All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{AA3402fig1.ps}\end{figure}$ Figure 1: The Spectral Energy Distribution of different types of Blazars represented by Synchrotron-Self-Compton models with emission peaking at different energies. LBL sources are those where the synchrotron peak is located at Infra-Red frequencies and therefore their X-ray emission is due to Inverse Compton radiation. HBL Blazars are those where the synchrotron component peaks in the UV/X-ray band making their $f_{\rm x}/f_{\rm r}$ flux ratio hundreds or thousands of times higher than that of LBLs.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{AA3402fig2.ps} \par\end{figure}$ Figure 2: The radio (5 GHz) ${\rm Log}N-{\rm Log}S$ of Blazars built combining several radio and multi-frequency surveys. The different symbols represent the surveys used (see text for details). The filled square symbols in the lower part of the diagram represent the ${\rm Log}N-{\rm Log}S$ of extreme HBL BL Lacs from the Sedentary Survey. Although these objects are a tiny minority ( $\approx$ 0.1%) of the overall Blazar population they play an important role in producing the Cosmic Background at X-ray and at very high energies ( $\gamma$ -ray/TeV).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{AA3402fig3.ps}\end{figure}$ Figure 3: The high Galactic Latitudes (|b| > 20) sky coverage of the RASS survey in the region of overlap with the NVSS catalog (Dec > -40 degrees).
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{AA3402fig4.eps}\end{figure}$ Figure 4: The $f_{\rm x}/f_{\rm r}$ distribution of Blazars estimated from the 1 Jy-ANR and from a sample of about 2000 HBL Blazar candidates (see text for details).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{AA3402fig5.ps}\end{figure}$ Figure 5: The extragalactic Cosmic Background Energy distribution at microwave, X-ray and $\gamma$ -ray energies.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{AA3402fig6.ps}\end{figure}$ Figure 6: The Blazar fractional contamination of the CMB (solid line) and the apparent increase in CMB temperature due to Blazars (dotted line) as a function of frequency.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{AA3402fig7.ps}\end{figure}$ Figure 7: The contribution of Blazars to the CMB fluctuation spectrum in the WMAP Q channel at 41 GHz as evaluated from the ${\rm Log}N-{\rm Log}S$ given in Fig. 2 (solid line). We also show the angular power spectrum for the Blazar population by adding an estimate of the possible contribution of radio sources with steep-spectrum at low radio frequencies which flatten at higher frequencies (dashed line). The dotted line includes also the effect of spectral and flux variability (see text for details). Although this additional contamination may be substantial a precise estimation can only be done through simultaneous high resolution observations at the same frequency. A typical CMB power spectrum evaluated in a $\Lambda$ CDM cosmology with $\Omega _{\rm m}=0.3, \Omega _{\Lambda }=0.65, \Omega _b=0.05$ which best fits the available data is shown forcomparison.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{AA3402fig8.ps}\end{figure}$ Figure 8: The contribution of Blazars to the CMB fluctuation spectrum as in Fig. 7 for the WMAP 94 GHz channel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{AA3402fig9.ps}\end{figure}$ Figure 9: The distribution of spectral slopes between the microwave (94 GHz) and X-ray (1 keV) band measured from the sample of 42 Blazars included in the WMAP catalog of bright microwave sources detected in the 94 GHz channel and for which X-ray measurements are available.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{AA3402fig10.ps}\end{figure}$ Figure 10: The possible contribution of LBL Blazars to the Hard X-ray/soft $\gamma$ -ray Background (shaded area). The three SSC curves corresponds to different $\nu _{\rm peak}$ values (log $\nu _{\rm peak}= 12.8$ , 13.5 and 13.8) and are constrained to go through the three star symbols representing 1) the total contribution of Blazars at 94 GHz ( $8\times 10^{-6}$ of the CMB intensity), 2) the average 5 GHz to 94 GHz slope ( $\alpha_{5-94~{\rm GHz}}$ = 0.2) and 3) the average spectral slope between 94 GHz and 1 keV ( $\langle$ $\alpha _{\mu x}$ $\rangle = 1.07$ ).