Table 2.
Rotation periods for unsaturated M dwarfs and cluster membership criteria.
| ID | C11 | (V − Ks)0 | Prot | ΔProt | pRV | d | dpm | Comment |
|---|---|---|---|---|---|---|---|---|
| (mag) | (d) | (d) | (pc) | (mas yr−1) | ||||
| 102025 | 248532 | 3.868 | 14.2 | 1.9 | 0.94 | 509 | 0.58 | |
| 304320 | 145504 | 3.938 | 32.0 | 3.5 | 0.86 | 497 | 0.23 | Likely astrometric binary |
| 400454 | 179867 | 4.110 | 22.0 | 6.2 | 0.94 | 468 | 0.60 | |
| 400856 | 172827 | 3.718 | 20.6 | 1.8 | 0.66 | 390 | 0.97 | Likely non-member |
| 522220 | 143090 | 4.295 | 30.0 | 3.5 | 0.94 | 521 | 1.02 | Likely non-member |
| 604445 | 87263 | 3.889 | 17.1 | 1.6 | 0.93 | 469 | 0.30 | |
| 612827 | 48244 | 4.322 | 48.0 | 6.0 | 0.92 | 561 | 0.38 | Photometric binary, likely non-member |
| 716466 | 184783 | 3.941 | 16.8 | 2.9 | 0.94 | 481 | 0.74 | |
| 801059 | 305389 | 4.187 | 27.0 | 3.6 | 0.93 | 471 | 0.17 |
Notes. C11: ID from Clem et al. (2011); pRV: membership probability from radial velocity (F19); d: distance from Bailer-Jones et al. (2018), mean cluster distance d = 484 pc; dpm: distance from cluster centre in proper motion space μα = −10.37, μδ = 5.18, based on Gaia DR2 (Gaia Collaboration 2018).
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