Table 7.
Results of the maximum likelihood analysis using the Gaia EDR3 data, showing the best-fit subcluster positions and standard deviations in parallax-proper motion space.
| EDR3 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Subcluster/ | ϖ | σϖ | μα | σμα | μδ | σμδ | Nr. of | Distance |
| Population | (mas) | (mas) | (mas yr−1) | (mas yr−1) | (mas yr−1) | (mas yr−1) | Stars | (pc) |
| A | 1.101±0.006 | 0.130 | −2.432±0.020 | 0.412 | −4.719±0.015 | 0.308 | 418 | 908±73 |
| B | 1.098±0.022 | 0.128 | −2.251±0.063 | 0.360 | −3.131±0.044 | 0.252 | 33 | 911±75 |
| C | 1.002±0.013 | 0.035 | −1.835±0.034 | 0.091 | −6.603±0.091 | 0.241 | 7 | 998±61 |
| D | 0.963±0.030 | 0.090 | −3.876±0.087 | 0.260 | −2.954±0.100 | 0.301 | 9 | 1038±48 |
| E | 1.075±0.016 | 0.060 | −1.374±0.036 | 0.133 | −3.424±0.054 | 0.201 | 14 | 931±62 |
| F | 1.092±0.032 | 0.085 | −3.632±0.046 | 0.121 | −3.883±0.054 | 0.143 | 7 | 916±46 |
| G | 0.997±0.029 | 0.229 | −1.909±0.645 | 5.159 | −3.124±0.524 | 4.192 | 64 | 1003±70 |
Notes. The parallax and proper motion errors are listed here as the standard errors in the mean for each parameter, which define the mean properties of each subcluster. The σϖ, σμα, and σμδ are the standard deviation or the intrinsic dispersion of the astrometric parameters. Note the large scatter in the parameters of population G, which renders it unusable to identify new members. The final column shows the average distance for each group and its error.
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