A relation between the radial velocity dispersion of young clusters and their age - Evidence for hardening as the formation scenario of massive close binaries

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Fig. 3.

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Median σ_1D obtained for distributions with different combinations of f_bin and P_cutoff. For this set of simulations, we used a sample of 20 stars ranging in masses from 15 to 60 M_⊙. The contours show the trends followed by σ_1D values of 5.5, 15, 25.3, 30.9, 50.3, and 66 km s⁻¹.

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