Table 1
Bayesian expansion ages of local young stellar associations.
RV | Members | Distance | Age | |||
---|---|---|---|---|---|---|
Origin | Coverage | final | μ ± σ | |||
% | (pc) | (Myr) | ||||
Association | Membership | |||||
EPCHA | SigMA | GLASSS | 37.8 | 37 | 102 | 6.4 ± 2.1 |
MuscaFG | UNION-A | GLASSS | 53.8 | 39 | 101 | 10.4 ± 1.4 |
ETCHA | UNION | GLASSS | 60.0 | 20 | 98 | 7.6 ± 3.4 |
TWA | L23-A | GLASSS | 58.5 | 41 | 63 | 10.2 ± 1.0 |
L23-B | GLASSS | 53.3 | 15 | 65 | 8.5 ± 1.3 | |
118TAU | UNIONS+L22-A | GLASSS | 60.0 | 35 | 107 | 24.0 ± 4.5 |
THOR | UNIONS+L22-B | GLASSS | 66.7 | 45 | 101 | 29.8 ± 4.9 |
Háap | UNIONS+L22-C | GLASSS | 55.6 | 63 | 90 | 25.9 ± 4.6 |
BPIC | Miret-Roig+2020 | Original | 73.1 | 26 | 42 | 23.4 ± 4.8 |
Balaam | Luhman2024-B | Original | 47.6 | 63 | 63 | 19.3 ± 4.7 |
OCT | UNION-A | GLASSS | 81.2 | 69 | 150 | 30.4 ± 4.6 |
HSC2597 | UNION-C | GLASSS | 41.2 | 17 | 138 | 39.6 ± 6.9 |
COL | UNION-A | GLASSS | 59.2 | 125 | 71 | 33.0 ± 9.2 |
OMAU | UNION-C | GLASSS | 46.7 | 15 | 36 | 40.1 ± 5.9 |
CAR | Luhman2024-AB | GLASSS | 44.8 | 259 | 112 | 45.4 ± 9.2 |
Platais8 | Luhman2024-AA | GLASSS | 42.0 | 362 | 133 | 28.3 ± 10.9 |
Nal | Luhman2024-BA | GLASSS | 11.4 | 35 | 183 | 16.1 ± 5.5 |
Chem | Luhman2024-BB | GLASSS | 30.3 | 132 | 168 | 22.2 ± 2.1 |
THA | Lee+2019-A | GLASSS | 58.4 | 161 | 42 | 32.9 ± 6.3 |
Lee+2019-B | GLASSS | 54.1 | 37 | 43 | 38.6 ± 5.4 |
Notes. The columns in this table correspond, from left to right, to the association’s abbreviated name, the selected membership’s list (the reasons for this selection will be described at each LYSA’s section), the RV origin and percentage of coverage (out of the final members), the final number of members (after the decontamination algorithm), the association’s distance, and the inferred Bayesian expansion age. For simplicity, the age is reported as the mean and standard deviation of the inferred age’s posterior distribution. Its 95% HDI (high density interval) is reported in Table B.1.
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