Table 2
Eclipsing O-star binaries with dynamical mass estimates.
| Star | Sp Type | mdynamical | mMSH1 | mMSH2 | mini | mevol | mstart | mend | Ref. |
|
|
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| MW | |||||||||
| HD93205A | O3V | 56.0 ± 4.0 | 58.3 | 58.0 | 67 –9/+9 | 65 –7/+7 | 67 –9/+6 | 64 –6/+8 | (1) |
| FO15 A | O5.5V | 30.0 ± 1.0 | 34.2 | 34.4 | 40 –7/+8 | 39 –6/+7 | 39 –6/+6 | 38 –5/+7 | (2) |
| FO15 B | O9.5V | 16.0 ± 1.0 | 16.5 | 15.6 | 18 –5/+4 | 18 –5/+4 | 18 –5/+4 | 18 –5/+4 | (2) |
| Theta Orionis C1 | O6Vpe | 35.8 ± 7.2 | 31.7 | 31.0 | 35 –7/+6 | 34 –6/+5 | 34 –6/+5 | 33 –6/+6 | (3) |
| V1036 Sco A | O6V | 32.0 ± 4.0 | 31.7 | 31.0 | 35 –7/+6 | 34 –6/+5 | 34 –6/+5 | 33 –6/+6 | (4) |
| V1036 Sco B | O7V | 32.0 ± 4.0 | 26.5 | 25.3 | 28 –6/+8 | 27 –5/+7 | 27 –5/+6 | 27 –5/+7 | (4) |
| LS1135 A | O6.5V | 30.0 ± 1.0 | 29.0 | 28.0 | 31 –7/+6 | 30 –6/+6 | 30 –6/+5 | 30 –6/+6 | (5) |
| V729 Cyg | O7Ianfp | 47.0 ± 9.0 | 40.9 | 38.4 | 47 –9/+36 | 39 –5/+23 | 40 –6/+23 | 39 –5/+24 | (4) |
| V1007 Sco A | O7.5IIIa | 29.5 ± 0.4 | 29.1 | 27.4 | 33 –5/+6 | 31 –4/+4 | 31 –5/+4 | 31 –4/+5 | (6) |
| V1007 Sco B | O7IIIa | 30.1 ± 0.4 | 31.2 | 29.6 | 36 –5/+7 | 34 –4/+5 | 34 –4/+5 | 33 –4/+5 | (6) |
| V3903 Sgr A | O7V | 27.3 ± 6.0 | 26.5 | 25.3 | 28 –6/+8 | 27 –5/+7 | 27 –5/+6 | 27 –5/+7 | (4) |
| V3903 Sgr B | O9V | 19.0 ± 4.0 | 18.0 | 17.1 | 19 –5/+5 | 19 –5/+4 | 19 –5/+4 | 19 –5/+4 | (4) |
| CPD –59 2603 A | O7V | 22.7 ± 4.0b | 26.5 | 25.3 | 28 –6/+8 | 27 –5/+7 | 27 –5/+6 | 27 –5/+7 | (4) |
| CPD –59 2603 B | O9.5V | 14.5 ± 4.0b | 16.5 | 15.6 | 18 –5/+4 | 18 –5/+4 | 18 –5/+4 | 18 –5/+4 | (4) |
| V1182 Aql A | O8Vnn | 31.0 ± 0.6 | 21.9 | 20.8 | 23 –6/+6 | 22 –5/+6 | 22 –5/+6 | 22 –5/+6 | (7) |
| EM Car A | O8V | 22.9 ± 3.0 | 21.9 | 20.8 | 23 –6/+6 | 22 –5/+6 | 22 –5/+6 | 22 –5/+6 | (4) |
| EM Car B | O8V | 21.4 ± 3.0 | 21.9 | 20.8 | 23 –6/+6 | 22 –5/+6 | 22 –5/+6 | 22 –5/+6 | (4) |
| CC Cas | O8.5III | 18.3 ± 5.0 | 24.8 | 23.7 | 29 –5/+6 | 27 –4/+5 | 27 –4/+5 | 27 –4/+5 | (4) |
| WR22 B | O9V | 20.6 ± 1.7 | 18.0 | 17.1 | 19 –5/+5 | 19 –5/+4 | 19 –5/+4 | 19 –5/+4 | (8) |
| V478 Cyg A | O9.5V | 16.6 ± 9.0 | 16.5 | 15.6 | 18 –5/+4 | 18 –5/+4 | 18 –5/+4 | 18 –5/+4 | (4) |
| V478 Cyg B | O9.5V | 16.3 ± 9.0 | 16.5 | 15.6 | 18 –5/+4 | 18 –5/+4 | 18 –5/+4 | 18 –5/+4 | (4) |
