Table 6
Parameters of the 1D velocity distributions determined in the mass bins and age bins shown in Fig. 9.
| Mass | t/tMS | # | Slow rotators | Fast rotators | ||||||||
| range | range | Stars | ĥ | μs | dispersion | % |
|
ℓ | μr |
|
dispersion | κr |
| (M⊙) | (km s-1) | (km s-1) | (km s-1) | (km s-1) | (km s-1) | (km s-1) | (km s-1) | |||||
|
|
||||||||||||
| 1.60–2.40 | 0.0–0.5 | 134 | 0.228 | — | — | 100 | 138 ± 1 | 26 ± 1 | 164 | 148 | 65 | 1.005 |
| 1.60–2.40 | 0.5–0.8 | 217 | 0.204 | — | — | 100 | 127 ± 1 | 52 ± 1 | 179 | 172 | 61 | 0.979 |
| 1.60–2.40 | 0.8–1 | 108 | 0.236 | — | — | 100 | 141 ± 1 | 40 ± 1 | 181 | 184 | 67 | 0.995 |
| 2.40–3.85 | 0.0–0.5 | 84 | 0.317 | 47 ± 1 | 22 | 89 | 221 ± 3 | 24 ± 3 | 245 | 241 | 105 | 1.101 |
| 2.40–3.85 | 0.5–0.8 | 188 | 0.268 | 49 ± 1 | 23 | 88 | 193 ± 2 | 15 ± 3 | 208 | 196 | 92 | 1.103 |
| 2.40–3.85 | 0.8–1 | 215 | 0.276 | 43 ± 1 | 20 | 88 | 184 ± 1 | 0 ± 1 | 184 | 184 | 88 | 1.053 |
Notes. As in Table 4, the corresponding number of normal stars and the smoothing parameter ĥ (expressed in logarithmic vsini) are given for each subsample. For each distribution, the parameters of the Maxwellian fit are listed: percentage of fast velocity distributions, mode and dispersion. The mode of the slow rotator distribution μs is derived from the Maxwellian fit. The fast rotator distribution is a lagged Maxwellian (see text and footnote2) and its mode is 
. The estimator 
was derived as the position of the maximum directly on the 1D fast distributions. Correction factors κr were derived as 
, where ⟨ v ⟩ is the mean of the full distribution.
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