All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{4197f1.eps} \end{figure}$ Figure 1: Synthetic CMDs for Z=0.0002, Y=0.23, and three different ages: 500 Myr (black), 2 Gyr (red), and 11 Gyr (blue). For each population, $M_V^{\rm tot}=-6$ mag is adopted. The simulation of photometric errors is not included.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{4197f2a.eps}\par\vspace*{2mm... ...}\par\vspace*{2mm} \includegraphics[width=5cm,clip]{4197f2c.eps} \end{figure}$ Figure 2: Comparison between present synthetic CMDs (red dots), without the inclusion of simulated photometric errors, and the observed ones of the globular clusters M 68, M 15, and M 30 (black dots). The assumed age is 11 Gyr, and the adopted chemical composition is Z=0.0002 and Y=0.23 (see text). The values of the distance modulus and the reddening obtained from the analysis are also indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4197f3a.eps}\hspace*{4mm} \... ....eps}\hspace*{4mm} \includegraphics[width=7cm,clip]{4197f3d.eps} \end{figure}$ Figure 3: Time evolution of selected integrated colours in the standard UBVRIJHK filters for models with $M_V^{\rm tot}=-4$ (red triangles, dashed lines) and $M_V^{\rm tot}=-8$ (black points, solid lines). $1\sigma$ colour dispersion is reported for each model, see text.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{4197f4.eps} \end{figure}$ Figure 4: V-K colour distribution resulting from 100 simulations for a model with 100 Myr, Z=0.0002, and $M_V^{\rm tot}=-4$ (solid) and -8 mag (dotted).
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4197f5a.eps}\hspace*{4mm} ... ...ps}\hspace*{4mm} \includegraphics[width=7.4cm,clip]{4197f5d.eps} \end{figure}$ Figure 5: Time evolution of selected integrated colours for SSPs with $M_V^{\rm tot}=-8$ calculated with the lower, central, and upper values for the Kroupa (2002) IMF exponent ( $\alpha$ ) for $M \geq 0.5~M_{\odot}$ . Black dots indicate our reference model ( $\alpha =2.3$ ), red triangles indicate models with $\alpha =2.0$ , and blue stars models with $\alpha =2.6$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm]{4197f6a.eps}\hspace*{4mm} \inc... ...f6c.eps}\hspace*{4mm} \includegraphics[width=7.4cm]{4197f6d.eps} \end{figure}$ Figure 6: Integrated colours (B-V, upper panels; V-K, lower panels) from recent papers: present models (black dots); Kurth et al. (1999, red Z=0.0001, green Z=0.0004 squares, solid line), Brocato et al. (2000, cyan dots), Anders & Fritze-v. Alvensleben (2003, orange solid line), Girardi et al. (2000, blue squares, short-dashed line), Zhang et al. (2002, pink circles, dotted line), Bruzual & Charlot (2003, violet Z=0.0001, brown Z=0.0004 circles, dashed line). Maraston (2005, red triangles, dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4197f7a.eps}\hspace*{4mm} \includegraphics[width=7cm,clip]{4197f7b.eps} \end{figure}$ Figure 7: Left panel: fraction of very low-mass stars ( $M\leq 0.6~M _{\odot}$ ) that contribute to the mass-luminosity ratio ( ${\cal M}/L$ ) (in solar units) as a function of the age for $M_V^{\rm tot}=-8$ . Filled circles represent our standard model in which all masses with $M \geq 0.08~ M_{\odot}$ are included; the effect of considering only stars with $M \geq 0.4~ M_{\odot}$ (filled triangles) or $M\geq 0.6~M_{\odot}$ (filled squares) is analysed separately. Right panel: as in the left panel, but when the WD population is (filled circles, standard model) or is not (filled squares) included.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4197f8.eps} \end{figure}$ Figure 8: Time behaviour of the logarithm of the cluster total mass needed to reach $M_V^{\rm tot}=-8$ normalized to the maximum value, as a function of age.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4197f9a.eps}\hspace*{4mm} ... ...ps}\hspace*{4mm} \includegraphics[width=7.4cm,clip]{4197f9d.eps} \end{figure}$ Figure 9: Time behaviour of the ${\cal M}/L$ ratio (in solar units) for selected passbands (U,B,V,K). For each model, $1\sigma$ dispersion is shown. Red triangles (dashed line) indicate models with $M_V^{\rm tot}=-4$ , and black dots (continuos line) models with $M_V^{\rm tot}-8$ .
