All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8453_012.ps}\end{figure}$ Figure 1: The location of the various available surveys in the XMM-LSS field. The thin, grey circles show the positions of the observed XMM X-ray pointings. The four solid thick circles show the 325 MHz pointings observed with the VLA, and the dots are at the positions of the sources detected at 325 MHz (Tasse et al. 2006) that overlap with the coverage of the CFHTLS-Wide optical data; these optical observations are indicated by the dotted lines for the T02 release and dashed lines for the T03 release. The SWIRE field is indicated by dashed lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8453_014.ps}\includegraphics[width=8.5cm,clip]{8453_015.ps}\end{figure}$ Figure 2: Left panel: the cumulative distribution of the angular distance from the radio source centroid to the closest neighbour in the optical catalog. In the simulated catalog, the magnitude cut is m_i=24, and the fraction $\theta (m)$ of radio sources having an optical counterpart is a variable. The first dash-dotted line on the left correspond to $\theta =100\%$ , while dash-dotted line on the right corresponds to $\theta =0\%$ . In this case, the best fit to the distribution of the actual data is obtained with $\theta =60\%$ . The right panel shows the best values of $\theta$ found for different limiting magnitudes. We model $\theta (m)$ as constant above i=27 and below i=17 and fit by a polynomial between these values (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8453_016.ps}\end{figure}$ Figure 3: Stellar mass distributions in the redshift range 0.1<z<1.2, for the observed radio sources' hosts (solid line) and for the estimated contribution from the misidentifications (grey dashed line). The dotted line (``Non Normalised Difference'') corresponds to the difference between these two distributions. We have used such a misidentification contribution subtraction to estimate $\theta (m,M,sS\!FR,z)$ , and give estimates of the association probabilities corrected for the misidentification contribution.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{8453_000.ps}\end{figure}$ Figure 4: The reduced $\chi ^2$ distribution of spectral fits using the SWIRE template library. The secondary bump at $\chi ^2\gtrsim 100$ shows that $\sim$ 30% of the population is not properly fit. Assuming this does not drive any selection effect, we have rejected these sources from the spectral type distribution study.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8453_001.ps}\\ [2mm] \includegraphics[width=8.8cm,clip]{8453_002.ps}\end{figure}$ Figure 5: Top panel: the g-r vs. r-i colour-colour plot for the S2 sample detected in all the u^*g'r'i'z' and IRAC bands (black dots), and for a subsample of normal galaxies similarly selected (grey dots). We classify as type-1 those objects which lie in the hashed area. The open circles indicate the classification based on the SED-type criteria (see bottom panel). We plot the colour-colour tracks for a type-1 QSO, an elliptical, and a starburst galaxy. The square, star, diamond and triangle symbols stand for redshifts 0, 0.5, 1.5, and 2 respectively. Bottom panel: the [3.6]-[4.5] versus [5.8]-[8.0] colour-colour plot for the sources of the same sample. The grey dotted line indicates the region in which Stern et al. (2005) finds $\sim$ 90% of the spectroscopically identified broad-line AGN. Based on the SWIRE template library, the objects best fit by a T1 AGN templates are plotted with small black circle. The bigger circles (``BLAGN'') indicate the sources classified as T1 AGN when progressively removing the information on the infrared and optical bands (``9 bands'': u^*g'r'i'z' + IRAC available; ``7 bands'': u^*g'r'i'z' + 5.8 and 8.0 $\mu$ m available; ``5 bands'': u^*g'r'i'z' available; ``3 bands'': g'r'i' available, see Sect. 5.1).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8453_003.ps}\end{figure}$ Figure 6: The distribution of the radio sources in the P_1.4 - SFR plane. The open circles indicate upper limits. The solid line is the SFR-P_1.4 relation given by Cram (1998). Below the dashed line, the contribution by star formation to the radio power is higher than 10%. In order to retrieve a purely radio-loud AGN sample, in the final source list, we have flagged these sources as being starburst-like.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8453_009.ps}\end{figure}$ Figure 7: For a sub-sample of sources detected at 3.6 and 4.5 $\mu$ m, we can compare the photometric redshifts as estimated using the ZPEG and the SWIRE template libraries. Here we show the cumulative distribution of $z_{\rm ZPEG}-z_{\rm SWIRE}$ for the T1 sources (``rejected'') and for the N/T2 sources (``selected''). The N/T2 sample is best fitted by a normal distribution with ${\rm sigma}=0.13$ .
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{8453_010.ps}\end{figure}$ Figure 8: In order to test the consistency of our results, we have derived the stellar mass function for normal galaxies (open diamonds and thick solid line), by using the $1/V_{\max}$ comoving number density estimator. Our estimates are in good agreement with measurements in the GOODS surveys (Fontana et al. 2006, grey dots and dash-dot line), which suggests that the stellar mass estimates are reliable for normal galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8453_011.ps}\end{figure}$ Figure 9: We compare our estimate of the radio luminosity function in 0.1<z<1.2 (open diamonds) with the Willott et al. (2001) RLF estimate (dashed line). Both the normalisation and slope are in good agreement, confirming that the photometric redshifts of the sample of N/T2 radio-loud galaxies are reliable.
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In the text

