Fig. 8.
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As in Fig. 7 but for clusters of bewteen 1.5 and 4.5 Gyr in age. We note the paucity of OCs older than 2.5 Gyr (in particular, only one SPA cluster is present, Ruprecth 171, from Casali et al. 2020). The data are quite well reproduced by the models; the exceptions are the old and very metal-poor clusters that have |z|> 1 kpc, further away from the Galactic plane than the plotted models.
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