Table A.1
Stellar and wind parameters obtained from quantitative analysis of our sample of O Vz stars.
| VFTS | SpT | LC | M v 1 | v sin i | T eff | Δ T eff | log g | Δlog g2 | log gc3 | Y(He)4 | log Q | Δlog Q | log L/L⊙ 5 | Comments6 |
| [kms-1] | [K] | [K] | [dex] | [dex] | [dex] | [dex] | [dex] | [dex] | ||||||
|
|
||||||||||||||
| 355 | O4 | V((n))((fc))z | –5.1 | 135 | 43 400 | 600 | 3.84 | 0.10 | 3.85 | 0.09 | <–12.9 | – | 5.52 | NC |
| 418 | O5 | V((n))((fc))z | –4.4 | 135 | 43 200 | 1700 | 4.09 | 0.13 | 4.10 | 0.09 | –13.0 | 0.3 | 5.24 | SB? |
| 511 | O5 | V((n))((fc))z | –4.9 | 105 | 43 700 | 1700 | 4.25 | 0.11 | 4.25 | 0.10 | <–12.9 | – | 5.46 | SB1s |
| 398 | O5.5 | V((n))((f))z | –5.1 | 65 | 41 200 | 1000 | 4.03 | 0.10 | 4.03 | <0.06 | –12.6 | 0.2 | 5.47 | SBvs |
| 601 | O5-6 | V((n))z | –5.4 | 125 | 40 300 | 500 | 3.93 | 0.10 | 3.94 | 0.09 | –13.2 | 0.4 | 5.55 | ... |
| 096 | O6 | V((n))((fc))z | –5.7 | 125 | 40 100 | 500 | 3.90 | 0.10 | 3.91 | 0.09 | –13.0 | 0.2 | 5.67 | SBvs VM2 |
| 110 | O6 | V((n))z | –5.0 | 150 | 39 900 | 1000 | 3.86 | 0.10 | 3.88 | <0.06 | –12.8 | 0.2 | 5.40 | VM2? |
| 117 | O6: | Vz | –4.1 | 75 | 41 300 | 1500 | 4.14 | 0.16 | 4.14 | 0.12 | <–13.0 | – | 5.02 | SB? |
| 356 | O6: | V(n)z | –4.5 | 215 | 39 300 | 1300 | 3.99 | 0.13 | 4.03 | 0.10 | <–13.0 | – | 5.14 | SB? |
| 470 | O6: | V((f))z | –4.1 | 75 | 39 300 | 600 | 3.93 | 0.10 | 3.94 | 0.10 | –13.0 | 0.5 | 4.97 | ... |
| 472 | O6 | Vz | –4.1 | 40 | 40 400 | 900 | 4.12 | 0.12 | 4.12 | 0.11 | <–12.9 | – | 5.01 | ... |
| 488 | O6 | V((f))z | –4.8 | 55 | 40 700 | 700 | 3.87 | 0.10 | 3.87 | 0.09 | –12.8 | 0.2 | 5.33 | ... |
| 536 | O6 | Vz | –4.4 | 40 | 41 500 | 1500 | 4.23 | 0.15 | 4.23 | 0.09 | –13.3 | 0.6 | 5.19 | SB? |
| 089 | O6.5 | V((f))z Nstr | –4.3 | 50 | 39 700 | 700 | 4.02 | 0.12 | 4.02 | 0.13 | <–13.3 | – | 5.09 | ... |
| 123 | O6.5 | Vz | –4.0 | 65 | 40 400 | 700 | 4.10 | 0.12 | 4.10 | 0.13 | <–13.3 | – | 4.99 | SB? |
| 549 | O6.5 | Vz | –4.3 | 110 | 39 800 | 1200 | 4.04 | 0.16 | 4.05 | 0.09 | <–13.0 | – | 5.09 | SB? |
| 761 | O6.5 | V((n))((f))z Nstr | –4.1 | 110 | 40 300 | 700 | 4.15 | 0.10 | 4.16 | 0.18 | <–13.5 | – | 4.99 | NC |
| 380 | O6-7 | Vz | –3.9 | 65 | 39 100 | 700 | 4.13 | 0.10 | 4.13 | <0.09 | <–12.9 | – | 4.92 | ... |
