5.86$\pm$0.12                         $-$0.88$\pm$0.07
  D4985     2.50               38000$\pm$ 700        5.79$\pm$0.17                         $-$0.80$\pm$0.14
  D10123    2.40               35200$\pm$ 690        5.73$\pm$0.14                         $-$0.84$\pm$0.09
  D10763    2.85               36000$\pm$1700        4.82$\pm$0.15                         $+$0.50$\pm$0.03
  D12564    1.75               36800$\pm$ 960        5.73$\pm$0.17                         $-$0.50$\pm$0.05
  D14695    2.16               38800$\pm$ 230        5.31$\pm$0.12                         $-$0.16$\pm$0.05
  D15116    1.50               40000$\pm$1700        6.08$\pm$0.38                         $-$0.51$\pm$0.17
  D16003    1.45               36600$\pm$ 550        5.89$\pm$0.12                         $-$1.00$\pm$0.09
  --------- ---------- ---------------------- -------------------- ----------------------------------------

  : Atmospheric parameters of the stars in $\omega$ Cen \[tab-paro\]

We fitted the hot stars ([$ {\rm T_{eff}}$]{}$\gtrsim$33,000 K) with H-He non-LTE model atmospheres to derive effective temperatures, surface gravities, and helium abundances. The helium-rich non-LTE model atmospheres were calculated with a modified version of the accelerated lambda iteration code of Werner & Dreizler ([@wedr99]). The model atoms for hydrogen and helium as well as the handling of the line broadening for the spectrum synthesis are similar to those of Werner ([@wern96]). The calculation of the helium-poor non-LTE model atmospheres is described in Napiwotzki ([@napi97]). For the cooler stars we used ATLAS9 model atmospheres for solar metallicity (Kurucz [@kuru93]) to account for effects of radiative levitation (see Moehler et al. [@mosw00] for details), from which we calculated spectra with Lemke’s version[^2] of the LINFOR program (developed originally by Holweger, Steffen, and Steenbock at Kiel University). To establish the best fit, we used the 