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{AA3402fig11.ps}\end{figure}$ Figure 11: The CMB, X-ray and $\gamma$ -ray cosmic backgrounds with superimposed the SED of the Blazar 3C 279 scaled so that its flux at 94 GHz matches the cumulative emission of the entire Blazar population (encircled star symbol).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{AA3402fig12.ps}\end{figure}$ Figure 12: The possible contribution of LBL Blazars to the $\gamma$ -ray Cosmic Background (shaded area). Simple SSC energy distributions fail to reproduce the observed intensity and slope of the $\gamma$ -ray Background. The observed range of $\gamma$ -ray emission with EGRET, normalized to radio flux, indicates that the duty cycle at these energies must be low (see text for details).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{AA3402fig13.ps}\end{figure}$ Figure 13: The CMB, X-ray and $\gamma$ -ray cosmic backgrounds with superimposed the SED of MKN 421 scaled to 1/1000 of the total Blazar contribution to the CMB since the radio ${\rm Log}N-{\rm Log}S$ of extreme HBL like this source (in the sedentary survey) is about 1/1000 of the ${\rm Log}N-{\rm Log}S$ of all Blazars.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{AA3402fig14.ps}\end{figure}$ Figure 14: The SED of the Blazar 3C 279 scaled down by a factor of 1000 (1 milli-3C 279) with superimposed the sensitivity of microwave (Planck LFI+HFI), X-ray (Swift XRT-XMM-Chandra) and $\gamma$ -ray (GLAST-LAT) satellites. A Blazar of this flux, or about 10 mJy at radio frequencies, would still be detected by Planck, by existing optical and X-ray satellites (Swift, XMM or Chandra) and would be above the GLAST limiting sensitivity during strong flares.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{AA3402fig3.ps}\end{figure}$	Figure 3: The high Galactic Latitudes (\|b\| > 20) sky coverage of the RASS survey in the region of overlap with the NVSS catalog (Dec > -40 degrees).
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{AA3402fig4.eps}\end{figure}$	Figure 4: The $f_{\rm x}/f_{\rm r}$ distribution of Blazars estimated from the 1 Jy-ANR and from a sample of about 2000 HBL Blazar candidates (see text for details).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{AA3402fig5.ps}\end{figure}$	Figure 5: The extragalactic Cosmic Background Energy distribution at microwave, X-ray and $\gamma$ -ray energies.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{AA3402fig6.ps}\end{figure}$	Figure 6: The Blazar fractional contamination of the CMB (solid line) and the apparent increase in CMB temperature due to Blazars (dotted line) as a function of frequency.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{AA3402fig8.ps}\end{figure}$	Figure 8: The contribution of Blazars to the CMB fluctuation spectrum as in Fig. 7 for the WMAP 94 GHz channel.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{AA3402fig9.ps}\end{figure}$	Figure 9: The distribution of spectral slopes between the microwave (94 GHz) and X-ray (1 keV) band measured from the sample of 42 Blazars included in the WMAP catalog of bright microwave sources detected in the 94 GHz channel and for which X-ray measurements are available.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{AA3402fig11.ps}\end{figure}$	Figure 11: The CMB, X-ray and $\gamma$ -ray cosmic backgrounds with superimposed the SED of the Blazar 3C 279 scaled so that its flux at 94 GHz matches the cumulative emission of the entire Blazar population (encircled star symbol).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{AA3402fig12.ps}\end{figure}$	Figure 12: The possible contribution of LBL Blazars to the $\gamma$ -ray Cosmic Background (shaded area). Simple SSC energy distributions fail to reproduce the observed intensity and slope of the $\gamma$ -ray Background. The observed range of $\gamma$ -ray emission with EGRET, normalized to radio flux, indicates that the duty cycle at these energies must be low (see text for details).
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{AA3402fig13.ps}\end{figure}$	Figure 13: The CMB, X-ray and $\gamma$ -ray cosmic backgrounds with superimposed the SED of MKN 421 scaled to 1/1000 of the total Blazar contribution to the CMB since the radio ${\rm Log}N-{\rm Log}S$ of extreme HBL like this source (in the sedentary survey) is about 1/1000 of the ${\rm Log}N-{\rm Log}S$ of all Blazars.
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