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Table D.1

Models which are able to achieve the best fit for each individual Wolf–Rayet star.

SMC M0 vrot ,0 T* log L XH vsini; vrot Pinc
AB [ M] [km s−1] [kK] [L] [km s−1]
1 (obs) <100 0.044 11.6
model 100 590 59 6.25 0.48 342
2 (obs) <50 0.014 0.29
model 35 400 47 5.54 0.53 302
4 (obs) <100 0.16 3.07
model 35 420 50 5.81 0.29 183
9 (obs) <200 0.40 45.3
model 70 600 60 6.12 0.32 251
10 (obs) <200 0.36 49.6
model 55 600 60 5.98 0.29 259
11 (obs) <200 0.34 26.1
model 100 600 62 6.31 0.37 267
12 (obs) <200 1 49.9
model 100 600 77 6.31 0.02 13

Notes. For each object we display the initial mass and initial rotation velocity of the best-fitting models and we compare the observed values (Hainich et al. 2015) of the fit parameters to their model values at the momentthe best fit is achieved. Next, we display the observed upper limit on the rotational velocity v sin i and the model vrot at the moment the best fit is achieved. For models where vrot exceeds the observedupper limit on vsini we calculate Pinc, i.e., the chance that vsini does not exceed the upper limit due to a low inclination of the rotational axis. is the lowest χ2 value achieved with our three fit parameters T*, log L and XH . In this table, only single stars are considered and compared to models that are core hydrogen burning.

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