All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3979f01.ps}\end{figure}$ Figure 1: The ACS GOODS-S field with superimposed the ISAAC tiling made by ESO to cover the whole field in J and Ks. The field shown is the ACS in the z-band limited to the area common to ACS and ISAAC observations. The cyan square marks the position of the ACS UDF. The NICMOS UDF Treasury observations cover a field that is inside the UDF. The red rectangle marks the position of the K20 survey. The four white quadrants show the actual coverage of VLT-VIMOS U band imaging; large gaps are visible, since the observing program has not yet been completed.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3979f02.ps}\end{figure}$ Figure 2: The four channels of the IRAC images for the GOODS-South field. The pointings are chosen to have the UDF in the overlapping regions, where the exposure time is twice that in the external parts. The K20 layout is shown, as well.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3979f03a.ps}\vspace*{5mm} \includegraphics[width=8.65cm,clip]{3979f03b.ps}\end{figure}$ Figure 3: The magnitude limits (at 1 sigma and in 1 sq. arcsec) for the z band in the GOODS area. Dark areas correspond to deeper exposures, while white zones are much shallower ones, as also shown in the histogram of the magnitude limits. The geometry of the dark and white areas depends on the dithering strategy adopted.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3979f04a.ps}\vspace*{5mm} \includegraphics[width=8.5cm,clip]{3979f04b.ps}\end{figure}$ Figure 4: The magnitude limits (at 1 sigma and in 1 sq. arcsec) for the Ks band in the GOODS area. Dark areas correspond to deeper exposures, while white zones are much shallower ones, as also shown in the histogram of the magnitude limits.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3979f05a.ps}\vspace*{5mm} \includegraphics[width=8cm,clip]{3979f05b.ps}\end{figure}$ Figure 5: The half-light radius of galaxies in the GOODS-CDFS region as a function of the observed z and Ks magnitudes. The solid line indicates the completeness at $90\%$ value for elliptical galaxies, while the short-dashed line shows the same for spiral galaxies. We simulated 100 galaxies for each bin of magnitude, half-light radius, and bulge/disk ratio: the magnitude range is from 20 to 30 in steps of 0.5, the half-light radius range from 0.1 to 1.5 in steps of 0.1 arcsec, and the B/D from 0.3 to 0.9 in steps of 0.1 for ellipticals or from 0.02 to 0.08 in steps of 0.01 for spiral galaxies. The completeness as a function of magnitudes and half-light radii is the fraction of galaxies recovered by our detection procedure, averaged over the whole bulge/disk ratio interval. Long-dashed lines represent the fainter envelope of the observed galaxies. The completeness limit is given by the intersection of the latter curve with the brightest segments between simulated ellipticals and spirals. The plume of observed objects with bright magnitudes and with small half-light radius are stars.
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In the text

$\begin{figure} \par\includegraphics[height=8.1cm,width=7.5cm,clip]{3979f06.ps}\end{figure}$ Figure 6: A schematic representation of the ConvPhot algorithm. a) Two objects are clearly detected and separated in the high resolution detection image (blue, solid-thin line). The same two objects are blended in the low resolution " measure'' image (red, solid-thick line) and have quite different colours. b) The two objects are isolated in the high resolution detection image and are individually smoothed to the PSF of the measure image to obtain the "model'' images. c) The intensity of each object is scaled to match the global profile of the measure image. The scaling factors are found with a global $\chi ^2$ minimisation over the whole object pixels.
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In the text

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{3979f07.ps}\end{figure}$ Figure 7: The $z_{{\rm ACS}}-z_{{\rm FORS}}$ colour as a function of the magnitude of the objects detected on the K20 survey ( upper panel). The histogram of this colour ( lower panel) shows that the ConvPhot magnitude determination is not biased and is compatible with aperture photometry.
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{3979f08.ps}\end{figure}$ Figure 8: Observed colours as a function of redshift for the objects with spectroscopic redshifts in the GOODS-S field. The solid lines are ( from top to bottom) the colours predicted by the Bruzual & Charlot (2003) code for the following cases: (i) a maximally old model, obtained assuming an exponential history of star-formation with timescale 0.1 Gyr started at z=10 with metallicity $Z=2.5~Z_\odot$ ; (ii) a similar model but with an exponential timescale of 5 Gyr and an actively star-forming and non-evolving model with a constant star-formation rate and age of 1 Gyr. Dotted lines represent the redshift range in which the colours are not reliable due to the incomplete modelling of dust emission at $\lambda \ge 5.5~\mu{\rm m}$ rest frame (see Sect. 7).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3979f09.ps}\end{figure}$ Figure 9: A so-called "Drop'' image produced by ConvPhot in the Ks band. The name derives from the fact that each z-band detected object that is fitted by ConvPhot is multiplied by zero (drop) in order to leave only those Ks bright galaxies not detected in the z band.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{3979f10.ps}\end{figure}$ Figure 10: The histogram of spectroscopic redshifts for galaxies in the GOODS-CDFS field. Three peaks in redshifts show the presence of large-scale structures like groups or sheet/wall of galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3979f11.ps}\end{figure}$ Figure 11: The B-z versus z-Ks colours for objects in the GOODS south. Small dots are galaxies with redshifts $z\le 1.4$ or $z\ge 2.5$ , squares are spectroscopically known AGNs, arrows indicate galaxies with 1.4<z<2.5 (spectroscopic and photometric redshifts), filled points are spectroscopically known stars, while stars represent objects with point-like morphology according to SExtractor. Solid lines indicate the BzK criterion to isolate star-forming ( upper left part of the diagram) and passively evolving galaxies ( upper right part of the diagram) at 1.4<z<2.5. Objects below the dashed line are stars, according to Daddi et al. (2004).
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In the text

