Table 1
Parameters of the suspected rapid rotators.
| Object | BAT99 7 | BAT99 51 | BAT99 88 | BAT99 94 | WR 2 |
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| Spectral type | WN4b | WN3b | WN4b/WCE | WN4b | WN2-w |
| T∗ [kK] | 141 | 89 | 112 | 141 | 141 |
| log Rt [R⊙] | 0.1 | 0.6 | 0.4 | 0.0 | 0.5 |
| R∗ [R⊙] | 1.3 | 1.9 | 2.1 | 1.3 | 0.9 |
| log Ṁ [M⊙ yr-1] | −4.5 | −5.2 | −4.8 | −4.4 | −5.3 |
| log L [L⊙] | 5.84 | 5.30 | 5.80 | 5.80 | 5.45 |
| M [M⊙] | 26 | 13 | 25 | 25 | 16 |
| η mom | 5.5 | 2.5 | 2.0 | 6.2 | 1.6 |
| X N | 0.015 a | 0.01 | 0.008 | 0.01 | 0.001 |
| X C | 7 × 10-5 | 7 × 10-5 | 0.005 a | 7 × 10-5 | 1 × 10-4 |
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| v∞ [km s-1] | 2400 | 1600 | 1600 | 2000 | 1800 |
| vcorsini [km s-1] | 2500 ± 500 | 2000 ± 400 | 1700 ± 340 | 2500 ± 500 | 3000 ± 600 |
| Rcor [R∗] | 16 ± 5 | 10 ± 3 | 12 ± 4 | 12 ± 4 | 6 ± 2 |
| v∗sini [km s-1] | 160 ± 80 | 200 ± 100 | 140 ± 70 | 210 ± 100 | 500 ± 250 |
Notes. The stellar parameters not involving the velocity field (upper part) were primarily adopted from Hainich et al. (2014) for the LMC stars, and from Hamann et al. (2006) for WR 2. All sampled stars are calculated with Fe mass fractions of XFe = 7 × 10-4. The LMC stars are calculated with a clumping factor of D = 10, while D = 4 was adopted for WR 2. The uncertainties are discussed in Sect. 4.5.
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