All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{3541f1.eps} \end{figure}$ Figure 1: The distribution of Galactic B stars included in the FUSE survey for stellar O VI with spectral type. Shaded regions in each histogram bar indicate the number of stars with luminosity classes I-III. The sample is strongly biased toward stars earlier than B3.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{3541f2.eps} \end{figure}$ Figure 2: The observed fluxes around the O VI doublet toward three early-B stars. Combs in the upper two panels mark the position of interstellar lines, most of which are due to H₂. We identified the Lyman $\beta$ of H I at 1026 Å and the C II, C II* absorption complex near 1037 Å that were particularly problematic "contaminants'' of the wind O VI absorption. Blue-shifted O VI absorption features are indicated for HD 219188 and HD 215733 (upper two panels). Similar features could not be identified for HD 92964 (lower panel) due to strong photospheric line blanketing.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm]{3541f3.eps} \end{figure}$ Figure 3: Synthetic spectra between -2300 and +600 km s^-1 of the rest wavelengths of the resonance doublets of O VI, N V, Si IV, and C IV (from top to bottom). The computed flux is plotted as a function of velocity with respect to the laboratory wavelength of the stronger (thick line) and weaker (thin line) member of each doublet. See Sect. 3 for a description of the model parameters. Since the computation did not include Auger ionization via X-rays, O VI and N V were not produced. The photospheric features in the vicinity of O VI are mostly due to Fe III.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3541f4.eps} \par\end{figure}$ Figure 4: Comparison of the observed wind profiles of HD 187459 for the resonance lines of O VI, N V, Si IV, and C IV (from top to bottom). The flux is plotted as a function of velocity with respect to the laboratory wavelength of the stronger (thick line) and weaker (thin line) member of each doublet. The velocity range where Lehner et al. (2003) observed time variability is indicated by vertical, dotted lines.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{3541f5.eps} \end{figure}$ Figure 5: Observed fluxes around the O VI doublet for three B0 V stars. HD 97471 and HD 207538 were observed by FUSE, while the spectrum of $\tau$ Sco was obtained by Copernicus. The positions of terrestrial airglow lines are indicated by the "Earth'' symbol in the FUSE spectra. The O VI wind features identified by Lamers & Rogerson (1978) are shown above the spectrum of $\tau$ Sco. Similar strong features are apparent in the spectrum of HD 97471, despite the strong interstellar C II, C II*, and H₂ lines around 1037 Å. However, no O VI wind features can be identified in the spectrum of HD 207538.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3541f6.eps} \end{figure}$ Figure 6: Comparison of the observed wind profiles of HD 219188 for the resonance lines of O VI, N V, Si IV, and C IV (from top to bottom). The flux is plotted as a function of velocity with respect to the laboratory wavelength of the stronger (thick line) and weaker (thin line) member of each doublet. The velocity range containing the O VI, Si IV, and C IV wind features is indicated by vertical, dotted lines. Note the serious contamination of the O VI doublet by interstellar lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3541f7.eps} \end{figure}$ Figure 7: Top panel: the measured optical depths of the blueshifted wind absorptions in the spectra of HD 219188, rebinned to 20 km s^-1 velocity bins. The thick and thin lines show O VI $\lambda$ 1031.93 and $\lambda$ 1037.62, respectively. Lower panel: the optical depth ratio of the O VI doublet in each velocity bins. The error bars reflect the estimated uncertainties introduced by the continuum placement around the wind features.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3541f8.eps} \end{figure}$ Figure 8: Same as Fig. 6 for HD 93840. Interstellar lines that contaminate the O VI absorption are indicated by tick marks.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3541f9.eps} \end{figure}$ Figure 9: Same as Fig. 8 for HD 191877.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3541f10.eps} \end{figure}$ Figure 10: Same as Fig. 8 for HD 215733.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3541f11.eps} \end{figure}$ Figure 11: Same as Fig. 6 for HD 92964. The dotted vertical lines indicate the velocity region where wind signatures are expected to appear.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3541f1.eps} \end{figure}$	Figure 1: The distribution of Galactic B stars included in the FUSE survey for stellar O VI with spectral type. Shaded regions in each histogram bar indicate the number of stars with luminosity classes I-III. The sample is strongly biased toward stars earlier than B3.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3541f8.eps} \end{figure}$	Figure 8: Same as Fig. 6 for HD 93840. Interstellar lines that contaminate the O VI absorption are indicated by tick marks.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3541f9.eps} \end{figure}$	Figure 9: Same as Fig. 8 for HD 191877.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3541f10.eps} \end{figure}$	Figure 10: Same as Fig. 8 for HD 215733.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3541f11.eps} \end{figure}$	Figure 11: Same as Fig. 6 for HD 92964. The dotted vertical lines indicate the velocity region where wind signatures are expected to appear.
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