ Figure 6: APS of some Galactic plane cut-off for the 1420 MHz maps: (from the top in each panel) original ( $\to$ fuchsia), after discrete source subtraction ( $\to$ blue) and DSs only ( $\to$ green).
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm,height=8.8cm,angle=90,clip]{8435f07.ps} \end{figure}$ Figure 7: As in Fig. 6, but at 408 MHz.
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In the text

$\begin{figure} \par\includegraphics[width=4cm,height=8.5cm,angle=90,clip]{8435f08.ps} \end{figure}$ Figure 8: Angular power spectra of the northern ( $b_{\rm gal} \ge b_{\rm cut}\;\to$ left panel) and southern ( $b_{\rm gal} \le -b_{\rm cut}\;\to$ right) cuts for the map of discrete sources at 1420 MHz. Color legend (see online version): black (dotted) $\to \vert b_{\rm cut}\vert=5^{\circ }$ , black $\to \vert b_{\rm cut}\vert=10^{\circ }$ , green $\to \vert b_{\rm cut}\vert=20^{\circ }$ , red $\to \vert b_{\rm cut}\vert=30^{\circ }$ , dark blue $\to \vert b_{\rm cut}\vert=40^{\circ }$ , fuchsia $\to \vert b_{\rm cut}\vert=50^{\circ }$ , light blue $\to \vert b_{\rm cut}\vert=60^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[height=8.5cm,angle=90,clip]{8435f09.ps} \end{figure}$ Figure 9: Comparison between the APS of the cuts for the DS-subtracted map at 1420 MHz. The left (respec. right) panels display the angular power spectra of the northern (respec. southern) cuts. First (respec. second) row panels: $b_{\rm cut}=5^{\circ }{-}40^{\circ }$ (respec. $b_{\rm cut}=40^{\circ }{-}60^{\circ }$ ). Color legend (see online version): black dotted $\to \vert b_{\rm cut}\vert=5^{\circ }$ , black $\to \vert b_{\rm cut}\vert=10^{\circ }$ , green $\to \vert b_{\rm cut}\vert=20^{\circ }$ , red $\to \vert b_{\rm cut}\vert=30^{\circ }$ , dark blue $\to \vert b_{\rm cut}\vert=40^{\circ }$ , fuchsia $\to \vert b_{\rm cut}\vert=50^{\circ }$ , dark green $\to \vert b_{\rm cut}\vert=60^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=3.8cm,height=8.6cm,angle=90,clip]{8435f10.ps} \end{figure}$ Figure 10: Comparison between the angular power spectra of the northern ( $b_{\rm gal} > b_{\rm cut}$ , $\to$ blue - upper lines) and southern ( $b_{\rm gal} < -b_{\rm cut}$ $\to$ red - lower) cuts for the DS-subtracted map at 1420 MHz.
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In the text

$\begin{figure} \par\includegraphics[width=5.7cm,height=8.8cm,angle=90,clip]{8435f11.ps} \end{figure}$ Figure 11: Angular power spectra of the northern ( top panels) and southern cuts ( bottom) for the DS-subtracted map at 1420 MHz together with the best fit curves obtained. The individual contributions of synchrotron emission (blue lines) and of sources (green lines) are also plotted (smoothed by the beam).
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In the text

$\begin{figure} \par\includegraphics[width=5.7cm,height=8.8cm,angle=90,clip]{8435f12.ps} \end{figure}$ Figure 12: As in Fig. 11, but at 408 MHz.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=4.2cm,height=4.4cm,clip]{8435f13... ...m} \includegraphics[width=4.2cm,height=4.4cm,clip]{8435f13b.ps} } \end{figure}$ Figure 13: Best-fit parameters obtained for the Galactic radio synchrotron emission APS against Galactic latitude.
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,height=8.7cm,angle=90,clip]{8435f14.ps} \end{figure}$ Figure 14: Angular power spectra of the DS-subtracted radio maps (green $\to$ 408 MHz, fuchsia $\to$ 1420 MHz) extrapolated to 23 GHz for a direct comparison with those of the WMAP 3-yr DS-subtracted synchrotron component (blue). The radio angular power spectra have been smoothed to $1^{\circ }$ to match the angular resolution of the 23 GHz map. The frequency spectral indices adopted in the extrapolation are $\beta_{(0.408-23)~{\rm GHz}}=-2.95$ and $\beta_{(1.4-23)~{\rm GHz}}=-2.90$ for the northern cut and $\beta_{(0.408-23)~{\rm GHz}}=-2.90$ and $\beta_{(1.4-23)~{\rm GHz}}=-2.83$ for the southern one.
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In the text

