The ionizing radiation from massive stars and its impact on H ii regions: results from modern model atmospheres

Abstract

We present a detailed comparison of the ionizing spectral energy distributions (SEDs) predicted by four modern stellar atmosphere codes, TLUSTY, CMFGEN, wM-basic and FASTWIND. We consider three sets of stellar parameters representing a late O-type dwarf (09.5 V), a mid-O-type (07 V) dwarf and an early O-type dwarf (05.5 V). We explore two different possibilities for such a comparison, following what we called evolutionary and observational approaches: in the evolutionary approach, one compares the SEDs of stars defined by the same values of T eff and log g; in the observational approach, the models to be compared do not necessarily have the same T eff and log g, but produce similar H and He I-IIoptical lines. We find that there is a better agreement, in terms of Q(H°), the ratio Q(He°)/Q(H°) and the shape of the SEDs predicted by the four codes in the spectral range between 13 and 30 eV, when models are compared following the observational approach. However, even in this case, large differences are found at higher energies. We then discuss how the differences in the SEDs may affect the overall properties of surrounding nebulae in terms of temperature and ionization structure. We find that the effect over the nebular temperature is not larger than 300-350 K. Contrarily, the different SEDs produce significantly different nebular ionization structures. This will lead to important consequences on the establishment of the ionization correction factors that are used in the abundance determination of H ii regions, as well as in the characterization of the ionizing stellar population from nebular line ratios.