Table D.1.
Stellar parameters of the SSEM-outliers.
| Star | SpC | Teff | log(ℒ/ℒ⊙) | v sin i | YHe | ϵN | ξN | Status |
|---|---|---|---|---|---|---|---|---|
| BD +57 247 | O9.7 IV | 32.8 ± 1.6 | 3.5 ± 0.3 | 28 | 0.17 ± 0.09 | 8.45 ± 0.12 | 6 | MD |
| HD 326329 | O9.7 V | 31.9 ± 0.4 | 3.49 ± 0.05 | 87 | 0.14 ± 0.02 | 8.15 ± 0.12 | 4 | SB1 |
| HD 36512 | O9.7 V | 33.5 ± 0.7 | 3.37 ± 0.14 | 13 | 0.12 ± 0.03 | 7.84 ± 0.12 | 4 | LS |
| HD 38666 | O9.5 V | 33.1 ± 0.4 | 3.64 ± 0.05 | 111 | 0.14 ± 0.02 | 7.81 ± 0.15 | 10 | SB1, RW |
| HD 202214 | O9.5 IV | 32.1 ± 1.0 | 3.56 ± 0.16 | 26 | 0.13 ± 0.04 | 8.07 ± 0.11 | 6 | LS |
| HD 93027 | O9.5 IV | 33.4 ± 0.7 | 3.60 ± 0.13 | 46 | 0.12 ± 0.03 | 7.67 ± 0.12 | 8 | MD |
| HD 12323 | ON9.2 V | 34.4 ± 1.0 | 3.57 ± 0.19 | 121 | 0.18 ± 0.07 | 8.32 ± 0.15 | 8 | SB1, RW |
| HD 76341 | O9.2 IV | 32.3 ± 0.7 | 3.90 ± 0.09 | 51 | 0.15 ± 0.04 | 7.8 ± 0.12 | 17 | LS |
| HD 44597 | O9.2 V | 34.1 ± 1.1 | 3.6 ± 0.2 | 15 | 0.12 ± 0.04 | 7.95 ± 0.12 | 9 | LS |
| HD 14633 | ON8.5 V | 34.6 ± 0.8 | 3.8 ± 0.13 | 121 | 0.19 ± 0.07 | 8.18 ± 0.20 | 15 | SB1, RW |
| HD 48279 | O8.5 V zNstrvar? | 36.2 ± 0.7 | 3.74 ± 0.12 | 131 | 0.14 ± 0.02 | 8.24 ± 0.15 | 13 | LS |
| ALS 15196 | O8.5 V | 36.4 ± 0.9 | 3.54 ± 0.13 | 66 | 0.12 ± 0.03 | 7.81 ± 0.12 | 6 | MD |
| HD 90273 | ON7 V ((f)) | 38.3 ± 0.7 | 4.00 ± 0.08 | 55 | < 0.16 | 8.39 ± 0.12 | 20 | MD |
| HD 193595 | O7 V ((f)) | 37.6 ± 0.6 | 4.0 ± 0.1 | 46 | 0.15 ± 0.02 | 8.35 ± 0.12 | 19 | LS |
| HD 12993 | O6.5 V ((f)) Nstr | 39.3 ± 1.0 | 3.88 ± 0.15 | 84 | 0.16 ± 0.05 | 8.40 ± 0.15 | 21 | LS, RW |
| HD 167633 | O6.5 V ((f)) | 37.7 ± 0.9 | 4.0 ± 0.1 | 129 | 0.13 ± 0.04 | 8.28 ± 0.15 | 21 | SB1 |
| HD 63005 | O6.5 IV | 38.1 ± 1.4 | 3.95 ± 0.19 | 57 | 0.12 ± 0.04 | 7.97 ± 0.12 | 18 | MD |
| HD 256725 | O5 V((fc))z | 41.4 ± 1.3 | 3.91 ± 0.15 | 67 | 0.12 ± 0.03 | 7.95 ± 0.15 | 17 | LS |
| CPD -35 2105 | O9.2 III | 31.5 ± 0.6 | 3.91 ± 0.11 | 80 | 0.11 ± 0.03 | 7.56 ± 0.12 | 17 | MD |
| HD 152247 | O9.2 III | 31.2 ± 0.5 | 3.97 ± 0.11 | 82 | 0.18 ± 0.05 | 7.67 ± 0.15 | 19 | SB1 |
| HD 305523 | O9 II-III | 32.0 ± 0.4 | 4.0 ± 0.05 | 57 | 0.12 ± 0.03 | 7.67 ± 0.12 | 20 | MD |
| HD 105627 | O9 III | 33.2 ± 0.6 | 3.99 ± 0.09 | 141 | 0.14 ± 0.05 | 7.89 ± 0.15 | 21 | SB1, RW |