$\begin{figure} \par\includegraphics[width=6.85cm,clip]{3979f12.ps}\end{figure}$ Figure 12: Upper panel: the relation between the spectroscopic (x-axis) and the photometric (y-axis) redshift on 668 galaxies with accurate spectroscopic redshift. In the inset, the distribution of the absolute scatter $\Delta z = (z_{{\rm spec}}-z_{{\rm phot}})$ is shown and compared with a Gaussian distribution with a standard deviation $\sigma =0.06$ (smooth red curve). Lower panel: relative scatter $(z_{{\rm spec}}-z_{{\rm phot}})/(1+z_{{\rm spec}})$ , restricted to the z<2 range and discarding the most discrepant objects in the same sample.
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{3979f13.ps}\end{figure}$ Figure 13: Upper panel: redshift distribution of 9862 galaxies in the z-selected sample. The typical magnitude limit is $z\simeq 26$ . Lower panel: redshift distribution of 2931 galaxies in the Ks-selected sample. The typical magnitude limit is $K{\rm s}\simeq 23.8$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3979f02.ps}\end{figure}$	Figure 2: The four channels of the IRAC images for the GOODS-South field. The pointings are chosen to have the UDF in the overlapping regions, where the exposure time is twice that in the external parts. The K20 layout is shown, as well.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3979f03a.ps}\vspace*{5mm} \includegraphics[width=8.65cm,clip]{3979f03b.ps}\end{figure}$	Figure 3: The magnitude limits (at 1 sigma and in 1 sq. arcsec) for the z band in the GOODS area. Dark areas correspond to deeper exposures, while white zones are much shallower ones, as also shown in the histogram of the magnitude limits. The geometry of the dark and white areas depends on the dithering strategy adopted.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3979f04a.ps}\vspace*{5mm} \includegraphics[width=8.5cm,clip]{3979f04b.ps}\end{figure}$	Figure 4: The magnitude limits (at 1 sigma and in 1 sq. arcsec) for the Ks band in the GOODS area. Dark areas correspond to deeper exposures, while white zones are much shallower ones, as also shown in the histogram of the magnitude limits.
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$\begin{figure} \par\includegraphics[width=8.45cm,clip]{3979f07.ps}\end{figure}$	Figure 7: The $z_{{\rm ACS}}-z_{{\rm FORS}}$ colour as a function of the magnitude of the objects detected on the K20 survey ( upper panel). The histogram of this colour ( lower panel) shows that the ConvPhot magnitude determination is not biased and is compatible with aperture photometry.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3979f09.ps}\end{figure}$	Figure 9: A so-called "Drop'' image produced by ConvPhot in the Ks band. The name derives from the fact that each z-band detected object that is fitted by ConvPhot is multiplied by zero (drop) in order to leave only those Ks bright galaxies not detected in the z band.
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$\begin{figure} \par\includegraphics[width=8.25cm,clip]{3979f10.ps}\end{figure}$	Figure 10: The histogram of spectroscopic redshifts for galaxies in the GOODS-CDFS field. Three peaks in redshifts show the presence of large-scale structures like groups or sheet/wall of galaxies.
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$\begin{figure} \par\includegraphics[width=8.35cm,clip]{3979f13.ps}\end{figure}$	Figure 13: Upper panel: redshift distribution of 9862 galaxies in the z-selected sample. The typical magnitude limit is $z\simeq 26$ . Lower panel: redshift distribution of 2931 galaxies in the Ks-selected sample. The typical magnitude limit is $K{\rm s}\simeq 23.8$ .
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