All Figures

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{4341_f1a.ps}\par\vspace*{1... ...par\vspace*{1.29mm} \includegraphics[width=8.3cm,clip]{4341_f1c.ps} \end{figure}$ Figure 1: Number counts of extended objects with ${\it S/N} > 5$ in the clusters and reference fields. Upper panel: the solid line shows the number counts in the Cl1252 field ( ${\simeq } 3.7$ square arcmin). The circles and the dotted line show the counts in the reference regions selected in the FIRES and GOODS-S fields respectively, normalized to the cluster area. The counts in the GOODS-S field are shown down to the completeness magnitude ( $K_{\rm s} \simeq 23$ ). Middle panel: the solid line shows the number counts in the Cl0910 field ( ${\simeq } 4.4$ square arcmin). The circles and the dotted line show the expected background level from reference regions selected in the SOFI and ISAAC GOODS-S fields, respectively. Lower panel: the solid line shows the number counts in the Cl0848 field ( ${\simeq } 1.8$ square arcmin), the circles show the expected background level based on the Hubble UDF. In all panels, the symbols/lines showing background number counts have been shifted by $\pm$ 0.05 mag along the x-axis to avoid overlapping errorbars.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{4341_f2a.ps}\par\vspace*{1... ...s}\par\vspace*{1mm} \includegraphics[width=7.9cm,clip]{4341_f2c.ps} \end{figure}$ Figure 2: Individual cluster luminosity functions for Cl1252 ( upper panel), Cl0910 ( middle), and Cl0848 ( lower). In all panels, the solid line shows the best-fit Schechter function as derived from the binned counts, and the inserted plot shows the 1, 2- $\sigma$ confidence levels on the parameters M^* and $\alpha$ , calculated from the maximum likelihood on binned counts (dashed lines) and from the maximum likelihood on unbinned, not background subtracted counts (solid thick lines - not shown for Cl0848, see text). The thick and thin crosses show the position of the best-fit parameters derived with the former and latter methods, respectively (see text for details). In the upper panel the empty circles show the Cl1252 LF as determined by T04, and the dotted histogram shows for comparison the LF from this work binned with the same bin size as in T04.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{4341_f3.ps} \end{figure}$ Figure 3: The composite cluster luminosity function at z=1.2 (filled dots) compared to the field galaxies LF at $z \simeq 1$ . The solid line shows the best-fit Schechter, and the inserted plot shows the 1, 2- $\sigma$ confidence levels on the Schechter parameters as in Fig. 2. All field galaxies LFs have been arbitrarily rescaled.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{4341_f4.ps} \end{figure}$ Figure 4: The composite cluster luminosity function at z=1.2 (filled dots) compared to the local cluster galaxies LF, corrected by 1.3 mag for passive evolution (see text). The solid line shows the best-fit Schechter, and the inserted plot shows the 1, 2- $\sigma$ confidence levels on the Schechter parameters as in Fig. 2. All local cluster galaxies LFs have been arbitrarily rescaled.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{4341_f5.ps} \end{figure}$ Figure 5: The background number counts as estimated in different control fields. The filled symbols show the counts from the control field in the FIRES region, the solid and dashed lines from those in the GOODS-S regions (ISAAC and SOFI, respectively), and the dotted lines show the counts from the 17 ISAAC tiles in the GOODS-S field.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4341_f6.ps} \end{figure}$ Figure 6: Impact of field-to-field variations on the determination of the LF. In the main panel the best-fit M^* and $\alpha$ (cross) and their 1- and 2- $\sigma$ confidence levels are shown, as in Figs. 3 and 4. The M^* and $\alpha$ parameters from LF determinations with 18 different small control fields are shown as squares. In the side-panels the distributions of these M^* ( top) and $\alpha$ ( right) are shown. Solid symbols ( in the main panel) and solid lines ( in the side panels) show the results for GOODS-S tiles counts complemented with FIRES counts at faint magnitudes, while empty symbols and dotted lines show the results with modified FIRES counts at faint magnitudes (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4341_f7.ps} \end{figure}$ Figure 7: The redshift evolution of the characteristic magnitude K^*. Different symbols show different determinations of K^* as indicated in the legend. The no evolution prediction is calculated from the Coma K^* (De Propris et al. 1998), k-corrected as in Pozzetti et al. (2003). Passive evolution model predictions are from Kodama & Arimoto (1997), normalized to the Coma K^*. All determinations have fixed slope $\alpha = -0.9$ , except Andreon (2001), Toft et al. (2003), Lin et al. (2004), T04 and the present work. For Lin et al. (2004) the plotted value is the mean of two values determined for $\alpha = -0.85$ and $\alpha = -1.1$ . For both this work and Toft et al. (2003) also the K^* value with $\alpha$ fixed at -0.9 is shown (corresponding empty symbol). Note that errors on M^* which are computed with $\alpha$ fixed and free are not directly comparable. Error bars on the x-axis, when plotted, represent the redshift range of clusters which are combined to draw that point.