Fig. 8.
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Photometric evolution of our instantaneous burst STARBURST99 models. The standard Salpeter (1955) IMF is shown in orange, while a truncated IMF (at 20 M⊙) is shown in blue, and a steep IMF (α = 3.3) is shown in green. Left panel: time evolution of FUV magnitude for a cluster mass of 2000 M⊙. The horizontal dashed line shows the detection limit for our sample (FUV = 23.8 mag). Middle panel: time evolution of FUV−NUV color. The horizontal dashed line shows the cut for blue clusters (FUV−NUV = 0). Right panel: time evolution of log(FHα/fλFUV). The horizontal dashed line shows the cut for Hα-bright clusters (log(FHα/fλFUV) = 1).
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