Table 1
Adopted spectral type-temperature calibration.
| Spect. type | Dwarf | Giant | Supergiant | |||
|---|---|---|---|---|---|---|
| Teff (kK) | BCK (mag) | Teff (kK) | BCK (mag) | Teff (kK) | BCK (mag) | |
| O4 | 46.0 | −4.99 | 41.7 | −4.87 | 40.2 | −4.78 |
| O5 | 41.3 | −4.84 | 39.9 | −4.63 | 38.5 | −4.44 |
| O6 | 39.5 | −4.72 | 38.0 | −4.50 | 36.5 | −4.27 |
| O7 | 38.7 | −4.58 | 36.5 | −4.37 | 34.5 | −4.15 |
| O8 | 36.4 | −4.30 | 35.0 | −4.15 | 32.5 | −4.01 |
| O9 | 33.2 | −3.97 | 31.7 | −3.94 | 30.0 | −3.63 |
| O9.5 | 32.1 | −3.82 | 30.5 | −3.75 | 29.0 | −3.48 |
| B0 | 31.0 | −3.74 | 29.5 | −3.61 | 27.2 | −3.29 |
| B0.5 | 29.6 | −3.57 | 28.5 | −3.47 | 24.3 | −2.89 |
| B1 | 27.3 | −3.28 | 23.9 | −2.93 | 22.3 | −2.62 |
| B1.5 | 26.1 | −3.17 | 22.5 | −2.70 | 20.6 | −2.38 |
| B2 | 24.9 | −3.07 | 21.2 | −2.53 | 18.9 | −2.18 |
| B2.5 | 23.9 | −2.95 | 19.8 | −2.34 | 17.2 | −1.78 |
| B3 | 21.5 | −2.59 | 18.4 | −2.05 | 15.5 | −1.45 |
| B5 | ... | 16.7 | −1.65 | 13.8 | −1.04 | |
| B8 | ... | ... | 12.0 | −0.62 | ||
| B9 | ... | ... | 10.5 | −0.27 | ||
| A0 | ... | ... | 9.5 | +0.02 | ||
| A2 | ... | ... | 8.5 | +0.30 | ||
| A5 | ... | ... | 7.7 | +0.35 | ||
| A7 | ... | ... | 7.2 | +0.49 | ||
| F0 | ... | ... | 6.7 | +0.62 | ||
| F2 | ... | ... | 6.4 | +0.72 | ||
| F5 | ... | ... | 5.9 | +0.85 | ||
Notes. Based on SMC results from Bouret et al. (2013) and Bouret et al. (2021) for O stars, Dufton et al. (2019) for B0–5 stars, and Evans & Howarth (2003) for cooler supergiants. Ks-band bolometric corrections combine V-band bolometric corrections from Bouret et al. (2013), Bouret et al. (2021), Lanz & Hubeny (2007), Kudritzki et al. (2008) and Cox (2000), and V − K colours from Martins & Plez (2006), Koornneef (1983) and Cox (2000).
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