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4197f10a.eps}\hspace*{4mm} \includegraphics[width=7cm,clip]{4197f10b.eps} \end{figure}$ Figure 10: Time evolution of ${\cal M}/L_B$ ( left panel) and ${\cal M}/L_K$ ( right panel) in our reference model (black dots) compared with the Bruzual & Charlot (2003, B&C 2003) for models with Z=0.0001 (violet dashed line), and Z=0.0004 (brown dashed line), Anders & Fritze-v. Alvensleben (2003, A&F 2003) models (orange solid line), and Maraston (2005, M2005) for Z=0.0003 (red triangles, dashed line). The IMF adopted by various authors are reported in Table 4.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4197f11a.eps}\hspace*{4mm}... ...s}\hspace*{4mm} \includegraphics[width=7.4cm,clip]{4197f11d.eps} \end{figure}$ Figure 11: Time evolution of ${\cal M}/L$ (in solar units) in selected passbands ( U, B, V, K) for models with $M_V^{\rm tot}=-8$ calculated with the lower, central, and upper values for the Kroupa (2002) IMF exponent for $M \leq 0.5~ M_{\odot}$ . Black dots indicate our reference model ( $\alpha =1.3$ ), red triangles indicate models with $\alpha =0.8$ , and blue stars models with $\alpha =1.8$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm]{4197f12a.eps}\hspace*{4mm} \in... ...2c.eps}\hspace*{4mm} \includegraphics[width=7.4cm]{4197f12d.eps} \end{figure}$ Figure 12: Time evolution of ${\cal M}/L$ (in solar units) in selected passbands ( U, B, V, K) for models with $M_V^{\rm tot}=-8$ calculated with the lower, central, and upper values for the Kroupa (2002) IMF exponent for $M \geq 0.5~M_{\odot}$ . Black dots indicate our reference model ( $\alpha =2.3$ ), red triangles indicate models with $\alpha =2.0$ , and blue stars indicate models with $\alpha =2.6$ .
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4197f1.eps} \end{figure}$	Figure 1: Synthetic CMDs for Z=0.0002, Y=0.23, and three different ages: 500 Myr (black), 2 Gyr (red), and 11 Gyr (blue). For each population, $M_V^{\rm tot}=-6$ mag is adopted. The simulation of photometric errors is not included.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{4197f3a.eps}\hspace{4mm} \... ....eps}\hspace{4mm} \includegraphics[width=7cm,clip]{4197f3d.eps} \end{figure}$	Figure 3: Time evolution of selected integrated colours in the standard UBVRIJHK filters for models with $M_V^{\rm tot}=-4$ (red triangles, dashed lines) and $M_V^{\rm tot}=-8$ (black points, solid lines). $1\sigma$ colour dispersion is reported for each model, see text.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{4197f4.eps} \end{figure}$	Figure 4: V-K colour distribution resulting from 100 simulations for a model with 100 Myr, Z=0.0002, and $M_V^{\rm tot}=-4$ (solid) and -8 mag (dotted).
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4197f5a.eps}\hspace{4mm} ... ...ps}\hspace{4mm} \includegraphics[width=7.4cm,clip]{4197f5d.eps} \end{figure}$	Figure 5: Time evolution of selected integrated colours for SSPs with $M_V^{\rm tot}=-8$ calculated with the lower, central, and upper values for the Kroupa (2002) IMF exponent ( $\alpha$ ) for $M \geq 0.5~M_{\odot}$ . Black dots indicate our reference model ( $\alpha =2.3$ ), red triangles indicate models with $\alpha =2.0$ , and blue stars models with $\alpha =2.6$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4197f8.eps} \end{figure}$	Figure 8: Time behaviour of the logarithm of the cluster total mass needed to reach $M_V^{\rm tot}=-8$ normalized to the maximum value, as a function of age.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4197f9a.eps}\hspace{4mm} ... ...ps}\hspace{4mm} \includegraphics[width=7.4cm,clip]{4197f9d.eps} \end{figure}$	Figure 9: Time behaviour of the ${\cal M}/L$ ratio (in solar units) for selected passbands (U,B,V,K). For each model, $1\sigma$ dispersion is shown. Red triangles (dashed line) indicate models with $M_V^{\rm tot}=-4$ , and black dots (continuos line) models with $M_V^{\rm tot}-8$ .
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