| HD 190864 | O6.5 III (f) | 37.5 ± 0.7 | 4.13 ± 0.08 | 66 | 0.14 ± 0.02 | 8.31 ± 0.20 | 23 | LS |
| HD 226868 | O9.7 Iab pvar | 28.7 ± 0.6 | 4.21 ± 0.08 | 95 | 0.18 ± 0.05 | 8.08 ± 0.12 | 26 | SB1 |
| HD 225146 | O9.7 Iab | 28.3 ± 0.9 | 4.08 ± 0.14 | 67 | 0.15 ± 0.06 | 7.87 ± 0.12 | 22 | LS, RW |
| HD 152405 | O9.7 II | 30.3 ± 0.7 | 4.00 ± 0.09 | 59 | 0.14 ± 0.04 | 8.07 ± 0.12 | 20 | SB1 |
| HD 75222 | O9.7 Iab | 29.5 ± 0.9 | 4.09 ± 0.11 | 86 | 0.14 ± 0.04 | 7.95 ± 0.11 | 23 | LS, RW |
| HD 167264 | O9.7 Iab | 28.4 ± 0.6 | 4.12 ± 0.11 | 71 | 0.12 ± 0.02 | 7.94 ± 0.11 | 23 | SB1 |
| HD 36486 | O9.5 II N wk | 30.1 ± 0.5 | 3.97 ± 0.06 | 100 | 0.11 ± 0.02 | 7.70 ± 0.12 | 19 | SB1 |
| BD -11 4586 | O8 Ib (f) | 32.4 ± 1.1 | 4.22 ± 0.15 | 74 | 0.13 ± 0.05 | 8.12 ± 0.12 | 26 | MD |
| HD 188001 | O7.5 Iab f | 32.2 ± 0.4 | 4.28 ± 0.05 | 69 | 0.23 ± 0.02 | 8.58 ± 0.28 | 28 | LS, RW |
| HD 332755 | O7.5 Ib-II | 35.2 ± 1.6 | 4.20 ± 0.22 | 2 | 0.15 ± 0.06 | 8.21 ± 0.13 | 26 | LS |
| HD 192639 | O7.5 Iab f | 34.1 ± 0.5 | 4.20 ± 0.05 | 82 | 0.14 ± 0.02 | 8.04 ± 0.16 | 26 | LS, RW |
| HD 117797 | O7.5 fp | 33.8 ± 0.5 | 4.18 ± 0.05 | 150 | 0.14 ± 0.02 | 8.22 ± 0.15 | 26 | SB1 |
| HD 69464 | O7 Ib (f) | 35.7 ± 1.0 | 4.22 ± 0.11 | 73 | 0.14 ± 0.03 | 8.05 ± 0.28 | 26 | LS |
| HD 163758 | O6.5 Ia fp | 34.9 ± 0.3 | 4.26 ± 0.06 | 76 | 0.20 ± 0.02 | 8.50 ± 0.13 | 27 | LS |
Notes. Stellar parameters for the 36 SSEM-outliers. Effective temperature (in kK), spectroscopic luminosity, He (as number ratio) and N abundances along with their computed uncertainties. In the case of v sin i (in km s−1), it has been considered a characteristic uncertainty of 10% of the central value. Microturbulence (ξN) in km s−1. The last column indicates the binarity status as likely single (LS), single line spectroscopic binary (SB1), or undetermined due to insufficient spectra (MD: more data needed), and whether they are claimed to be runaways (RW) either in Maíz Apellániz et al. (2018) or Carretero-Castrillo et al. (2023). Spectral type (SpC) from the Galactic O-star catalog (GOSC, Maíz Apellániz et al. 2013). Stars are sorted by luminosity class (LC) and then by increasing spectral type.
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