$\begin{figure} \par\mbox{\hspace*{1cm}\includegraphics[width=1.30in]{8453_019.ps... ...h=2.78in]{8453_035.ps}\includegraphics[width=1.30in]{8453_036.ps} } \end{figure}$ Figure E.1: Greyscale: the i-band image. Contours: The 325 MHz contours drawn at levels of $3\sigma _{\rm local}\times {1,1.4,2,2.8,4,...}$ . The local noise $\sigma _{\rm local}$ appears in each overlay, and is in units of mJy.beam^-1. The largest cross indicates the position of the optical identification with the highest identification probability, $p_{\max}$ . The thickness of the other crosses scales as $p/p_{\max}$ where p is the probability of identification of the given source. Small crosses indicate the positions of the Gaussian fitting components appearing in the Tasse et al. (2006) source list, used for the centroïd position calculation. On the bottom left corner of each image, the radio source morphological classification is given, as well as the flag status of the optical host in the optical catalog: Masked = 1 if the objects is masked, Star = 1 if it is point-like, and Sat. = 1 if it is saturated.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_037.ps}\includegrap... ...0in]{8453_070.ps}\includegraphics[width=1.30in]{8453_071.ps} } \par \end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\hspace*{7mm}\includegraphics[width=1.30in]{8453_072.ps... ...3_100.ps}\includegraphics[width=1.30in]{8453_101.ps}\hspace*{7mm}}\end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\hspace*{5mm}\includegraphics[width=1.30in]{8453_102.ps... ...53_130.ps}\includegraphics[width=1.30in]{8453_131.ps}\hspace*{5mm}} \end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_132.ps}\includegrap... ...h=1.30in]{8453_159.ps}\includegraphics[width=1.30in]{8453_160.ps} } \end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_161.ps}\includegrap... ...h=1.30in]{8453_182.ps}\includegraphics[width=1.30in]{8453_183.ps} } \end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_184.ps}\includegrap... ...h=1.30in]{8453_218.ps}\includegraphics[width=1.30in]{8453_219.ps} } \end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_220.ps}\includegrap... ...=1.30in]{8453_253.ps}\includegraphics[width=1.30in]{8453_254.ps} }\end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.24in]{8453_255.ps}\includegrap... ...=1.24in]{8453_288.ps}\includegraphics[width=1.24in]{8453_289.ps} }\end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_290.ps}\includegrap... ...=1.30in]{8453_309.ps}\includegraphics[width=1.30in]{8453_310.ps} }\end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_311.ps}\includegrap... ...=1.32in]{8453_338.ps}\includegraphics[width=1.30in]{8453_339.ps} }\end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_340.ps}\includegrap... ...=1.30in]{8453_375.ps}\includegraphics[width=1.30in]{8453_376.ps} }\end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\hspace*{7mm}\includegraphics[width=1.24in]{8453_377.ps... ...3_402.ps}\includegraphics[width=1.24in]{8453_403.ps}\hspace*{4cm}}\end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_404.ps}\includegrap... ...3_431.ps}\includegraphics[width=1.30in]{8453_432.ps}\hspace*{2cm}}\end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=2.93in]{8453_433.ps}\includegrap... ...3_444.ps}\includegraphics[width=1.30in]{8453_445.ps}\hspace*{8mm}}\end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_446.ps}\includegrap... ...=1.30in]{8453_473.ps}\includegraphics[width=1.30in]{8453_474.ps} }\end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_475.ps}\includegrap... ...=1.30in]{8453_510.ps}\includegraphics[width=1.30in]{8453_511.ps} }\end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_512.ps}\includegrap... ...518.ps}\includegraphics[width=1.30in]{8453_519.ps}\hspace*{5.2cm}}\end{figure}$ Figure E.1: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=1.24in]{8453_520.ps}\includegrap... ...h=1.24in]{8453_553.ps}\includegraphics[width=1.24in]{8453_554.ps} } \end{figure}$ Figure E.2: Greyscale: the i-band image. Contours: the 610 MHz contours drawn at levels of $3\sigma _{\rm local}\times {1,1.4,2,2.8,4,..}$ . The local noise $\sigma _{\rm local}$ appears in each overlay, and is in units of mJy beam^-1. The largest cross indicates the position of the optical identification with the highest identification probability, $p_{\max}$ . The thickness of the other crosses scales as $p/p_{\max}$ where p is the probability of identification of the given source. Small crosses indicate the positions of the Gaussian fitting components appearing in the Tasse et al. (2007) source list, used for the centroïd position calculation. On the bottom left corner of each image, the radio source morphological classification is given, as well as the flag status of the optical host in the optical catalog: Masked = 1 if the objects is masked, Star = 1 if it is point-like, and Sat. = 1 if it is saturated.
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In the text

