All Figures

	Figure 1: Cluster evolution in the { }-plane for metallicities ( ) and dissolution timescales  Myr. Solid lines represent evolutionary tracks for initial masses in the range   with 0.5-dex intervals, while the dotted curves denote cluster isochrones at ages  Gyr. Dots denote the onset of the preferential loss of low-mass stars for each evolutionary track.
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In the text

	Figure 2: Mass-to-light ratio versus mass for globular clusters in different galaxies. The Cen A data is from Mieske et al. (2008), all other data is taken from Rejkuba et al. (2007). The canonical (mass-independent) models are overplotted as solid, dashed and dotted lines for , respectively.
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In the text

Figure 3: Comparison of t=12 Gyr model cluster isochrones in the { }-plane to globular clusters in four different galaxies. Clusters with metallicities are denoted with blue diamonds, green triangles, and red squares, respectively. Model curves for these metallicities are shown in the same colours, with dotted, dashed and solid lines, respectively. In all cases an age of t=12 Gyr is assumed. For each galaxy, a dash-dotted line of constant luminosity represents the faintest cluster that is covered by the models, illustrating that the samples are magnitude-limited. Metallicities are from Beasley et al. (2008, Cen A), Harris (1996, Milky Way), Dubath & Grillmair (1997, M 31) and Mackey & Gilmore (2004, LMC). To prevent crowding, error bars are only shown for clusters that fall outside the range covered by the models.

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In the text