All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig1.eps}} \end{figure}$ Figure 1: Resulting de-reddened spectrum of HD 45166 decomposed into the qWR star (full black line) and the B7 V companion (dashed red line). As anticipated in Paper I, the qWR star is dominant in the blue part of the spectrum, while the B7 V companion dominates for $\lambda>5000~ {\AA}$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig2.eps}} \end{figure}$ Figure 2: Normalized spectrum of the qWR star in HD 45166 (black line) compared with spherical CMFGEN models with $\ensuremath{\mathit{T}_{\rm eff}} =50~000~{\rm K}$ (purple dash-double-dotted line), $\ensuremath{\mathit{T}_{\rm eff}} =46~000~{\rm K}$ (blue dot-double-dashed line), $\ensuremath{\mathit{T}_{\rm eff}} =43~000~{\rm K}$ (green dot-dashed line), and $\ensuremath{\mathit{T}_{\rm eff}} =35~000~{\rm K}$ (red dashed line). A model with the same parameters proposed by Willis & Burnley (2006) ( $\ensuremath{\mathit{T}_{\rm eff}} =35~000~{\rm K}$ , $\ensuremath{v_{\infty}} =1200~\ensuremath{{\rm km~s^{-1}}}$ ) produces fits similar to the original $\ensuremath{\mathit{T}_{\rm eff}} =35~000~{\rm K}$ model, and does not fit our optical data as well. For clarity, such a model is compared only to He II $\lambda$ 4686 (brown thick line).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig3.eps}} \end{figure}$ Figure 3: a) Comparison between the continuum flux predicted by CMFGEN models for the qWR star in the range $32~000 {\rm K}< \ensuremath{\mathit{T}_{\rm eff}} < 50~000 ~ {\rm K}$ . All models were scaled to the observed de-reddened flux of the qWR star at 5500 Å ( $3.09 \times 10^{-13}$ erg s^-1 cm^-2 Å^-1, see Fig. 1). Since the continuum slope is very weakly sensitive to the value of $\ensuremath{\mathit{T}_{\rm eff}}$ (see text for discussion), the models are basically superimposed on each other. b) Ratio between the continuum flux predicted by a CMFGEN model with a given $\ensuremath{\mathit{T}_{\rm eff}}$ and the continuum flux of the $\ensuremath{\mathit{T}_{\rm eff}} = 50~ 000$ K CMFGEN model. c) Comparison between the total de-reddened observed flux of HD 45166 (black) and the flux predicted by the radiative-transfer model (red dashed line). The model shown here is composed of the sum of the continuum of the B7 V template from the companion (shown in Fig. 1) and the continuum of the best CMFGEN model for the qWR star.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig4.eps}} \end{figure}$ Figure 4: Velocity law (panel a)), density structure b), electron density c), and Rosseland optical depth d) of HD 45166 as a function of distance.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig5.eps}} \end{figure}$ Figure 5: Ionization fractions of HD 45166 as a function of distance, derived from the spherical CMFGEN models of the most abundant ions in the wind of the qWR star. The ionization fractions are normalized by the total number of ions.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig6.eps}} \end{figure}$ Figure 6: Comparison between the line profiles predicted by the best CMFGEN spherical model with the observations of HD 45166, in the spectral region 3850-5950 Å. The strongest spectral lines used in the analysis are identified.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig7.eps}} \end{figure}$ Figure 7: Same as Fig. 6, but for the spectral region of 6000-8800 Å.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig8.eps}} \end{figure}$ Figure 8: Line formation region for the strongest lines of HD 45166 used in the spectroscopic analysis. For each panel the quantity $\xi$ is displayed, which is related to the EW of the line (following Hillier 1989) as ${\it EW}=\int_{\ensuremath{\mathit{R}_{\star}} }^{\infty}\xi(r){\rm d}(\log~r)$ .
