All Tables

Table 1: Final atomic model used in the analysis of HD 45166. A single-level ion of one higher ionization stage is included for every species (e.g. C VI for carbon) and omitted below for brevity.
Table 2: Fundamental parameters derived for the qWR star
in HD 45166.
Table 3: Surface chemical abundances of HD 45166.
Table 4: Abundance ratios (in number) of HD 45166 compared todifferent object classes.
Table 5: Summary of the parameters used to compute the spectrum in 2D geometry using the Busche & Hillier (2005) code. Note that the density contrast between equator and pole is given by 1+a for oblate models, and 1/(1+a) for prolate models.
Table 6: $\sigma /I$ for the strongest lines present in HD 45166. Both $\sigma$ and I were measured at the centroid of the lines.
Table 7: Average FHWM and radial velocity of the spectral lines for the most abundant ions present in HD 45166.
Table B.1: Equivalent width of the CNO emission lines in HD 45166 obtained from the observations. References: Willis & Stickland (1983) for ultraviolet lines (1200-3300 Å), and this work for optical lines (3700-9000 Å). Key: y=line is present; $y?=\rm doubtful$ identification due to low S/N; ?=doubtful identification due to presence of a telluric line; bl=blended with other lines; n=line is definitely not present.