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Fig. 8

image

Rotation period distribution of the β Pic members (only the ± 3σ fits to the distribution are plotted as solid black lines) is compared with the distribution of the h Per single members (light-blue open squares) in the top-left panel; with the distribution of IC 2391+IC 2602+Argus members (violet open circles), and NGC 2547 members (blue asterisks) in the bottom-left panel, and with the distribution of the Pleiades members (brown small bullets) in the bottom-right panel. Thick solid lines are linear fits to the 90th percentile of the distribution of the comparison clusters. Filled bullets connected with dashed lines indicate the model rotation period predicted by the Gallet & Bouvier (2015) for 1.0, 0.8 and 0.5 M.

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