All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{5474fg01.ps}\end{figure}$ Figure 1: Relation between the stellar masses derived with the inclusion of the Spitzer bands (14 bands) and those without the Spitzer bands (10 bands), as a function of redshift, on the Ks-selected galaxies of the GOODS-MUSIC sample. In the lower panel we plot the ratio between the two estimates, for each galaxy in the Ks-selected sample. In the upper, the distribution of such a ratio in different redshift ranges.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5474fg02.ps}\end{figure}$ Figure 2: Effect of the Spitzer bands on the mass estimate. Upper panel we plot the distribution of the relative uncertainty (at the $1\sigma$ level) in the mass estimate, when the Spitzer bands are included (14 bands) or not (10 bands). The distribution is computed over all Ks-selected galaxies. Lower panel: ratio of the uncertainty (at the $1\sigma$ level) in the mass estimate, when the Spitzer bands are included (14 bands) or not (10 bands), as a function of redshift.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5474fg03.ps}\end{figure}$ Figure 3: Stellar Masses for individual galaxies of the GOODS-MUSIC sample, as a function of redshift. Upper panel: the Ks-selected (filled circles) and the Z₈₅₀-selected sample (small dots) on the overall redshift range. Lower panel: same quantities, for galaxies at $z\geq 2$ . Objects in the Ks-selected sample are shown with large empty circles if they are also included in the Z₈₅₀-selected one, and with large filled circles if included only in the Ks-band catalog. Small dots are from the remaining Z₈₅₀-selected objects. In both panels, lines represent the completeness threshold, computed as described in the text. Thick lines correspond to the completeness threshold for a Ks-selected sample with respect to passively evolving models (continuous line) and dusty starburst with E(B-V)=1.1 (dashed). The thin lines show the same thresholds if a 4.5 $\mu$ m-selected sample would be used, for the two same spectral models.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{5474fg04.ps}\end{figure}$ Figure 4: Galaxy stellar Mass Functions in the GOODS-MUSIC sample, in different redshift ranges. Big circles represent the Galaxy Stellar Mass Functions of the Ks-selected sample, computed with the $1/V_{\rm max}$ formalism up to the appropriate completeness level, as described in the text, while small triangles show the Galaxy Stellar Mass Functions of the Z₈₅₀-selected sample, computed without any correction for incompleteness coverage of the M/L at faint limits. The dashed region represents the local GSMF of Cole et al. (2001), encompassing its original and the "rescaled'' version that we obtained in F04 (see text for details). The solid line is the evolutionary STY fit of our data, computed over the global redshift range 0.4<z<4, that we describe in Sect. 3.2.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5474fg05.ps}\end{figure}$ Figure 5: Contour levels of all the pairs of free parameters involved in the Schechter fitting of the GSMF, as obtained by a Maximum Likelihood minimization. Inner ellipses represent the $1\sigma$ contour, outer ones the $3\sigma$ contour. All contours have been obtained with marginalization of the other free parameters.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5474fg06.ps}\end{figure}$ Figure 6: The evolution of the Schechter parameters M^*(characteristic mass) and $\alpha$ (slope) as a function of redshift. Points represent the individual fits to the single redshift bin of Fig. 4 with their uncertainty, while lines represents the evolutionary STY fit of our data, computed over the global redshift range 0.4<z<4, that we describe in Sect. 3.2. Solid line is the second-order form for M^* (our fiducial model); dashed line is for $M^*=M^*_1 \times z + M^*_2 \times z^{M^*_3}$ ; dotted line is for $M^*\propto \log~(1+z)$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5474fg07.ps}\end{figure}$ Figure 7: Ratio between the observed Galaxy Stellar Mass Functions in the GOODS-MUSIC sample and the local GSMF, in the same redshift bins of Fig. 4. The observed data are normalized to two different choices of the local GSMF, namely the original one of Cole et al. (2001) (filled squares) and its rescaled version, that we described in the text (filled circles). The shaded area shows the corresponding ratios for the global Schechter fit, that we describe in Sect. 3.2.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{5474fg08.ps}\end{figure}$ Figure 8: Global Stellar Mass Density as function of redshift. Upper panel: the total Stellar Mass Density (integrated from log $(M_*/M_\odot )=8$ to log $(M_*/M_\odot )=13$ ) as estimated in the present work, obtained by an integration of our fiducial Schechter function (solid line). It is compared with other estimates adopted from the literature: the local value by Cole et al. (2001) (large empty circle), Fontana et al. (2004) (red filled circles), Fontana et al. (2003) (HDFS, open diamonds), Dickinson et al. (2003) (open squares), Cohen et al. (2001) (open crosses), Brinchmann & Ellis (2000) (filled diamonds), Drory et al. (2005) (open triangles, K-selected sample with horizontal basis, I-selected sample with vertical basis). Lower panel: the mass density computed only on galaxies more massive than log ( $M_*/M_\odot )=11$ . We remark that the value at $z\simeq 0.5$ is affected by an undersampling of massive galaxies because of the small size of the volume element. The solid line shows the mass density computed with our fiducial Schechter fit. See text and Table 1 for details. The two dotted lines represent an exponentially declining evolution of the stellar mass density, with timescales $\tau = 6, 0.6$ Gyr obtained by fitting the data at z<1.5and z>1.5, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{5474fg09.ps}\end{figure}$ Figure 9: Comparison between the observed Stellar Mass Density in massive galaxies (defined as those above $M_*>10^{11}~M_\odot$ ) and the corresponding predictions by recent theoretical models, as a function of redshift. Both data and models have been normalized to their own corresponding local value, for the relevant IMF. The shaded area represent the data obtained in the present work, normalized with two different choices of the local mass function (see text for details). The other curves show the prediction of theoretical models, as labelled in the legend: Bower et al. (2006) (B06), Menci et al. (2006) (M06), Monaco et al. (2006) (MFT06), Nagamine et al. (2005a) (N-TVD), Nagamine et al. (2005b) (N-SPH).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{5474fg10.ps}\end{figure}$ Figure 10: Comparison between the observed GSMF and a set of recent theoretical models. As in Fig. 4, large circles represent the mass-complete, Ks-selected sample. Lines refer to different models, as in Fig. 9. The dashed areas represent the confidence regions of the models by Nagamine et al. (2005a,b), where the limits are the predicted mass functions calculated at z=2, z=3 and z=4.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5474fg11.ps}\end{figure}$ Figure 11: Left: spectral Energy Distributions of two galaxies with photometric redshift >4, that would result very massive $M_*\simeq 5$ $\times$ $10^{11}~M_\odot$ . In the inset, the $\chi ^2$ as a function of redshift of the photometric redshift is shown. Right panel: spectral Energy Distributions of two objects with similar colours and uncertainty in redshift, that are assigned a photometric redshift $\simeq$ 2.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5474fg05.ps}\end{figure}$	Figure 5: Contour levels of all the pairs of free parameters involved in the Schechter fitting of the GSMF, as obtained by a Maximum Likelihood minimization. Inner ellipses represent the $1\sigma$ contour, outer ones the $3\sigma$ contour. All contours have been obtained with marginalization of the other free parameters.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{5474fg10.ps}\end{figure}$	Figure 10: Comparison between the observed GSMF and a set of recent theoretical models. As in Fig. 4, large circles represent the mass-complete, Ks-selected sample. Lines refer to different models, as in Fig. 9. The dashed areas represent the confidence regions of the models by Nagamine et al. (2005a,b), where the limits are the predicted mass functions calculated at z=2, z=3 and z=4.
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