All Figures

$\begin{figure} \par\includegraphics[width=13.8cm,clip]{3020.f1} \end{figure}$ Figure 1: Aitoff map of the NVSS source density. Scales run from $2\sigma$ below (black) to $2\sigma$ above the mean source density (white). The region of the galactic plane with $\vert b\vert<10\hbox {$^\circ $ }$ is indicated by solid lines. Besides the expected enhancement of the source density due to the large population of galactic radio sources, the NVSS catalogue suffers from large numbers of spurious sources around bright or extended sources (white regions), as well as an overall decrease in the source density below $\delta =-10\hbox {$^\circ $ }$ (see the greyscale change at $\delta =-10\hbox {$^\circ $ }$ ). See text and Table 1 for details.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3020.f2}\hspace*{2mm} \includegraphics[width=8.2cm,clip]{3020.f3} \end{figure}$ Figure 2: The NVSS source density as a function of declination for various flux-limited sub-samples. Below $\sim$ 10 mJy beam^-1 the source density is non-uniform due to changes in the configuration of the VLA at $\delta =-10\hbox {$^\circ $ }$ and $\delta =+78\hbox {$^\circ $ }$ (dotted lines).
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In the text

$\begin{figure} \par\includegraphics[width=14.8cm,clip]{3020.f4} \end{figure}$ Figure 3: Aitoff map of the FIRST source density. Scales run from $2\sigma$ below (black) to $2\sigma$ above (white) the mean source density. The region of the galactic plane with $\vert b\vert<10\hbox {$^\circ $ }$ is indicated by solid lines.
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In the text

$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f5} \end{figure}$ Figure 4: The rms-noise level as a function of galactic latitude. The average rms-noise level of the survey is $\sim$ 0.48 mJy beam^-1. Dotted lines enclose the region $\vert b\vert<10\hbox {$^\circ $ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f6} \end{figure}$ Figure 5: The FIRST source density as a function of declination for various limiting flux densities.
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In the text

$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f7} \end{figure}$ Figure 6: The angular two-point correlation function of S>10 mJy NVSS sources. The power-law fits described in the text are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f8} \end{figure}$ Figure 7: The angular two-point correlation function of S>3 mJy FIRST sources. The power-law fits described in the text are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f9} \end{figure}$ Figure 8: Angular correlation functions for the flux density intervals 10<S<40 mJy and S>200 mJy. The power-law fits to the data described in the text are overplotted. Because of an unexplained "bump'' in the S>200 mJy signal at $0.1\protect\la\theta\protect\la0.3$ (connected points), the small- and large-scale correlation functions were fitted separately over the ranges $\theta \le 0.1$ and $\theta \ge 0.3$ , respectively.
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In the text

$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f10} \end{figure}$ Figure 9: The amplitude of the cosmological angular correlation function ( $\gamma =1.8$ ) of NVSS and FIRST as a function of 1.4 GHz flux density limit. For comparison, we have indicated the results for the WENSS and GB6 surveys from Rengelink (1998) and Rengelink & Röttgering (1999).
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In the text

$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f11} \end{figure}$ Figure 10: The modeled physical size distribution of S>10 mJy FRII radio galaxies in the NVSS catalogue. The source density in the linear size-redshift plane is indicated by contours to illustrate the underlying redshift distribution (darker greyscales indicate higher densities). Sources lying above the line can, in principle, be resolved given the angular resolution of the NVSS of 45 $^{\prime \prime }$ (FWHM).
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In the text

$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f12} \end{figure}$ Figure 11: The angular size distribution for FRII radio galaxies in the NVSS calculated from the modeled physical size distribution (assuming $\Omega _M=1$ ). The number of input sources was chosen to match the predicted number of FRIIs in the S>10 mJy subsample. The binsize is 1 $^{\prime \prime }$ .
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In the text

$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f13} \end{figure}$ Figure 12: The ratio of observed doubles to modeled doubles per distance interval. The angular resolution of the NVSS is indicated by the dotted line.
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In the text

$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f14} \end{figure}$ Figure 13: Dashed lines show the redshift distributions for S_1.4>10 mJy, computed from the free-form models 1-4, the pure luminosity evolution model (PLE) and the luminosity/density evolution model (LDE) of Dunlop & Peacock (1990) (see text for details). The average of the six different models is indicated by the solid curve.
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In the text

$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f15} \end{figure}$ Figure 14: The redshift distributions for S_1.4>100 mJy. See the caption of Fig. 13 for details.
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In the text