$\begin{figure} \par\includegraphics[width=5.4cm,height=8cm,angle=90,clip]{8435f15.ps} \end{figure}$ Figure 15: Mean angular power spectra, $\langle C_{\ell}(\nu)\rangle_{\ell\in[20,40]}$ , of high latitude cuts ( $b_{\rm cut} = \pm 40^{\circ }$ ) against frequency. The straight line defined by the mean APS of the two lower frequencies is also plotted.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,height=13cm,angle=90,clip]{8435f16.ps}\end{figure}$ Figure 16: Comparison between the CMB APS retrieved by Hinshaw et al. (2007) and the synchrotron angular power spectra derived for some cuts of the 1420 MHz map (from Table 1 and Fig. 11), extrapolated to 30 GHz and 70 GHz with a spectral index of -2.9. Color legend (see online version): blue (upper straight lines) $\to$ $C_{\ell }^{\rm N}$ (northern cut), red (lower) $\to$ $C_{\ell }^{\rm S}$ (southern cut). The left panels also display the APS for the all-sky (black line) extrapolated as above. The empty square in the top right panel marks the upper limit on synchrotron contamination inferred from COBE-DMR observations (Kogut et al. 1996).
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In the text

$\begin{figure} \par\includegraphics[width=3.8cm,height=8.8cm,angle=90,clip]{8435f17.ps} \end{figure}$ Figure 17: Comparison between the angular power spectra derived using Anafast (fuchsia) and via integration of the correlation function. Some examples of good ( left panel), fair and poor ( right) agreement are shown for the map at 1420 MHz after DSs subtraction.
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In the text

$\begin{figure} \par\begin{tabular}{@{}ccc@{}} Fit no SRC & Best Model & Fit no ... ...idth=3.9cm,height=5.9cm,angle=90]{8435f18j.ps} & \\ \end{tabular} \end{figure}$ Figure 18: Maps of the best fit parameters obtained by fitting the angular power spectra of the local analysis patches at 1420 MHz. The maps aligned along each row refer to the same parameter. From the top, ${\rm log}(k_{100}^{\rm synch}/{\rm mK}^2)$ , $\alpha ^{\rm synch}$ , ${\rm log} (c^{\rm src}/{\rm mK}^2)$ and ${\rm log}(c^{\rm noise}/{\rm mK}^2)$ . The first and third columns correspond to the extreme cases, assuming respectively that the source contribution or the noise contamination is negligible.
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In the text

$\begin{figure} \begin{tabular}{@{}ccc@{}} Fit no SRC & Best Model & Fit no Noi... ...th=3.8cm,height=5.8cm,angle=90]{8435f19j.ps} & \\ \end{tabular} \end{figure}$ Figure 19: As in Fig. 18, but at 408 MHz.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,height=7.3cm,angle=90,clip]{8435f20.ps} \end{figure}$ Figure 20: Correlation between the best fit values obtained for the synchrotron emission APS normalized amplitude (k₁₀₀) at 408 MHz and 1420 MHz.
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In the text