| CPD –59 2628 A | O9.5V | 14.0 ± 20.0 | 16.5 | 15.6 | 18 –5/+4 | 18 –5/+4 | 18 –5/+4 | 18 –5/+4 | (4) |
|
|
|||||||||
| LMC | |||||||||
| LMC MACHO 053441.3 A | O3If | 41.2 ± 12.0 | 66.9 | 67.5 | 81 –10/+9 | 72 –8/+9 | 82 –10/+6 | 76 –5/+7 | (4) |
| LMC MACHO 053441.3 B | O6V | 27.0 ± 12.0 | 31.7 | 31.0 | 37 –5/+3 | 36 –4/+3 | 37 –5/+3 | 36 –4/+3 | (4) |
| LMC R136–38 A | O3V | 56.9 ± 6.0 | 58.3 | 58.0 | 64 –7/+7 | 64 –7/+7 | 64 –7/+7 | 64 –7/+7 | (4) |
| LMC R136–38 B | O6V | 23.4 ± 2.0 | 31.7 | 31.0 | 37 –5/+3 | 36 –4/+3 | 37 –5/+3 | 36 –4/+3 | (4) |
| LMC R136–42 A | O3V | 40.3 ± 1.0 | 58.3 | 58.0 | 64 –7/+7 | 64 –7/+7 | 64 –7/+7 | 64 –7/+7 | (4) |
| LMC R136–42 B | O3V | 32.6 ± 1.0 | 58.3 | 58.0 | 64 –7/+7 | 64 –7/+7 | 64 –7/+7 | 64 –7/+7 | (4) |
| LH 54–425 A | O3V | 50.0 ± 10.0 | 58.3 | 58.0 | 64 –7/+7 | 64 –7/+7 | 64 –7/+7 | 64 –7/+7 | (9) |
| LH 54–425 B | O5V | 30.0 ± 6.0 | 37.3 | 38.1 | 44 –5/+5 | 44 –5/+5 | 44 –5/+4 | 43 –4/+5 | (9) |
| LMC R136–77 A | O5.5V | 28.9 ± 3.0 | 34.2 | 34.4 | 40 –5/+4 | 40 –5/+4 | 40 –5/+4 | 39 –4/+4 | (4) |
| LMC R136–77 B | O5.5V | 26.2 ± 3.0 | 34.2 | 34.4 | 40 –5/+4 | 40 –5/+4 | 40 –5/+4 | 39 –4/+4 | (4) |
| LMC–SC1–105 A | O7V | 30.9 ± 1.0 | 26.5 | 25.3 | 31 –5/+3 | 30 –4/+3 | 31 –5/+3 | 30 –4/+3 | (10) |
Notes. For these massive stars dynamical mass estimates, mdyn, exist from the orbits of binaries. The other mass estimates are from the theoretical Teff calibration (mMSH1) and observational Teff calibration (mMSH2) by MSH05, together with the initial (mini), mean evolutionary (mevol), minimal (mstart) and maximal (mend) present-day mass from this work. The horizontal lines separates objects in the LMC from Galactic ones. All masses are in M⊙. For the Milky Way stars Table 4 was used to derive the masses and for the LMC stars Table 6.
Different luminosity class determinations exist in the literature. The most recent one was used.
Luminosity class V was assumed.
References. (1) Morrell et al. (2001); Gies (2003), (2) Niemela et al. (2006), (3) Kraus et al. (2009), (4) Gies (2003), (5) Fernández Lajús & Niemela (2006), (6) Mayer et al. (2008), (7) Mayer et al. (2005), (8) Schweickhardt et al. (1999), (9) Williams et al. (2008), (10) Bonanos (2009).
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