Abstract
The properties of young, unresolved stellar populations are often derived from observations of optical nebular emission lines using evolutionary synthesis and photoionization codes (e.g. Stasinska et al., 2001). The reliability of this technique depends on the accuracy of the theoretical ionizing fluxes used to predict the nebular line strength ratios. With recent advances in computing and the development of large codes to calculate non-LTE line blanketed atmospheres, it is now feasible to compute a grid of realistic ionizing fluxes for O and Wolf-Rayet (WR) stars. We present such a grid for five metallicities (0.05, 0.2, 0.4, 1 and 2 Z⨀) for use with the Starburst99 (Leitherer et al., 1999) evolutionary synthesis code and analyses of single star H ii regions.
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