Table 4
Parameters of the 1D velocity distributions for normal stars as a function of the stellar mass.
| Mass | # | Slow rotators | Fast rotators | |||||||||
| range | Stars | ĥ | % | μs |
|
dispersion | % |
|
ℓ | μr |
|
dispersion |
| (M⊙) | (km s-1) | (km s-1) | (km s-1) | (km s-1) | (km s-1) | (km s-1) | (km s-1) | (km s-1) | ||||
|
|
||||||||||||
| ∗ 1.60–2.00 | 191 | 0.200 | — | — | — | — | 100 | 114 ± 1 | 46 ± 1 | 160 | 148 | 54 |
| 1.70–2.10 | 216 | 0.194 | — | — | — | — | 100 | 124 ± 1 | 46 ± 1 | 170 | 151 | 59 |
| 1.80–2.20 | 220 | 0.177 | — | — | — | — | 100 | 128 ± 1 | 48 ± 1 | 176 | 160 | 61 |
| ∗ 1.90–2.30 | 249 | 0.190 | — | — | — | — | 100 | 133 ± 1 | 44 ± 1 | 177 | 169 | 63 |
| 2.00–2.40 | 276 | 0.201 | — | — | — | — | 100 | 140 ± 1 | 45 ± 1 | 185 | 181 | 67 |
| 2.10–2.50 | 274 | 0.227 | 3 | 25 ± 1 | 22 | 12 | 97 | 154 ± 1 | 27 ± 1 | 181 | 181 | 73 |
| ∗ 2.20–2.60 | 273 | 0.247 | 8 | 37 ± 1 | 43 | 18 | 92 | 164 ± 1 | 18 ± 1 | 183 | 184 | 78 |
| 2.30–2.70 | 248 | 0.260 | 12 | 44 ± 1 | 43 | 21 | 88 | 179 ± 1 | 12 ± 2 | 191 | 187 | 85 |
| 2.35–2.85 | 282 | 0.259 | 12 | 47 ± 1 | 49 | 22 | 88 | 210 ± 1 | 0 ± 1 | 210 | 178 | 100 |
| ∗ 2.45–2.95 | 274 | 0.254 | 18 | 52 ± 1 | 46 | 25 | 82 | 185 ± 3 | 14 ± 4 | 199 | 193 | 88 |
| 2.55–3.05 | 235 | 0.254 | 20 | 61 ± 1 | 52 | 29 | 80 | 191 ± 2 | 20 ± 3 | 211 | 214 | 91 |
| 2.65–3.15 | 209 | 0.253 | 15 | 55 ± 1 | 46 | 26 | 85 | 183 ± 2 | 24 ± 3 | 208 | 205 | 87 |
| ∗ 2.65–3.35 | 259 | 0.249 | 14 | 52 ± 1 | 43 | 25 | 86 | 187 ± 2 | 29 ± 3 | 216 | 214 | 89 |
| 2.75–3.45 | 225 | 0.270 | 13 | 47 ± 1 | 40 | 22 | 87 | 201 ± 2 | 18 ± 3 | 219 | 217 | 96 |
| 2.85–3.55 | 190 | 0.278 | 10 | 39 ± 1 | 37 | 19 | 90 | 202 ± 2 | 20 ± 2 | 222 | 217 | 96 |
| ∗ 2.95–3.65 | 153 | 0.290 | 6 | 32 ± 1 | 31 | 15 | 94 | 224 ± 2 | 0 ± 1 | 224 | 220 | 107 |
| 3.05–3.75 | 131 | 0.301 | 5 | 31 ± 1 | 31 | 15 | 95 | 229 ± 1 | 0 ± 1 | 229 | 190 | 109 |
| 3.15–3.85 | 122 | 0.314 | 8 | 32 ± 1 | 28 | 15 | 92 | 224 ± 2 | 15 ± 2 | 238 | 220 | 107 |
Notes. The defined mass ranges and the corresponding number of normal stars are given. The smoothing parameter ĥ is given for each subsample, it is expressed in logarithmic vsini. For each distribution, the parameters of the Maxwellian fit are listed: percentage of slow and fast velocity distributions, mode and dispersion. For slow rotators, the distribution mode μs is derived from the Maxwellian fit. The fast rotator distribution is a lagged Maxwellian (see text and footnote2), and its mode is 
, where α is the parameter of the Maxwellian distribution. The estimators μ′ are derived as the position of the maximum directly on the 1D distributions. The distributions are shown in Fig. 6 for six of the eighteen mass ranges, indicated by asterisks.
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