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[angle=90]{9511fi9a.ps} \... ...cs[angle=90]{9511fi9h.ps} \includegraphics[angle=90]{9511fi9i.ps} } \end{figure}$ Figure 9: Density contrast of the HD 45166 models with latitude-dependent density distributions (normalized to the density distribution of the spherical model), as a function of latitude. Each model is labeled as in Table 5; model 9 has the same density distribution as model 4, and is not shown. The equator of the star is at [x,0], while the pole is located at [0,y]. The colorbar in the right has a linear color scale, which we adopted the same for all models, to highlight the different density variations as a function of latitude. The maximum value in the colorbar is 1.8, which corresponds to the maximum value found in model 5.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511f10.eps}} \end{figure}$ Figure 10: Comparison between the line profiles computed with the 2D code of Busche & Hillier (2005) (blue line) with the observations of HD 45166 around He I $\lambda$ 5876 (black line). For each panel the models are labelled as in Table 5, followed by the density contrast equator:pole, and the parameter b. The best spherical-symmetric CMFGEN model (red dashed line) is repeated in each panel for comparison (see text for further details). The weak dip in the observed He I $\lambda$ 5876 line profile is likely due to incomplete subtraction of the secondary star spectrum.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{9511f11a.eps}}... ...}}\par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{9511f11c.eps}} \end{figure}$ Figure 11: Average intensity spectrum and TVS of HD 45166 for He II $\lambda$ 4686 ( upper panel), C IV $\lambda \lambda$ 5801-5812 ( middle), and He I $\lambda$ 5876 ( bottom). The TVS statistical threshold significance of p=1%, 5%, and 30% are represented by the dotted, dashed, and dot-dashed horizontal lines, respectively. The vertical dotted lines mark the position of the zero velocity for the relevant line presented in each panel. See text for details.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511f13.eps}} \end{figure}$ Figure 12: Upper panel: radial density profile of the C³⁺ and C⁴⁺ ions along the wind of HD 45166. Lower panel: line formation region of C IV $\lambda \lambda$ 5801. The quantity $\xi$ is related to the EW of the line (following Hillier 1989) as ${\it EW}=\int_{\ensuremath{\mathit{R}_{\star}} }^{\infty}\xi(r){\rm d}(\log~r)$ .
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics{9511f14.eps}} \end{figure}$ Figure A.1: Intensity of the He II lines of the Pickering series as a function of the upper quantum number, normalized such that I(He II $\lambda$ 5411) = 1. The open squares represent the observed values of HD 45166, the filled circles correspond to the theoretical prediction for an optically-thin gas, using tabulated values from Oliveira & Steiner (2004).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig1.eps}} \end{figure}$	Figure 1: Resulting de-reddened spectrum of HD 45166 decomposed into the qWR star (full black line) and the B7 V companion (dashed red line). As anticipated in Paper I, the qWR star is dominant in the blue part of the spectrum, while the B7 V companion dominates for $\lambda>5000~ {\AA}$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig4.eps}} \end{figure}$	Figure 4: Velocity law (panel a)), density structure b), electron density c), and Rosseland optical depth d) of HD 45166 as a function of distance.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig5.eps}} \end{figure}$	Figure 5: Ionization fractions of HD 45166 as a function of distance, derived from the spherical CMFGEN models of the most abundant ions in the wind of the qWR star. The ionization fractions are normalized by the total number of ions.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig6.eps}} \end{figure}$	Figure 6: Comparison between the line profiles predicted by the best CMFGEN spherical model with the observations of HD 45166, in the spectral region 3850-5950 Å. The strongest spectral lines used in the analysis are identified.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig7.eps}} \end{figure}$	Figure 7: Same as Fig. 6, but for the spectral region of 6000-8800 Å.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511fig8.eps}} \end{figure}$	Figure 8: Line formation region for the strongest lines of HD 45166 used in the spectroscopic analysis. For each panel the quantity $\xi$ is displayed, which is related to the EW of the line (following Hillier 1989) as ${\it EW}=\int_{\ensuremath{\mathit{R}_{\star}} }^{\infty}\xi(r){\rm d}(\log~r)$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9511f13.eps}} \end{figure}$	Figure 12: Upper panel: radial density profile of the C³⁺ and C⁴⁺ ions along the wind of HD 45166. Lower panel: line formation region of C IV $\lambda \lambda$ 5801. The quantity $\xi$ is related to the EW of the line (following Hillier 1989) as ${\it EW}=\int_{\ensuremath{\mathit{R}_{\star}} }^{\infty}\xi(r){\rm d}(\log~r)$ .
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics{9511f14.eps}} \end{figure}$	Figure A.1: Intensity of the He II lines of the Pickering series as a function of the upper quantum number, normalized such that I(He II $\lambda$ 5411) = 1. The open squares represent the observed values of HD 45166, the filled circles correspond to the theoretical prediction for an optically-thin gas, using tabulated values from Oliveira & Steiner (2004).
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