$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f16} \end{figure}$ Figure 15: Spatial correlation lengths and $1\sigma$ errors derived from the cosmological ${w(\theta )}$ of the NVSS, assuming an evolution parameter $\epsilon =-1.2$ , and the $\Lambda$ CDM model Universe. The dotted line indicates the flux density limit at which FRI- and FRII-type radio sources contribute roughly equally to 1.4 GHz radio source counts. The dashed line indicates the flux density limit above which the contribution of FRIIs is $\protect\ga$ $75\%$ . The top axis indicates the effective radio luminosity as a function of flux density limit.
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In the text

$\begin{figure} \par\includegraphics[width=\textwidth,clip]{3020.f17} \end{figure}$ Figure 16: The redshift evolution of galaxy clustering in a $\Lambda$ CDM Universe. See the text for references to data taken from literature. Lines represent the following models: (i) stable clustering ( $\epsilon =0$ ) normalized to r₀ of local ellipticals and clusters ( dotted lines), (ii) linear clustering ( $\epsilon =1$ ) normalized to 5 h^-1 Mpc ( dot-dashed line), (iii) clustering of the dark matter ( thick solid line, from Jenkins et al. 1998, see also Moustakas & Somerville 2002 for a useful parameterization), (iv) galaxy conservation model normalized to r₀ of local ellipticals ( thin solid line, see Fry 1996), (v) hierarchical model for clustering evolution of early-type galaxies normalized to r₀ of local ellipticals ( thick dashed line, from Kauffmann et al. 1999b), and (vi) clustering evolution as a function of dark matter halo masses with $\mathcal{M}_{\rm min}=10^{12{-}14}~M_\odot$ ( thin dashed lines, from Matarrese et al. 1997). A nice representation of this figure showing actual images of the various objects rather than symbols can be found at our website: http://www.strw.leidenuniv.nl/~overzier/r0.html.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3020.f2}\hspace*{2mm} \includegraphics[width=8.2cm,clip]{3020.f3} \end{figure}$	Figure 2: The NVSS source density as a function of declination for various flux-limited sub-samples. Below $\sim$ 10 mJy beam^-1 the source density is non-uniform due to changes in the configuration of the VLA at $\delta =-10\hbox {$^\circ $ }$ and $\delta =+78\hbox {$^\circ $ }$ (dotted lines).
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$\begin{figure} \par\includegraphics[width=14.8cm,clip]{3020.f4} \end{figure}$	Figure 3: Aitoff map of the FIRST source density. Scales run from $2\sigma$ below (black) to $2\sigma$ above (white) the mean source density. The region of the galactic plane with $\vert b\vert<10\hbox {$^\circ $ }$ is indicated by solid lines.
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$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f5} \end{figure}$	Figure 4: The rms-noise level as a function of galactic latitude. The average rms-noise level of the survey is $\sim$ 0.48 mJy beam^-1. Dotted lines enclose the region $\vert b\vert<10\hbox {$^\circ $ }$ .
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$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f6} \end{figure}$	Figure 5: The FIRST source density as a function of declination for various limiting flux densities.
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$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f7} \end{figure}$	Figure 6: The angular two-point correlation function of S>10 mJy NVSS sources. The power-law fits described in the text are indicated.
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$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f8} \end{figure}$	Figure 7: The angular two-point correlation function of S>3 mJy FIRST sources. The power-law fits described in the text are indicated.
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$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f10} \end{figure}$	Figure 9: The amplitude of the cosmological angular correlation function ( $\gamma =1.8$ ) of NVSS and FIRST as a function of 1.4 GHz flux density limit. For comparison, we have indicated the results for the WENSS and GB6 surveys from Rengelink (1998) and Rengelink & Röttgering (1999).
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$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f12} \end{figure}$	Figure 11: The angular size distribution for FRII radio galaxies in the NVSS calculated from the modeled physical size distribution (assuming $\Omega _M=1$ ). The number of input sources was chosen to match the predicted number of FRIIs in the S>10 mJy subsample. The binsize is 1 $^{\prime \prime }$ .
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$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f13} \end{figure}$	Figure 12: The ratio of observed doubles to modeled doubles per distance interval. The angular resolution of the NVSS is indicated by the dotted line.
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$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f14} \end{figure}$	Figure 13: Dashed lines show the redshift distributions for S_1.4>10 mJy, computed from the free-form models 1-4, the pure luminosity evolution model (PLE) and the luminosity/density evolution model (LDE) of Dunlop & Peacock (1990) (see text for details). The average of the six different models is indicated by the solid curve.
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$\begin{figure} \par\includegraphics[width=\columnwidth,clip]{3020.f15} \end{figure}$	Figure 14: The redshift distributions for S_1.4>100 mJy. See the caption of Fig. 13 for details.
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