The temperature of VFTS 145 (O8fp) is based on the lines He i λ4471, N iii λ4634/4640, and N iv λ4058. The He ii absorption lines are narrower than the models which suggests a lower log g value than 4.0. The spectrum shows weak RV variations and LPVs. The star is multiple in the HST observations and therefore the luminosity might be overestimated. N is enriched. He ii λ4686 is quite strong relative to H_α. The only way to increase the He ii emission line strength without increasing Ṁ is by increasing the He surface abundance.