of all our targets. We examined the three individual spectra to search for variability that might indicate binarity or problems with the spectra, but did not find any such evidence. Additional observations of this very hot star are needed to better determine its cluster membership and evolutionary status and we therefore omit it from all further discussion. Figs. \[ngc2808\_tg\] and \[ngc2808\_the\] show the results for all other stars.

[psfile=0505\_5.ps hscale=42 vscale=42 hoffset=-0 voffset=-60 angle=0]{}

[psfile=0505\_6.ps hscale=42 vscale=42 hoffset=-0 voffset=-60 angle=0]{}

In order to verify if the atmospheric parameters can reproduce the UIT observations, we calculated UIT fluxes from the observed $V$ magnitudes, using the model spectra from the best fits. The model spectra were first reddened by [$ {\rm E_{B-V}}$]{} = . Then mean fluxes through both the UIT 1520 Å and the $V$ filters were calculated to obtain the $m_{1520}-V$ colour, which was added to the observed $V$ magnitude from Walker ([@walk99]) to obtain the expected $m_{1520}$ magnitude. The results are compared to the UIT observations in Fig. \[uit\]. The agreement is good for the majority of the stars considering the low quality of the UIT data. The largest discrepancies are for the two helium-rich stars (W6849 and W14040), 