THE POPULATION OF MASSIVE STARS IN R136 FROM FAINT OBJECT CAMERA ULTRAVIOLET OBSERVATIONS

New ultraviolet (lambda congruent-to 1300 angstrom, lambda congruent-t o 3400 angstrom), HST Faint Object Camera observations have been used to derive the UV color-magnitude diagram (CMD) of R136. The main scien tific goal is the study of the upper end of the stellar mass function at ultraviolet wavelengths where the color degeneracy encountered in v isual CMDs is less severe. The CMD has been compared to a set of theor etical isochrones, which have been computed using the latest generatio n of evolutionary models and model atmospheres for early-type stars. W olf-Rayet stars are included, and their emergent fluxes are calculated with the theoretical continuum energy distributions of Schmutz et al. Comparison of the theoretical and observed CMD suggests that there ar e no stars brighter than M130 congruent-to -11. We use the observed ma in sequence turnoff and the known spectroscopic properties of the stel lar population to derive constraints on the most probable age of R136. The presence of WNL stars and the lack of red supergiants suggests a most likely age of 3 +/- 1 Myr. A theoretical isochrone of 3 +/- 1 Myr is consistent with the observed stellar content of R136 if the most m assive stars have initial masses around congruent-to 50 M..