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Table 3

Stellar parameters of stars that are considered in the discussion.

Star Spectral type Source log L⋆/L⊙ Teff T⋆ log Ṁ/ ν∞ ‡ ν∞ ▴ Y † N ★ log Q0 M ⋆ / M ⊙ ◆ Γe ◆ νsini Source M V R V E(B − V) E(V − Ks)
VFTS [kK] [kK] [M⊙/yr] [km s-1] [km s-1] [ph s-1] [km s-1] [mag]
016 O2 III-If* 1 6.23 53.1 54.1 –5.4 3400 3410 0.25 ne 50.08 120 0.38 94 i –6.1 3.34 0.356 1.046
064 O7.5 II(f) 1 6.0 39.8 39.9 –5.4 – 2640 0.25 e 49.68 88 0.3 104 i –6.5 5.85 0.45 2.266
072 O2 V-III(n)((f*)) 1 5.96 50.1 50.7 –5.8 – 3340 0.25 e 49.75 84 0.29 200 i –5.7 4.84 0.18 0.755
108 WN7h 3 5.7 39.8 53.1 –4.0 1000 1950 0.775 e 49.50 33# 0.29 < 200 iii –5.9 4.28 0.311 1.157
169 O2.5 V(n)((f*)) 1 5.89 47.3 47.7 –5.5 – 3200 0.25 n 49.70 76 0.27 200 ii –5.7 5.07 0.35 1.534
171 O8 II-III(f) 1 5.59 37.6 37.7 –5.7 – 2670 0.25 ne 49.18 54 0.19 81 i –5.7 4.63 0.268 1.077
180 O3 If* 4 5.92 42.2 42.3 –5.0 2500 2360 0.55 e 49.65 58 0.32 93 i –6.1 4.89 0.237 1.004
216 O4 V((fc)) 1 5.84 44.7 44.9 –5.7 – 3040 0.25 n 49.62 72 0.26 100 ii –5.7 2.91 0.571 1.474
259 O6 Iaf 1 6.1 37.6 37.7 –5.0 – 2350 0.325 e 49.71 94 0.35 66 i –7.0 4.0 0.529 1.844
267 O3 III-I(n)f* 1 6.01 44.7 44.9 –5.1 – 2960 0.25 ne 49.79 89 0.31 145 i –6.2 4.35 0.27 1.02
333 O8 II-III((f)) 1 6.02 37.6 37.7 –5.4 – 2490 0.25 n 49.61 90 0.31 77 i –6.8 2.91 0.258 0.666
404 O3.5 V(n)((fc)) 1 5.91 44.7 44.9 –5.8 – 3010 0.25 n 49.69 78 0.28 – – –5.9 4.57 0.341 1.352
422 O4 III(f) 1 5.7 39.8 39.9 –5.6 – 2770 0.25 ne 49.38 61 0.22 356 i –5.8 4.3 0.56 2.093
427 WN8(h) 3 6.13 39.8 41.6 –3.9 1000 1610 0.925 e 49.90 48# 0.46 < 200 iii –7.0 4.16 0.534 1.934
455 O5: V:n 1 5.63 42.2 42.3 –5.6 – 2970 0.25 ne 49.36 56 0.2 – – –5.4 3.7 0.47 1.525
457 O3.5 If*/WN7 4 6.2 39.8 39.9 –4.6 1800 2340 0.4 e 49.89 100 0.39 < 200 iii –7.0 2.83 0.806 2.015
482 O2.5 If*/WN6 4 6.4 42.2 42.3 –4.4 2600 2540 0.325 e 50.14 145 0.45 < 200 iii –7.3 3.85 0.436 1.467
506 ON2 V((n))((f*)) 1 6.24 47.3 47.7 –5.6 – 3040 0.25 e 50.05 122 0.38 100 ii –6.5 3.99 0.341 1.187
512 O2 V-III((f*)) 1 6.04 47.3 47.7 –5.6 – 3120 0.25 ne 49.86 93 0.32 – – –6.1 3.57 0.52 1.628
518 O3.5 III(f*) 1 5.75 44.7 44.9 –5.5 – 3090 0.25 e 49.53 65 0.23 91 i –5.5 3.6 0.591 1.864
532 O3 V(n)((f*))z + OB 1 5.74 44.7 44.9 –5.8 – 3090 0.25 n 49.52 64 0.23 – – –5.5 3.36 0.521 1.542
542 O2 If*/WN5 4 6.16 44.7 44.9 –4.6 2700 2520 0.475 e 49.94 87 0.39 < 200 iii –6.5 3.71 0.408 1.324
545 O2 If*/WN5 4 6.3 47.3 47.7 –4.6 2800 3020 0.25 e 50.11 133 0.4 < 200 iii –6.7 3.67 0.436 1.421
566 O3 III(f*) 1 5.85 44.7 44.9 –5.4 – 3030 0.25 e 49.63 73 0.26 91 i –5.8 3.48 0.381 1.162
599 O3 III(f*) 1 5.99 44.7 44.9 –5.3 – 2970 0.25 e 49.77 87 0.3 113 i –6.1 3.55 0.401 1.248
603 O4 III(fc) 1 5.98 42.2 42.3 –5.4 – 2810 0.25 ne 49.71 85 0.3 – – –6.3 4.9 0.360 1.528