| 392 | O6-7 | V((f))z | –4.5 | 40 | 37 600 | 800 | 3.87 | 0.10 | 3.87 | 0.10 | –13.1 | 0.2 | 5.11 | ... |
| 706 | O6-7 | Vnnz | –4.2 | 375 | 38 000 | 1200 | 3.80 | 0.13 | 3.95 | 0.11 | <–12.9 | – | 5.02 | ... |
| 722 | O7 | Vnnz | –4.1 | 405 | 36 600 | 800 | 3.84 | 0.10 | 4.01 | 0.11 | <–13.4 | – | 4.91 | SB? NC |
| 724 | O7 | Vnnz | –4.3 | 370 | 37 600 | 3300 | 3.78 | 0.41 | 3.93 | 0.19 | <–13.0 | – | 5.01 | NC |
| 849 | O7 | Vz | –4.1 | 95 | 39 800 | 600 | 4.16 | 0.11 | 4.17 | 0.11 | <–13.4 | – | 5.02 | NC |
| 751 | O7-8 | Vnnz | –4.4 | 360 | 36 000 | 1500 | 3.90 | 0.25 | 4.01 | 0.10 | <–13.0 | – | 5.01 | NC |
| 266 | O8 | V((f))z | –4.3 | 40 | 38 000 | 500 | 4.01 | 0.10 | 4.01 | 0.10 | –13.2 | 0.3 | 5.05 | ... |
| 014 | O8.5 | Vz | – | 90 | 37 100 | 600 | 3.91 | 0.10 | – | <0.06 | <–13.0 | – | – | SBs |
| 168 | O8.5 | Vz | –4.1 | 40 | 37 300 | 500 | 4.02 | 0.10 | 4.02 | 0.10 | <–13.8 | – | 4.92 | SB? |
| 252 | O8.5 | Vz | –3.6 | 100 | 37 000 | 500 | 4.21 | 0.10 | 4.22 | 0.11 | <–13.0 | – | 4.73 | ... |
| 638 | O8.5 | Vz | –3.5 | 45 | 36 900 | 500 | 4.20 | 0.10 | 4.20 | 0.10 | –13.1 | 0.3 | 4.68 | ... |
| 067 | O9.5 | Vz | –3.3 | 40 | 35 000 | 1100 | 4.12 | 0.19 | 4.12 | 0.08 | <–13.5 | – | 4.56 | SB? |
| 132 | O9.5 | Vz | –3.6 | 40 | 35 600 | 700 | 4.18 | 0.10 | 4.18 | 0.10 | <–13.5 | – | 4.71 | ... |
Notes.
Values taken from Maíz Apellániz et al. (in prep); the estimated average uncertainties are ΔMV = 0.3, accounting for uncertainties in the distance modulus (see Gibson 2000) and the apparent magnitudes.
log gc = log [g + (vsini)2/R∗] (see Herrero et al. 1992; Repolust et al. 2004).
The combined uncertainties in MV and Teff (from the IACOB-GBAT analysis) lead to an estimated average error in luminosity of Δlog L/L⊙ = 0.13 dex.
Relevant comments from Table 1 of Walborn et al. (in prep.): SB, spectroscopic binary; 1, single lined; 2, double lined; s, small amplitude (10–20 km s-1 ); vs, very small amplitude (<10 km s-1 ); SB?, stellar absorption displaced from nebular emission lines but no radial-velocity variation measured; SB2?, confirmed SB with possible second companion or unconfirmed SB but two companions visible in the line-of-sight; VMn, visual multiple of n components within the 1.2′′ Medusa fibre, as determined from HST/WFC3 images; NC, no WFC3 coverage.
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