Notes. Photometry follows Bonanos et al. (2009). The primary source for the B, V photometry is Selman et al. (1999); their observations were obtained over only ~10 min, so the (B−V) colours are insensitive to orbital variability. JHK results are from IRSF (the InfraRed Survey Facility; Kato et al. 2007), and the mid-IR photometry from Spitzer “SAGE” Legacy Science Program (Meixner et al. 2006). Measurement uncertainties are ≲005, excepting the [5.8] magnitude for VFTS 450 (±015), but both stars are variable with amplitudes of ~02 (Fig. 5). The last two columns are average results from our OGLE photometry (Sect. 2.2.1).