608 O4 III(f) 1 5.86 42.2 42.3 –5.4 – 2860 0.25 e 49.60 74 0.26 – – –6.0 3.54 0.481 1.49
617 WN5ha 8 6.29 53.1 53.7 –4.3 2800 2650 0.625 e 50.14 90 0.46 < 200 iii –6.3 4.5 0.212 0.848
621 O2 V((f*))z 1 6.14 50.1 50.7 –5.8 – 3260 0.25 e 49.97 107 0.35 80 ii –6.1 5.09 0.591 2.595
626 O5–6 n(f)p 1 5.6 39.8 39.9 –5.5 – 2590 0.4 e 49.27 46 0.21 278 i –5.5 3.28 0.581 1.679
664 O7 II(f) 1 5.72 39.8 39.9 –5.5 – 2760 0.25 e 49.40 62 0.23 63 i –5.8 3.39 0.46 1.371
669 O8 Ib(f) 1 5.71 37.6 37.7 –5.6 – 2510 0.325 e 49.31 57 0.23 64 i –6.0 2.8 0.590 1.466
682 WN5h 2 6.51 52.1 54.4 –4.2 2600 2860 0.45 e 50.35 153 0.51 < 200 iii –6.9 4.74 0.941 3.863
695 WN6h + ? 2 6.5 39.8 39.9 –3.7 1600 1620 0.85 e 50.22 96# 0.58 <200 iii –7.8 4.42 0.315 1.211
755 O3 Vn((f*)) 1 5.64 47.3 47.7 –6.0 – 3330 0.25 n 49.45 57 0.2 285 ii –5.1 2.86 0.561 1.421
758 WN5h 2 6.36 47.3 47.6 –3.9 2000 2090 0.775 e 50.17 84# 0.51 <200 iii –7.0 3.63 0.428 1.362
797 O3.5 V((n))((fc)) 1 5.57 44.7 44.9 –6.1 – 3180 0.25 n 49.35 53 0.19 140 ii –5.1 3.38 0.372 1.106
1001 WN6(h) 5 6.2 39.8 42.2 –3.8 1100 1700 0.85 e 49.96 60# 0.47 < 200 iii –7.4 2.93 0.523 1.36
1017 O2 If*/WN5 4 6.21 50.1 50.5 –4.5 2700 2670 0.55 e 50.04 86 0.42 < 200 iii –6.3 3.87 0.597 2.015
1018 O3 III(f*) + mid/late O 5,6 5.92 42.2 42.3 –5.9 – 2830 0.25 n 49.65 79 0.28 – – –6.1 4.15 0.507 1.83
1021 O4 If+ 5 6.34 39.8 39.9 –4.6 – 2530 0.25 e 50.02 141 0.41 < 200 iii –7.3 4.16 0.519 1.881
1022 O3.5 If*/WN7 4 6.48 42.2 42.3 –4.3 2700 2670 0.25 ne 50.22 178 0.46 < 200 iii –7.5 4.36 0.567 2.149
1025 WN5h 7 6.58 42.2 42.3 –3.9 – 1910 0.7 e 50.32 132 0.58 < 200 iii –7.9 4.5 0.608 2.373
Mk42 O2 If* 4 6.56 47.3 47.7 –4.6 2800 2840 0.325 e 50.37 189 0.49 < 200 iii –7.4 4.09 0.4 1.426

Notes. Sources: (1)Walborn et al. (2014); (2)Evans et al. (2011); (3)Crowther & Smith (1997); (4)Crowther & Walborn (2011); (5)Massey & Hunter (1998); (6)Hénault-Brunet et al. (2012); (7)Crowther & Dessart (1998); (8)Foellmi et al. (2003); (9)Melnick (1985); (10)Walborn & Blades (1997). () Stellar masses and Eddington factors under the assumption of He-core burning using the relation by Gräfener et al. (2011): VFTS 108 (20 M⊙, 0.29), 427 (38 M⊙, 0.46), 695 (72 M⊙, 0.58), 758 (55 M⊙, 0.51), and 1001 (42 M⊙, 0.47). Sources for νsini: (i) Ramírez-Agudelo et al. (2013); (ii) Sabín-Sanjulián et al. (2014); (iii) conservative upper limits from this work.

(†)

Y is the helium mass fraction;

(‡)

measured ν∞;

(▴)

calculated ν∞ using Lamers et al. (1995) with Eq. (6), nitrogen abundance: n for normal, ne for between normal and enhanced, and e for enhanced;

(◆)

using the mass-luminosity relation for chemical homogeneity by Gräfener et al. (2011).

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