All Tables

Table 1: Basic parameters. Identifications: FLAMES targets ("NGC330'' and "NGC346'') from Evans et al. (2006), "MPG'' from Massey et al. (1989), "AzV'' from Azzopardi & Vigneau (1975,1982) and "Sk'' from Sanduleak (1968). Photometric data for the FLAMES targets is from Momany et al. (2001); for objects with a primary AzV identification these are from Massey (2002) and Massey et al. (2004). Spectral types of the FLAMES targets are from Evans et al. (2006). For convenience previously published spectral types are also given. Sources of these classifications are W77 (Walborn 1977); NMC (Niemela et al. 1986); G87 (Garmany et al. 1987); MPG (Massey et al. 1989); W00 (Walborn et al. 2000); EH04 (Evans et al. 2004b). Spectral types for the field O-type stars were taken from the catalogues of Garmany et al. (1987) and Walborn et al. (2002). Wind velocities given without brackets are from Prinja & Crowther (1998); Evans et al. (2004a); Haser et al. (1998); Garmany & Fitzpatrick (1988); Massey et al. (2004); Crowther et al. (2002); Bouret et al. (2003); Evans et al. (2004c). Values between brackets are calculated from the escape velocity at the stellar surface.
Table 2: Results of the formal tests. Input parameters of the formal test models are given in the "In'' column and parameters obtained with the automated fitting method by fitting synthetic data created from these models are listed in the "Out'' column. The results were obtained by evolving a population of 72 FASTWIND models over a course of 200 generations.
Table 3: Fundamental parameters determined using GA optimised spectral fits, with $T_{\rm eff}$ in kK, $\log{{g}}$ and $\log{{g}}_{\rm c}$ in cm s^-2, $R_{\star }$ in $R_{\odot }$ , $L_{\star }$ in $L_{\odot }$ , $v_{\rm turb}$ and $v_{\rm r}\sin i$ in km s^-1, $\dot{M}$ in $M_{\odot}~{\rm yr}^{-1}$ , $M_{\rm s}$ and $M_{\rm ev}$ in $M_{\odot }$ and Q₀ in number of photons per second. Results were obtained using a population of 72 FASTWIND models evolved over a minimum of 150 generations. Gravities corrected for centrifugal acceleration ( $\log{{g}}_{\rm c}$ ) were used to calculate the spectroscopic masses ( $M_{\rm s}$ ). Evolutionary masses ( $M_{\rm ev}$ ) were derived from the tracks of Charbonnel et al. (1993). Note that "NGC'' is omitted from the identifications of the FLAMES targets.
Table 4: Optimum width based error estimates for the seven fit parameters. The ND entries correspond to error in $v_{\rm turb}$ that reach up to the maximum allowed value of $v_{\rm turb}$ and, therefore, are formally not defined. See text for details on the calculation of the uncertainties in the derived parameters. Units: $T_{\rm eff}$ in kK, $\log{{g}}$ and $\log{{g}}_{\rm c}$ in cm s^-2, $R_{\star }$ in $R_{\odot }$ , $L_{\star }$ in $L_{\odot }$ , $v_{\rm turb}$ and $v_{\rm r}\sin i$ in km s^-1, $\dot{M}$ in $M_{\odot}~{\rm yr}^{-1}$ , $M_{\rm s}$ and $M_{\rm ev}$ in $M_{\odot }$ and Q₀ in number of photons per second. Note that "NGC'' is omitted from the identifications of the FLAMES targets.