STIS Spectral Imagery of the OB Stars in NGC 604: The Most Luminous Stars

Abstract

We present results using 2-D spectral imagery and photometry obtained with the Hubble Space Telescope (HST) for the starburst H II region, NGC 604, in nearby galaxy M33. The spectral imagery was acquired with the Space Telescope Imaging Spectrograph (STIS) using the MAMA/G140L configuration, spanning 1170-1730 A. From a single 1720 sec STIS exposure, we extracted spectra for 49 stars and derived individual UV spectral types for 40 stars in the crowded 25"x2" stellar field. These stars represent a significant fraction of the young, luminous O and B stars. Three objects have pronounced He II 1640 emission, the signature of W-R or luminous Of stars. By combining UV fluxes with WFPC and WFPC2 visual photometry, we derive the extinction curve for NGC 604. We use this curve, the distance for M33, derived UV spectral types, and HST photometry, to determine positions of these stars in the upper H-R diagram. The revised O star effective temperature scale (Martins et al.) is essential in obtaining reliable positions in the log(L*)-log(T(eff)) plane. These stars are quite young with an age of ~3 Myr. The spectra and photometry indicate three exceedingly luminous objects. Their inferred locations in the H-R diagram indicate stellar masses > 120 solar masses. High spatial resolution HST imagery provides no evidence of multiple stars composing these objects. Still we cannot eliminate the possibility that they are unresolved multiple stars of lower mass, possibly W-R stars. Tests demonstrate that the ten most luminous stars predominantly determine the UV spectral features seen in the total light of NGC 604. We conclude that interpretation of spectral fitting of more distant starburst galaxies, where individual stars are not resolved, must be done with extreme care.