All Figures

$\begin{figure} \par\includegraphics[height=6.2cm, width=6.5cm]{WMAP_counts_int.ps}\end{figure}$ Figure 1: Integral counts of extragalactic sources in the WMAP K-band (centered at 22.8 GHz).
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In the text

$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{WMAP_lat_distr.ps}\end{figure}$ Figure 2: Surface density of WMAP extragalactic sources as a function of Galactic latitude.
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In the text

$\begin{figure} \par\includegraphics[height=6.2cm, width=6.6cm]{WMAP_zdistr_FSRQ.ps}\end{figure}$ Figure 3: Redshift distribution of WMAP FSRQs (histogram) compared with the best-fit model (solid line).
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In the text

$\begin{figure} \par\includegraphics[height=6.2cm, width=6.2cm]{WMAP_counts_FSRQ.ps}\end{figure}$ Figure 4: Differential counts of WMAP FSRQs compared with the best-fit model (solid line).
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In the text

$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{PS18_Waldram_counts.ps}\end{figure}$ Figure 5: Comparison of the model (solid line) with the differential 15 GHz counts from the main survey (filled circles) and the deeper survey (filled squares) by Waldram et al. (2003) and with total differential counts at 18 GHz by Ricci et al. (2004; crosses).
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In the text

$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{qJy_counts_FSRQ.ps}\end{figure}$ Figure 6: Counts of FSRQs in the Parkes quarter-Jy sample compared with the best-fit model (solid line).
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In the text

$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{qJy_counts_BLL.ps}\end{figure}$ Figure 7: Counts of BL Lac objects in the Parkes quarter-Jy sample compared with the best-fit model (solid line).
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In the text

$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{qJy_z_FSRQ.ps}\end{figure}$ Figure 8: Redshift distribution of FSRQs in the Parkes quarter-Jy sample (histogram) compared with the best-fit model (solid line).
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In the text

$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{KUHR_z_FSRQ.ps}\end{figure}$ Figure 9: Redshift distribution of FSRQs in the Kühr et al. (1981) sample (histogram) compared with the best-fit model (solid line).
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In the text

$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{Pauliny_Gregory_counts.ps}\end{figure}$ Figure 10: Differential counts at 5 GHz compared with the best-fit model (solid line). Data from Gregory & Condon (1991, asterisks) and Pauliny-Toth et al. (1978a, diamonds; 1978b, triangles).
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In the text

$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{PS18_flat_counts.ps}\end{figure}$ Figure 11: Differential counts at 18 GHz of flat-spectrum sources by Ricci et al. (2004) compared with the best-fit model (solid line).
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In the text

$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{Peacock_Toffol_LLF.ps}\end{figure}$ Figure 12: Local luminosity functions at 2.7 GHz by Peacock (1985) (crosses) and Toffolatti et al. (1987) (asterisks) compared with the best-fit model (solid line).
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In the text

$\begin{figure} \par\includegraphics[height=10.5cm, width=12.5cm]{total_counts_20GHz_quater.ps}\end{figure}$ Figure 13: Predicted differential counts at 20 GHz for various extragalactic source populations. Upper left-hand panel (classical radio sources): FSRQs (dotted line); BL Lacs (dashed line); steep-spectrum sources (triple dot-dashed line). Upper right-hand panel (special sources): ADAFs (dotted line); extreme GPS quasars and galaxies (dashed line); GRB afterglows (dot-dashed line). Lower left-hand panel (star-forming galaxies): proto-spheroids (dotted line); spirals (dot-dashed line); starburst galaxies (dashed line). Lower right-hand panel: SZ effects on galactic scales (dotted line) and on cluster scales (dashed line). The sum of contributions shown in each panel and the overall total counts are indicated by a thin and thick solid line, respectively.
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In the text

$\begin{figure} \par\includegraphics[height=10.5cm, width=12.5cm]{total_counts_30GHz_quater.ps}\end{figure}$ Figure 14: Same as in Fig. 13, but at 30 GHz.
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In the text

$\begin{figure} \par\includegraphics[height=6.2cm, width=6.5cm]{WMAP_counts_int.ps}\end{figure}$	Figure 1: Integral counts of extragalactic sources in the WMAP K-band (centered at 22.8 GHz).
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$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{WMAP_lat_distr.ps}\end{figure}$	Figure 2: Surface density of WMAP extragalactic sources as a function of Galactic latitude.
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$\begin{figure} \par\includegraphics[height=6.2cm, width=6.6cm]{WMAP_zdistr_FSRQ.ps}\end{figure}$	Figure 3: Redshift distribution of WMAP FSRQs (histogram) compared with the best-fit model (solid line).
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$\begin{figure} \par\includegraphics[height=6.2cm, width=6.2cm]{WMAP_counts_FSRQ.ps}\end{figure}$	Figure 4: Differential counts of WMAP FSRQs compared with the best-fit model (solid line).
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$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{PS18_Waldram_counts.ps}\end{figure}$	Figure 5: Comparison of the model (solid line) with the differential 15 GHz counts from the main survey (filled circles) and the deeper survey (filled squares) by Waldram et al. (2003) and with total differential counts at 18 GHz by Ricci et al. (2004; crosses).
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$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{qJy_counts_FSRQ.ps}\end{figure}$	Figure 6: Counts of FSRQs in the Parkes quarter-Jy sample compared with the best-fit model (solid line).
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$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{qJy_counts_BLL.ps}\end{figure}$	Figure 7: Counts of BL Lac objects in the Parkes quarter-Jy sample compared with the best-fit model (solid line).
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$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{qJy_z_FSRQ.ps}\end{figure}$	Figure 8: Redshift distribution of FSRQs in the Parkes quarter-Jy sample (histogram) compared with the best-fit model (solid line).
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$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{KUHR_z_FSRQ.ps}\end{figure}$	Figure 9: Redshift distribution of FSRQs in the Kühr et al. (1981) sample (histogram) compared with the best-fit model (solid line).
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$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{Pauliny_Gregory_counts.ps}\end{figure}$	Figure 10: Differential counts at 5 GHz compared with the best-fit model (solid line). Data from Gregory & Condon (1991, asterisks) and Pauliny-Toth et al. (1978a, diamonds; 1978b, triangles).
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$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{PS18_flat_counts.ps}\end{figure}$	Figure 11: Differential counts at 18 GHz of flat-spectrum sources by Ricci et al. (2004) compared with the best-fit model (solid line).
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$\begin{figure} \par\includegraphics[height=6cm, width=6cm]{Peacock_Toffol_LLF.ps}\end{figure}$	Figure 12: Local luminosity functions at 2.7 GHz by Peacock (1985) (crosses) and Toffolatti et al. (1987) (asterisks) compared with the best-fit model (solid line).
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$\begin{figure} \par\includegraphics[height=10.5cm, width=12.5cm]{total_counts_30GHz_quater.ps}\end{figure}$	Figure 14: Same as in Fig. 13, but at 30 GHz.
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