Realistic ionizing fluxes for young stellar populations from 0.05 to 2 Z

• DOI: 10.1046/j.1365-8711.2002.06042.x
• Publication Date: 2003-03-12T14:27:20Z
• Authors: L. J. Smith; R. P. F. Norris; P. A. Crowther
• Keywords: Blanketing; Line (geometry); O-type star

We present a new grid of ionizing fluxes for O and Wolf-Rayet stars use with evolutionary synthesis codes single star H II region analyses. A total 230 expanding, non-LTE, line-blanketed model atmospheres have been calculated five metallicities (0.05, 0.2, 0.4, 1 2 solar) using the WM-basic code Pauldrach et al. (2001) CMFGEN Hillier & Miller (1998). The stellar wind parameters are scaled metallicity both W-R stars. incorporate models into Starburst99 (Leitherer 1999) compare outputs Schaerer Vacca (1998) Leitherer (1999). changes in output dramatic, particularly below 228 A. also find lower He I continuum Z > 0.4 solar ages < 7 Myr because increased line blanketing. test accuracy by constructing photoionization models. show that dwarf grid, 5876/H beta decreases between = twice similar manner to observations (e.g. Bresolin due effect therefore suggest lowering upper mass limit at high abundances is not required explain observations. For case an instantaneous burst, we plot softness parameter "eta prime" against abundance indicator R_23. coincident data (1999), during phase, unlike previous which over-predict hardness radiation.