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Table 1.

Binary star physical properties.

O-star Adopted Adopted Mass at Period
Spectral mass mass mass end CHeB Present at end LX time LX time
System type est. (WR) (O) (WR) period CHeB (Myr) (Myr)/0.4
WR21 WN5+O4-5 37–60 > 19 > 37 > 10 8.3 11.8 0.3 0.8
WR30 WC6+O6-8 24–50 16 34 14 18.8 20.4 0.0 0.0
WR31 WN4+O8V 24–34 > 11 > 24 > 7 4.8 6.1 2.5 6.3
WR35a WN6+O8.5V 19–33 18 19 10 41.9 68.2 0.0 0.0
WR42 WC7+O7V 27–37 16 27 14 7.9 8.7 1.8 4.5
WR47 WN6+O5V 37–70 > 40 > 47 > 20 6.2 10.5 0.6 1.5
WR79 WC7+O5-8 24–60 > 10 > 24 > 7 8.9 10.7 1.1 2.8
WR97 WN5+O7 > 30 > 17 > 30 > 9 12.6 18.3 0.0 0.0
WR113 WC8+O8-9IV 20–30 > 11 > 22 > 8 29.7 35.9 0.0 0.0
WR11 WC8+O7.5III-V 25–47 10 31 8 78.5 86.8 0.0 0.0
WR127 WN3+O8.5V 17–24 > 9 > 20 > 6 9.5 11.8 0.8 2.0
WR139 WN5+O6III-V 28–59 9 28 6 4.2 5.0 3.0 7.5
WR151 WN4+O5V 28–56 20 28 10 2.1 3.4 5.7 14.3
WR133 WN5+O9I 34–66 17 34 9 112.4 158.1 0.0 0.0
WR141 WN5+O5III-V 26–59 36 26 18 21.7 43.1 0.0 0.0
WR155 WN6+O9II-Ib 30–44 24 30 12 1.6 2.6 1.5 3.8
WR9 WC5+O7 > 30 9 32 8 14.3 15.0 0.1 0.3

Notes. For the selected observed WR+O binaries, the mass-range of the O star based on its spectral type and luminosity class, the adopted WR and O masses based on all available data, the estimated mass of the WR star at the end of core helium burning, the present observed period and the estimated period at the end of the core helium burning phase of the WR star, the time (in Myr) where the resulting wind-fed BH+O is observable as a X-ray binary, and finally the number of expected wind-fed BH high-mass X-ray binaries. Masses are in M and periods are in days.

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