All Figures

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{2688f1.eps} \end{figure}$ Figure 1: Mass fractions in GW and in remaining galaxy as a function of the initial (proto)galactic mass M, for four different redshifts of formation. Thick lines: galactic models with the PNJ IMF; thin lines: galactic models with the Salpeter IMF.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2688f2.eps} \end{figure}$ Figure 2: Iron abundance (in solar units) of the GW, for galaxies of initial (baryonic) mass M as indicated in each panel, and as a function of the redshift of formation. Thick lines: galactic models with the PNJ IMF; thin lines: models with the Salpeter IMF (redshift independent).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{2688f3.eps} \end{figure}$ Figure 3: The M/L ratio in the B band for living stars in the PNJ galaxies ( dots and triangles, two example models, see legend) and in the Salpeter galaxies ( thin line; mass limits for the Salpeter IMF are [0.18-120] $M_{\odot }$ ).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{2688f4.eps} \end{figure}$ Figure 4: Fraction of living stars within the "galactic remnant'' $R_{\rm gal}$ , decreasing with age in favour of remnants and ejected gas. PNJ models for three initial (proto)galactic masses and two redshifts of formation shown for the sake of example (see legend). Thick lines with no dots correspond to the Salpeter models.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{2688f5.eps} \end{figure}$ Figure 5: M/L ratio of the global "galactic remnant'' $R_{\rm gal}$ (stars+remnants+gas ejected after the GW), as a function of age. Symbols as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{2688f6.eps} \end{figure}$ Figure 6: The IMLR in the GW for model galaxies with the PNJ IMF ( thick lines) and the Salpeter IMF ( thin lines).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{2688f7.eps} \end{figure}$ Figure 7: The observed B-band luminosity function of cluster galaxies by Trentham (1998), in relative frequency.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2688f8.eps} \end{figure}$ Figure 8: An example of Galactic Formation History $\Psi _{\rm G}$ [Gyr^-1] as a function of redshift and corresponding Luminosity Function (observational data by Trentham 1998). Model parameters are listed in Table 2.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{2688f9.eps} \end{figure}$ Figure 9: Evolution of the characteristic mass M_* (in this example, with $M_{\rm Nor}=3 \times 10^{13}~M_{\odot}$ ) and of the minimum and maximum mass limits for the GIMF, $M_{\rm i}=M_*/100$ and $M_{\rm u}=100 ~ M_*$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{2688f10.eps} \end{figure}$ Figure 10: Luminosity Function of cluster galaxies as predicted by our "fiducial'' Model A; triangles are the observational data by Trentham (1998). Both the model LF and data are shown normalized to the same total (unit) number of objects in the observed range (M_B between -22 and -11 mag).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2688f11.eps} \end{figure}$ Figure 11: Top panel: GFH of our Model A as a function of redshift; $\Psi _{\rm G}$ is expressed in mass fraction of the cluster per Gyr. Bottom panel: comparison of the shape of our GFH with the "Madau plot'' (data from Steidel et al. 1999); the theoretical curve $\Psi _{\rm G}$ is arbitrarily normalized so that its maximum value reaches $\log(\Psi_{\rm G})=-0.8$ , similar to the maximum in the data.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.9cm,clip]{2688f12.eps} \end{figure}$ Figure 12: Time evolution of the cluster components for Model A.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{2688f13.eps} \end{figure}$ Figure 13: Evolution of the iron abundance in the ICM. At high redshift (z>1.5) metallicities for Damped Lyman $\alpha$ systems and Lyman Break Galaxies are shown for the sake of qualitative comparison (metallicity ranges for LBGs and DLAs at z=3 are from Pettini 2000).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{2688f14.eps} \end{figure}$ Figure 14: Same as Figs. 10-13, but for Model AS based on the Salpeter IMF.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{2688f15.eps} \end{figure}$ Figure 15: Results for Models M1, M2 and M3 which differ from our fiducial Model A in the characteristic mass $M_{\rm Nor}$ , increasing from M1 to M3 (Table 2). a) Luminosity Function; b) evolution of the iron abundance; c) evolution of the cluster components; d) Galactic Formation History. Lines, symbols and data as in Figs. 10 to 13.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{2688f16.eps} \end{figure}$ Figure 16: Results for Models AfYz15 and M2fYz15, analogous to models A and M2 but with fixed galactic yields corresponding to the PNJ models with z=15. Panels and symbols as in Fig. 15.