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Table 1

Sample stars and photometry.

Source ST U B V J H K AV MV

NGC 2244
HD 46223 O4V((f)) 6.712 7.484 7.266 6.742 6.684 6.693 1.54  −5.22
HD 46150 O5V((f))z 6.043 6.875 6.745 6.446 6.451 6.453 1.27  −5.48
HD 46485 O7Vn 7.876 8.563 8.243 7.565 7.492 7.463 1.86  −4.57
HD 46056 O8Vn 7.705 8.445 8.245 7.837 7.816 7.837 1.49  −4.20
HD 46149-1 O8V 6.982 7.774 7.602 7.245 7.232 7.268 1.40  −4.13
HD 46149-2 O8.5–9V 1.40  −3.84
HD 46202 O9.5V 7.623 8.360 8.183 7.784 7.760 7.737 1.42  −4.19

Mon OB2
HD 46573 O7V((f))z 7.613 8.273 7.933 7.197 7.148 7.145 1.92  −4.94
HD 48279 ON8.5V 7.254 8.047 7.910 7.650 7.681 7.710 1.29  −4.33
HD 46966 O8.5IV 5.910 6.827 6.877 6.919 6.951 7.035 0.71  −4.78
HD 48099-1 O5.5V((f)) 5.387 6.323 6.366 6.445 6.490 6.512 0.73  −5.39
HD 48099-2 O9V 0.73  −3.89

Notes. Spectral types are from Sota et al. (2011) and Mahy et al. (2009). Magnitudes are from Maíz-Apellániz et al. (2004). The extinction AV is 3.1 × E(B − V). The absolute magnitude assumes a distance of 1.55 kpc. For binary stars, we give the observed magnitudes of the system on the row of the primary star. For binary systems, the absolute V magnitudes of each component are computed assuming the V-band flux ratio typical for stars of the same spectral type (see Sect. 4).

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