All Figures

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0221Fig1.eps}\end{figure}$ Figure 1: Normalized profiles vs. heliocentric velocity of the interstellar OVI detections for HD 20863, HD 74604 and HD 124367. The thick bold line is the best-fit model to the observed OVI data points. Also shown on the same velocity scale are the normalized profiles of the CII (1035 Å) and OI (1039 Å) interstellar lines.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0221Fig2.eps}\end{figure}$ Figure 2: Normalized profiles vs. heliocentric velocity of the interstellar OVI detections for HD 149630 and HD 149730. The thick bold line is the best-fit model to the observed OVI data points. Also shown on the same velocity scale are the normalized profiles of the CII (1035 Å) and OI (1039 Å) interstellar lines.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{0221Fig3.eps}\end{figure}$ Figure 3: Examples of sight-lines with only upper limits to OVI interstellar absorption. 2- $\sigma$ limits are HD 26670 (17.5 mÅ), HD 90972 (10.6 mÅ), HD 176638 (13.3 mÅ) and HD 188665 (7.6 mÅ). Note that the absorption feature at -20 km s^-1 seen towards HD 176638 is too narrow to be consistent with that expected from an OVI absorption line.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{0221Fig4.eps}\end{figure}$ Figure 4: Location of the 5 B-type stars with detectable OVI absorption with respect to the neutral gas density contours derived by Lallement et al. (2003) for the Local Cavity region. Each of the 5 maps lists the relevant projection (in galactic longitude and latitude) required to produce the gas volume density distribution (in black) to a distance of 200 pc in all directions. White volumes typically have values of N(NaI) < 5 $\times$ 10¹⁰ cm^-2, while black (dense) volumes have an average NaI density some 20-50 times higher.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0221Fig1.eps}\end{figure}$	Figure 1: Normalized profiles vs. heliocentric velocity of the interstellar OVI detections for HD 20863, HD 74604 and HD 124367. The thick bold line is the best-fit model to the observed OVI data points. Also shown on the same velocity scale are the normalized profiles of the CII (1035 Å) and OI (1039 Å) interstellar lines.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0221Fig2.eps}\end{figure}$	Figure 2: Normalized profiles vs. heliocentric velocity of the interstellar OVI detections for HD 149630 and HD 149730. The thick bold line is the best-fit model to the observed OVI data points. Also shown on the same velocity scale are the normalized profiles of the CII (1035 Å) and OI (1039 Å) interstellar lines.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{0221Fig3.eps}\end{figure}$	Figure 3: Examples of sight-lines with only upper limits to OVI interstellar absorption. 2- $\sigma$ limits are HD 26670 (17.5 mÅ), HD 90972 (10.6 mÅ), HD 176638 (13.3 mÅ) and HD 188665 (7.6 mÅ). Note that the absorption feature at -20 km s^-1 seen towards HD 176638 is too narrow to be consistent with that expected from an OVI absorption line.
Open with DEXTER