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{2688f17.eps} \end{figure}$ Figure 17: Evolution of the [O/Fe] abundance ratio as a function of redshift for our Models A, AS and AfY, compared to observations for low redshift clusters.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{2688f1.eps} \end{figure}$	Figure 1: Mass fractions in GW and in remaining galaxy as a function of the initial (proto)galactic mass M, for four different redshifts of formation. Thick lines: galactic models with the PNJ IMF; thin lines: galactic models with the Salpeter IMF.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{2688f2.eps} \end{figure}$	Figure 2: Iron abundance (in solar units) of the GW, for galaxies of initial (baryonic) mass M as indicated in each panel, and as a function of the redshift of formation. Thick lines: galactic models with the PNJ IMF; thin lines: models with the Salpeter IMF (redshift independent).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{2688f3.eps} \end{figure}$	Figure 3: The M/L ratio in the B band for living stars in the PNJ galaxies ( dots and triangles, two example models, see legend) and in the Salpeter galaxies ( thin line; mass limits for the Salpeter IMF are [0.18-120] $M_{\odot }$ ).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{2688f4.eps} \end{figure}$	Figure 4: Fraction of living stars within the "galactic remnant'' $R_{\rm gal}$ , decreasing with age in favour of remnants and ejected gas. PNJ models for three initial (proto)galactic masses and two redshifts of formation shown for the sake of example (see legend). Thick lines with no dots correspond to the Salpeter models.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{2688f5.eps} \end{figure}$	Figure 5: M/L ratio of the global "galactic remnant'' $R_{\rm gal}$ (stars+remnants+gas ejected after the GW), as a function of age. Symbols as in Fig. 4.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{2688f6.eps} \end{figure}$	Figure 6: The IMLR in the GW for model galaxies with the PNJ IMF ( thick lines) and the Salpeter IMF ( thin lines).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{2688f7.eps} \end{figure}$	Figure 7: The observed B-band luminosity function of cluster galaxies by Trentham (1998), in relative frequency.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2688f8.eps} \end{figure}$	Figure 8: An example of Galactic Formation History $\Psi _{\rm G}$ [Gyr^-1] as a function of redshift and corresponding Luminosity Function (observational data by Trentham 1998). Model parameters are listed in Table 2.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{2688f9.eps} \end{figure}$	Figure 9: Evolution of the characteristic mass M_* (in this example, with $M_{\rm Nor}=3 \times 10^{13}~M_{\odot}$ ) and of the minimum and maximum mass limits for the GIMF, $M_{\rm i}=M_/100$ and $M_{\rm u}=100 ~ M_$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{2688f10.eps} \end{figure}$	Figure 10: Luminosity Function of cluster galaxies as predicted by our "fiducial'' Model A; triangles are the observational data by Trentham (1998). Both the model LF and data are shown normalized to the same total (unit) number of objects in the observed range (M_B between -22 and -11 mag).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.9cm,clip]{2688f12.eps} \end{figure}$	Figure 12: Time evolution of the cluster components for Model A.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{2688f13.eps} \end{figure}$	Figure 13: Evolution of the iron abundance in the ICM. At high redshift (z>1.5) metallicities for Damped Lyman $\alpha$ systems and Lyman Break Galaxies are shown for the sake of qualitative comparison (metallicity ranges for LBGs and DLAs at z=3 are from Pettini 2000).
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$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{2688f14.eps} \end{figure}$	Figure 14: Same as Figs. 10-13, but for Model AS based on the Salpeter IMF.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{2688f15.eps} \end{figure}$	Figure 15: Results for Models M1, M2 and M3 which differ from our fiducial Model A in the characteristic mass $M_{\rm Nor}$ , increasing from M1 to M3 (Table 2). a) Luminosity Function; b) evolution of the iron abundance; c) evolution of the cluster components; d) Galactic Formation History. Lines, symbols and data as in Figs. 10 to 13.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{2688f16.eps} \end{figure}$	Figure 16: Results for Models AfYz15 and M2fYz15, analogous to models A and M2 but with fixed galactic yields corresponding to the PNJ models with z=15. Panels and symbols as in Fig. 15.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{2688f17.eps} \end{figure}$	Figure 17: Evolution of the [O/Fe] abundance ratio as a function of redshift for our Models A, AS and AfY, compared to observations for low redshift clusters.
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