Table 1.
Properties of the clusters considered in this study.
| Cluster | d | tCMD | tDT |  |
σp | σv | R50 | nstars | ndiv | neva | neva, 70 | ϕeva | σeva | |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| [pc] | [Myr] | [Myr] | [Myr] | [pc] | [km s−1] | [pc] | ||||||||
| α Sco 1 | 148 |
 |
 (b) |
 |
0.31 | 0.07 | 7.8 | 57 | 21 | 7 | 2 | 0.93 | 1.12 | |
| α Sco 2 | 148 |
 |
 (b) |
 |
0.62 | 0.10 | 6.8 | 78 | 33 | 6 | 2 | 0.89 | 1.16 | |
| β Sco | 153 |
 (a) |
 (b) |
 |
0.53 | 0.12 | 4.7 | 61 | 14 | 16 | 4 | 0.88 | 0.74 | |
| δ Sco | 142 |
 (a) |
 (b) |
 |
0.42 | 0.09 | 4.7 | 131 | 13 | 52 | 16 | 0.89 | 0.24 | |
| ν Sco | 139 |
 (a) |
 (b) |
 |
0.39 | 0.13 | 2.0 | 57 | 22 | 6 | 2 | 0.91 | 1.14 | |
| π Sco | 123 |
 |
 (b) |
 |
0.26 | 0.13 | 15.7 | 88 | 17 | 27 | 8 | 0.88 | 0.37 | |
| σ Sco | 152 |
 |
 (b) |
 |
0.63 | 0.14 | 9.8 | 104 | 25 | 27 | 6 | 0.88 | 0.49 | |
| ρ Oph | 139 |
 (a) |
 (b) |
 |
0.52 | 0.10 | 3.3 | 94 | 37 | 10 | 3 | 0.88 | 0.74 | |
| β Pic | 40 |
 (a) |
 (c) |
 |
0.13 | 0.29 | 24.3 | 26 | 0 | 13 | 4 | 0.87 | 0.60 | |
| Tuc-Hor | 47 |
 (a) |
 (d) |
 |
0.03 | 0.40 | 17.1 | 21 | 2 | 8 | 3 | 0.87 | 0.61 |
Notes. Columns indicate (1) the cluster name, (2) the distance to the cluster, (3) the CMD age from the PARSEC isochrones used in this work, (4) the dynamical traceback age, (5) the corrected evaporation age determined in this work, (6–7) the observational error in positions and velocities, (8) the core radius, (9) the number of stars used to obtain the CMD and dynamical traceback ages and the starting sample for the evaporation ages, (10) the number of divergent stars, (11) the number of evaporated stars, (12) the number of stars used to compute the evaporation age, and (13–14) the correction factor and the uncertainty of the evaporation age (see Appendix B).
References. (a) Miret-Roig et al. (2024); (b) Miret-Roig et al. (2022); (c) Miret-Roig et al. (2020); (d) Galli et al. (2023).
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