Table 3.
Group proper motions in α* and δ derived in this work and those from the Villafranca II and III works, all based on Gaia EDR3 astrometry.
| This work | Villafranca II-III | ||||
|---|---|---|---|---|---|
| Group | N | μα * ,g | μδ, g | μα * ,g | μδ, g |
| O-002 (Trumpler 14) | 32 | −6.580 ± 0.240 | 2.089 ± 0.246 | −6.534 ± 0.023 | 2.076 ± 0.023 |
| O-003 (Trumpler 16 W) | 8 | −7.179 ± 0.102 | 2.730 ± 0.103 | −7.128 ± 0.024 | 2.670 ± 0.024 |
| O-025 (Trumpler 16 E) | 47 | −6.894 ± 0.214 | 2.647 ± 0.177 | −6.877 ± 0.023 | 2.596 ± 0.023 |
| O-027 (Trumpler 15) | 17 | −6.172 ± 0.164 | 2.224 ± 0.175 | −6.282 ± 0.023 | 2.131 ± 0.023 |
| O-028 (Collinder 228) | 53 | −6.896 ± 0.334 | 2.332 ± 0.396 | −6.713 ± 0.021 | 2.070 ± 0.021 |
| O-029 (Collinder 232) | 12 | −6.667 ± 0.414 | 2.238 ± 0.294 | −6.552 ± 0.023 | 2.142 ± 0.023 |
| O-030 (Bochum 11) | 19 | −6.559 ± 0.204 | 2.328 ± 0.307 | −6.635 ± 0.021 | 2.279 ± 0.021 |
Notes. Group uncertainties reported in this work refer to the standard deviation of the selected OB stars while those in Villafranca II-III correspond to the standard deviation of the mean (with the angular covariance term included) of all the stars identified as group members, a much larger number than the one used in this work.
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