$\begin{figure}\par\mbox{\includegraphics[width=1.30in]{8453_555.ps}\includegraph... ...h=1.30in]{8453_589.ps}\includegraphics[width=1.30in]{8453_590.ps} } \end{figure}$ Figure E.2: continued.
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In the text

$\begin{figure}\par\mbox{\includegraphics[width=1.30in]{8453_591.ps}\includegraph... ...h=1.30in]{8453_624.ps}\includegraphics[width=1.30in]{8453_625.ps} } \end{figure}$ Figure E.2: continued.
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In the text

$\begin{figure}\par\mbox{\includegraphics[width=1.30in]{8453_626.ps}\includegraph... ...53_636.ps}\includegraphics[width=1.30in]{8453_637.ps}\hspace*{5cm}} \end{figure}$ Figure E.2: continued.
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In the text

$\begin{figure} \par\includegraphics[width=4.8in]{8453_638.ps}\par {\hspace*{1cm}\includegraphics[width=3.8in]{8453_639.ps}\hspace*{1cm}} \end{figure}$ Figure E.3: Greyscale: the i-band image. Contours: the 325 MHz contours drawn at levels of $3\sigma _{\rm local}\times {1,1.4,2,2.8,4,..}$ . Small crosses indicate the positions of the Gaussian fitting components appearing in the Tasse et al. (2006) source list, used for the centroïd position calculation. The top panel shows the radio halo/relic candidate reported in Tasse et al. (2006). The radio source in the lower panel has a spectral index $\alpha _{1400}^{325}=-1.65$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{8453_000.ps}\end{figure}$	Figure 4: The reduced $\chi ^2$ distribution of spectral fits using the SWIRE template library. The secondary bump at $\chi ^2\gtrsim 100$ shows that $\sim$ 30% of the population is not properly fit. Assuming this does not drive any selection effect, we have rejected these sources from the spectral type distribution study.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8453_011.ps}\end{figure}$	Figure 9: We compare our estimate of the radio luminosity function in 0.1<z<1.2 (open diamonds) with the Willott et al. (2001) RLF estimate (dashed line). Both the normalisation and slope are in good agreement, confirming that the photometric redshifts of the sample of N/T2 radio-loud galaxies are reliable.
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$\begin{figure} \par\mbox{\includegraphics[width=1.30in]{8453_037.ps}\includegrap... ...0in]{8453_070.ps}\includegraphics[width=1.30in]{8453_071.ps} } \par \end{figure}$	Figure E.1: continued.
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$\begin{figure}\par\mbox{\includegraphics[width=1.30in]{8453_555.ps}\includegraph... ...h=1.30in]{8453_589.ps}\includegraphics[width=1.30in]{8453_590.ps} } \end{figure}$	Figure E.2: continued.
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