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{4341_f8.ps} \end{figure}$ Figure 8: The contribution of early and late type galaxies to the LF of Cl1252. The filled and empty symbols show the LFs for early and late type photometric members (based on the T04 sample), classified from their broad band colours. The dashed line shows the contribution of morphologically selected early-types (Blakeslee et al. 2003). The solid histogram shows the number counts of all galaxies (excluding spectroscopic interlopers) along the red sequence as determined in (Blakeslee et al. 2003) (no statistical subtraction of the field galaxies contamination was made; the shaded area shows the effect of photometric errors - see text). The solid curve shows the best-fit Schechter function for the Cl1252 global LF.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4341_f9.ps}\par \end{figure}$ Figure 9: The evolution of the restframe K band mass-to-light ratio. The filled circles are the M/L ratios from this work. The star shows the M/L determined for Cl1252 using the T04 LF. The filled squares are K band M/L measurement from Rines et al. (2001), Kneib et al. (2003), Lin et al. (2003), Rines et al. (2004). The empty symbols show the K band M/L ratio derived from published M/L estimates in other passbands, i.e. B/B_j band (circle) from Girardi et al. (2000), Hoekstra et al. (2002), Sanderson & Ponman (2003), Gavazzi et al. (2004), R/r band (square) from Carlberg et al. (1997) and Andernach et al. (2004), and V band from Cirimele et al. (1997) and Hradecky et al. (2000) (see text). Crossed and circled points have masses determined from galaxy kinematics or strong/weak lensing respectively, at a difference with X-ray masses used in this work. The solid line traces the evolution expected from pure luminosity evolution of a simple stellar population formed at z=5, assuming that the cluster M/L ratio only evolves because of stellar evolution in galaxies, and neglecting any evolution in the dark mass. The dotted line shows the reference (z=0) value.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4341_f10.ps} \end{figure}$ Figure 10: The stellar mass function as determined from the composite $K_{\rm s}$ band LF. The shaded area accounts for errors in the $K_{\rm s}$ band LF and in the stellar mass to $K_{\rm s}$ light ratio (see text for details). Other determinations of the stellar mass function are shown for reference, as indicated in the legend.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{4341_f3.ps} \end{figure}$	Figure 3: The composite cluster luminosity function at z=1.2 (filled dots) compared to the field galaxies LF at $z \simeq 1$ . The solid line shows the best-fit Schechter, and the inserted plot shows the 1, 2- $\sigma$ confidence levels on the Schechter parameters as in Fig. 2. All field galaxies LFs have been arbitrarily rescaled.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{4341_f4.ps} \end{figure}$	Figure 4: The composite cluster luminosity function at z=1.2 (filled dots) compared to the local cluster galaxies LF, corrected by 1.3 mag for passive evolution (see text). The solid line shows the best-fit Schechter, and the inserted plot shows the 1, 2- $\sigma$ confidence levels on the Schechter parameters as in Fig. 2. All local cluster galaxies LFs have been arbitrarily rescaled.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{4341_f5.ps} \end{figure}$	Figure 5: The background number counts as estimated in different control fields. The filled symbols show the counts from the control field in the FIRES region, the solid and dashed lines from those in the GOODS-S regions (ISAAC and SOFI, respectively), and the dotted lines show the counts from the 17 ISAAC tiles in the GOODS-S field.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4341_f10.ps} \end{figure}$	Figure 10: The stellar mass function as determined from the composite $K_{\rm s}$ band LF. The shaded area accounts for errors in the $K_{\rm s}$ band LF and in the stellar mass to $K_{\rm s}$ light ratio (see text for details). Other determinations of the stellar mass function are shown for reference, as indicated in the legend.
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