$\begin{figure} \par\includegraphics[height=8.8cm,width=4.7cm,angle=90,clip]{8435f01.ps} \end{figure}$	Figure 1: Angular power spectra of the Galactic plane cut-offs ( $\vert b_{\rm gal}\vert \ge b_{\rm cut}$ ) at radio frequencies. Each line refers to a certain $b_{\rm cut}$ ( from the bottom: black $\to 40^{\circ }$ , fuchsia $\to 50^{\circ }$ , green $\to 60^{\circ }$ ).
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$\begin{figure} \par\includegraphics[width=5.2cm,height=8.5cm,angle=90,clip]{8435f02.ps}\end{figure}$	Figure 2: Comparison between the cut-off angular power spectra of the original (fuchsia lines at the top) and destriped (blue) version of the 408 MHz map. The cut-off angular power spectra of the difference map are also shown (green lines at the bottom).
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$\begin{figure} \par\begin{tabular}{c} \includegraphics[width=4.5cm,angle=90]{84... ...ncludegraphics[width=4.5cm,angle=90]{8435f03b.ps}\\ \end{tabular} \end{figure}$	Figure 3: Mollweide projection of the `HEALPix` maps produced at 408 MHz ( top) and 1420 MHz ( bottom) by subtracting the discrete sources. The maps are in Galactic coordinates. The center of the maps is l = 0 , b = 0. The Galactic longitude increases toward the left up to $180^{\circ }$ .
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$\begin{figure} \par\begin{tabular}{cc} \includegraphics[width=2.3cm,angle=90,cl... ... & \includegraphics[width=3cm,clip]{8435f04f.ps}\\ \end{tabular} \end{figure}$	Figure 4: `HEALPix` maps of the Galactic plane cut-offs extracted from the 1.4 GHz all-sky map after DS subtraction. A mollweide projection is displayed for the cuts with $\vert b_{\rm cut}\vert\le 20^{\circ }$ and a gnomonic view (centered on a Galactic pole) for those with $\vert b_{\rm cut}\vert\ge 40^{\circ }$ .
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$\begin{figure} \par\begin{tabular}{cc} \includegraphics[width=2.3cm,angle=90,cl... ... & \includegraphics[width=3cm,clip]{8435f05f.ps}\\ \end{tabular} \end{figure}$	Figure 5: As in Fig. 4, but at 408 MHz.
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$\begin{figure} \par\includegraphics[width=5.2cm,height=8.8cm,angle=90,clip]{8435f06.ps} \end{figure}$	Figure 6: APS of some Galactic plane cut-off for the 1420 MHz maps: (from the top in each panel) original ( $\to$ fuchsia), after discrete source subtraction ( $\to$ blue) and DSs only ( $\to$ green).
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$\begin{figure} \par\includegraphics[width=5.2cm,height=8.8cm,angle=90,clip]{8435f07.ps} \end{figure}$	Figure 7: As in Fig. 6, but at 408 MHz.
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$\begin{figure} \par\includegraphics[width=3.8cm,height=8.6cm,angle=90,clip]{8435f10.ps} \end{figure}$	Figure 10: Comparison between the angular power spectra of the northern ( $b_{\rm gal} > b_{\rm cut}$ , $\to$ blue - upper lines) and southern ( $b_{\rm gal} < -b_{\rm cut}$ $\to$ red - lower) cuts for the DS-subtracted map at 1420 MHz.
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$\begin{figure} \par\includegraphics[width=5.7cm,height=8.8cm,angle=90,clip]{8435f11.ps} \end{figure}$	Figure 11: Angular power spectra of the northern ( top panels) and southern cuts ( bottom) for the DS-subtracted map at 1420 MHz together with the best fit curves obtained. The individual contributions of synchrotron emission (blue lines) and of sources (green lines) are also plotted (smoothed by the beam).
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$\begin{figure} \par\includegraphics[width=5.7cm,height=8.8cm,angle=90,clip]{8435f12.ps} \end{figure}$	Figure 12: As in Fig. 11, but at 408 MHz.
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$\begin{figure} \par\mbox{\includegraphics[width=4.2cm,height=4.4cm,clip]{8435f13... ...m} \includegraphics[width=4.2cm,height=4.4cm,clip]{8435f13b.ps} } \end{figure}$	Figure 13: Best-fit parameters obtained for the Galactic radio synchrotron emission APS against Galactic latitude.
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$\begin{figure} \par\includegraphics[width=5.4cm,height=8cm,angle=90,clip]{8435f15.ps} \end{figure}$	Figure 15: Mean angular power spectra, $\langle C_{\ell}(\nu)\rangle_{\ell\in[20,40]}$ , of high latitude cuts ( $b_{\rm cut} = \pm 40^{\circ }$ ) against frequency. The straight line defined by the mean APS of the two lower frequencies is also plotted.
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$\begin{figure} \par\includegraphics[width=3.8cm,height=8.8cm,angle=90,clip]{8435f17.ps} \end{figure}$	Figure 17: Comparison between the angular power spectra derived using `Anafast` (fuchsia) and via integration of the correlation function. Some examples of good ( left panel), fair and poor ( right) agreement are shown for the map at 1420 MHz after DSs subtraction.
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$\begin{figure} \begin{tabular}{@{}ccc@{}} Fit no SRC & Best Model & Fit no Noi... ...th=3.8cm,height=5.8cm,angle=90]{8435f19j.ps} & \\ \end{tabular} \end{figure}$	Figure 19: As in Fig. 18, but at 408 MHz.
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$\begin{figure} \par\includegraphics[width=5cm,height=7.3cm,angle=90,clip]{8435f20.ps} \end{figure}$	Figure 20: Correlation between the best fit values obtained for the synchrotron emission APS normalized amplitude (k₁₀₀) at 408 MHz and 1420 MHz.
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