Fundamental parameters of Galactic luminous OB stars. IV. The upper HR diagram

We present observations and analyses of seven Galactic O stars of type O6 and earlier. The analyses are carried out using NLTE plane-parallel, hydrostatic models as well as NLTE spherical models with mass-loss. With detailed calcula- tions for the former and simulations for the latter, it is shown that the flux blocking due to UV metal lines is important for these objects, in agreement with previous studies, and the way the mechanism operates is explained. We find that the plane- parallel, hydrostatic unblanketed model atmospheres have in- creasing difficulties in fitting the early-type spectra of massive stars, and for 50 000 K and above a fit seems to be impossible. The gravities derived are relatively low even for the luminosity class V stars. These objects also show the mass discrepancy found in earlier studies, indicating that sphericity and mass-loss are important, even at their higher gravities. We then perform an analysis using spherical models with mass-loss. It is found that gravities should be increased by 0.1-0.25 dex, reducing, but not solving, the mass discrepancy. We show that spectroscopic masses are in better agreement with the theory of radiatively driven winds than evolutionary masses are. A helium abundance larger than solar is also obtained for most objects. Some additional effects (partly related to present approxi- mations) that have an influence in our analyses are studied. It is found that Heii4200 is less sensitive to details of the model calculations than Heii4541 and thus it is preferred for tempe- rature determinations, with the consequence of lower effective temperatures. It is shown that the fits to He ii4686 are im- proved when the upward rates of the Heii resonance lines are reduced (with respect to the conventional treatment adequate for lines formed in expanding atmospheres), either by setting them in detailed balance or by artificially adding extra opacity sources that simulate line blocking. The Heii blend with H is also affected. Some stars of our sample have such high mass-loss rates that the derivation of gravities from the wings of Balmer lines, in