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Table C.4

Best-fitting atmospheric and wind parameters of our sample stars.

VFTS SpT M K T eff log  g log  gc a log  Y b νturb νesini ν log  L R log  Dmom M spec c M evol
(mag) (kK) (cm s-2) (cm s-2) (M yr-1) (kms-1) (kms-1) (kms-1) (L) (R) (g cm s-2) (M) (M)

016 O2III-If* –5.3
035 O9.5IIIn –2.4
046 O9.7II((n)) –4.5
070 O9.7II –2.7
076 O9.2III –4.1
077 O9.5:IIIn –2.5
080 O9.7II-III((n)) –3.3
087 O9.7Ib-II –4.9
091 O9.5IIIn –3.4
103 O8.5III((f)) –4.3
104 O9.7II-III((n)) –2.4
109 O9.7II:n –3.0
113 O9.7IIorB0IV? –2.5
128 O9.5III:((n)) –2.5
141 O9.5II-III((n)) –3.5
151 O6.5II(f)p –5.7
153 O9III((n)) –4.2
160 O9.5III((n)) –4.9
172 O9III((f)) –2.5
178 O9.7Iab –5.9
180 O3If* –5.4
185 O7.5III((f)) –4.5
188 O9.7:III: –3.0
192 O9.7IIorB0IV? –2.3
205 O9.7II((n))orB0IV((n))? –2.8
207 O9.7II((n)) –2.7
210 O9.7II-III((n)) –3.0
226 O9.7III –2.5
235 O9.7III –3.0
244 O5III(n)(fc) –4.7
253 O9.5II –3.7
259 O6Iaf –6.1
267 O3III-I(n)f* –5.4
304 O9.7III –2.4
306 O8.5II((f)) –5.0
328 O9.5III(n) –2.5
346 O9.7III –2.9
370 O9.7III –2.8
399 O9IIIn –3.7
466 O9III –4.4
495 O9.7II-IIIn –2.9
502 O9.7II –5.6
503 O9III –4.2
513 O6-7II(f) –3.4
518 O3.5III(f*) –4.6
546 O8-9III:((n)) –3.9
566 O3III(f*) –5.0
569 O9.2III: –3.3
571 O9.5II-III(n) –2.6
574 O9.5IIIn –2.5
599 O3III(f*) –5.3
607 O9.7III –2.8
615 O9.5IIInn –3.9
620 O9.7III(n) –2.3
622 O9.7III –2.2
664 O7II(f) –5.0
669 O8Ib(f) –5.1
711 O9.7III –3.2 39
753 O9.7II-III –3.4
764 O9.7Ia –6.4
777 O9.2II –5.0
782 O8.5III –4.3
787 O9.7III –2.8
807 O9.5III –3.4
819 ON8III((f)) –3.2
843 O9.5IIIn –2.7

Newly identified spectroscopic binaries

064* O7.5II(f) –5.5
093* O9.2III-IV –3.8
171* O8II-III(f) –4.9
332* O9.2II-III –4.8
333* O8II-III((f)) –6.0
440* O6-6.5II(f) –5.4

Notes. Parameters of stars that include nitrogen in the spectral analysis are marked with in the first column (see also list in Table C.1). Newly detected binaries fits are listed separately. The quoted uncertainties identify the locations, with respect to the best-fit values, of the upper and lower boundaries of the 95% confidence intervals. They reflect statistical uncertainties of the fitting process and hence do not account for systematic uncertainties (see Sects. 3.2 and 3.3).

(a)

log  gc = log  [ g + (νesini)2/R ];

(b)

Y is the helium mass fraction;

(c)

Spectroscopic mass computed with Newtonian gravity (gc).

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