All Figures

$\begin{figure} \par\includegraphics[width=5.7cm,clip]{h3896_f1a.ps}\hspace*{4mm}... ...c.ps}\hspace*{4mm} \includegraphics[width=5.7cm,clip]{h3896_f1d.ps} \end{figure}$ Figure 1: The time evolution of integrated colours (V-I), (V-K), (J-H), and (H-K) as a function of age, for the metallicity grid presented in this paper (solid line: Z=0.05, dotted: Z=0.02, short-dashed: Z=0.008, long-dashed: Z=0.004, and dot-dashed line: Z=0.0004).
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{h3896_f2.ps} \end{figure}$ Figure 2: V-K vs. B-V two-colour diagram. The solid dots with error bars correspond to the star clusters in the merger remnant NGC 7252 compiled by Maraston et al. (2001). The triangles represent LMC globular clusters with SWB type between 3 and 5.5 (Searle et al. 1980). B-V comes from van den Bergh (1981) and V-K from Persson et al. (1983). The typical error bar for LMC clusters is indicated. The lines show the evolution of the SSP models of this paper, for ages ranging from 50 Myr to 15 Gyr.
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In the text

$\begin{figure} \par\includegraphics[width=11.4cm,clip]{h3896_f3.ps} \end{figure}$ Figure 3: Similar to Fig. 2 but for different SSP models as indicated in each panel.
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In the text

$\begin{figure} \par\includegraphics[width=5.7cm,clip]{h3896_f4a.ps}\hspace*{1.5m... ...ps}\hspace*{1.5mm} \includegraphics[width=5.7cm,clip]{h3896_f4c.ps} \end{figure}$ Figure 4: The evolution of stellar mass-to-light ratios for K-band (left), V-band (middle) and bolometric light (right). Metallicities are coded with different line styles as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{h3896_f5a.ps}\hspace*{2mm} \includegraphics[width=7.8cm,clip]{h3896_f5b.ps}\end{figure}$ Figure 5: Left: effects of the IMF on M/L_K M/L_V compared to the effect of TP-AGB stars, at solar metallicity. Right: effect of TP-AGB stars on the K-band mass-to-light ratio for different metallicities as noted in the plots. Continuous lines show models where TP-AGB stars are accounted for, while dotted lines show models where these stars are neglected.
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In the text

$\begin{figure} \par\includegraphics[width=5.7cm,clip]{h3896_f1a.ps}\hspace{4mm}... ...c.ps}\hspace{4mm} \includegraphics[width=5.7cm,clip]{h3896_f1d.ps} \end{figure}$	Figure 1: The time evolution of integrated colours (V-I), (V-K), (J-H), and (H-K) as a function of age, for the metallicity grid presented in this paper (solid line: Z=0.05, dotted: Z=0.02, short-dashed: Z=0.008, long-dashed: Z=0.004, and dot-dashed line: Z=0.0004).
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$\begin{figure} \par\includegraphics[width=11.4cm,clip]{h3896_f3.ps} \end{figure}$	Figure 3: Similar to Fig. 2 but for different SSP models as indicated in each panel.
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$\begin{figure} \par\includegraphics[width=5.7cm,clip]{h3896_f4a.ps}\hspace{1.5m... ...ps}\hspace{1.5mm} \includegraphics[width=5.7cm,clip]{h3896_f4c.ps} \end{figure}$	Figure 4: The evolution of stellar mass-to-light ratios for K-band (left), V-band (middle) and bolometric light (right). Metallicities are coded with different line styles as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{h3896_f5a.ps}\hspace*{2mm} \includegraphics[width=7.8cm,clip]{h3896_f5b.ps}\end{figure}$	Figure 5: Left: effects of the IMF on M/L_K M/L_V compared to the effect of TP-AGB stars, at solar metallicity. Right: effect of TP-AGB stars on the K-band mass-to-light ratio for different metallicities as noted in the plots. Continuous lines show models where TP-AGB stars are accounted for, while dotted lines show models where these stars are neglected.
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