All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{8373fig1.eps}\end{figure}$ Figure 1: Molecular lines. From top to bottom: ¹²CO J=2-1 emission line (Sect. 3.3) in the millimeter range with the SEST, two examples of the CO ultraviolet absorption bands (A-X (2, 0) and A-X (0, 0)) observed with STIS, and the CH and CH⁺ visible absorption lines (Sect. 3.1). Histogram-style curves represent the observations normalized to the continuum, solid lines are the best fits, and dashed lines, the profiles before convolution with the instrument line spread function, i.e. the intrinsic interstellar profile. The letters A, B and C indicate velocity components that will be introduced in the spectral analysis.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8373fig2.ps}\end{figure}$ Figure 2: Sample lines from neutral species. Histogram-style curves represent the observations (in ${\rm erg~cm^{-2}~s^{-1}}~\textrm{Å}^{-1}$ ), solid lines are the best fits, and dashed lines, the profiles before convolution with the instrument line spread function, i.e. the intrinsic interstellar profile. An asymmetry is evident on most profiles which are therefore best fitted with two components, called A and B.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{8373fig3.ps}\end{figure}$ Figure 3: Sample of lines from ionized species and neutral species with ionization potential close to that of H I. Same line style as Fig. 2. Most fits have been performed with the same line-of-sight model, made of 4 components with same velocity and same temperature for all species. There are only three exceptions: (i) An additional component of high-temperature gas is included at the velocity of component 4 to fit the extended blue wing of the strong Mg II and C II* lines. (ii) In the O I** profile an additional component is considered, blueward of component 4. (iii) The S II profiles include an extra absorption on the red side of component 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8373fig4.ps}\end{figure}$ Figure 4: Highly-ionized species observed with STIS. As an indication, consistent absorption line profiles for gas at a temperature of 900 000 K and at the velocity of component 4 are superimposed.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8373fig5.ps}\end{figure}$ Figure 5: H I emission line in the direction of HD 102065 derived from the IAR Southern Sky survey. The thick line represents the difference with respect to a reference position outside of the Blue cloud.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8373fig6.ps}\end{figure}$ Figure 6: IRAS 12 $\mu$ m image (IRIS processing, Miville-Deschênes & Lagache 2005) with contours of H I emission at $V_{\rm LSR} = -1~{\rm ~ km ~ {s}^{-1}}$ (white dashed) and $5~{\rm ~ km ~ {s}^{-1}}$ (black solid) taken from the IAR survey (30' resolution and $1.3~{\rm ~ km ~ {s}^{-1}}$ width velocity channels, Bajaja et al. 2005). The position of HD 102065 and the T Tauri star T Cha are marked. Contours are labeled with the brightness temperature. The 30 K contour is thicker. The cloud tail is roughly at a constant Galactic longitude. The Galactic coordinates of HD 102065 are $l = 300.0^\circ$ and $b = -18.0^\circ$ . The electronic version is in color.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8373fig7.ps}\end{figure}$ Figure 7: H I position-velocity diagram across the Blue Cloud at the Galactic latitude of HD 102065 ( $b=-18^\circ$ ). This figure shows that the two velocity components at respectively 0.1 and 4.2 ${\rm ~ km ~ {s}^{-1}}$ each extends on one side of the star position ( $l=300^\circ$ ) where they overlap. The emission at the OFF position (see text) has been subtracted to highlight the gas associated with the cloud.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm]{8373fig8.ps}\end{figure}$ Figure 8: Example of a $\Delta \chi ^{2}$ curve, here for C I in component A. Each point corresponds to a fit performed with the C I column density in component A fixed to the value given in abscissa. $\Delta \chi ^{2}$ is rescaled by dividing it by the 95 %-confidence level for this fit (rescaled $\Delta \chi ^{2}=1.41$ ). 3 $\sigma$ -uncertainty is given by $\Delta \chi ^{2}=3^{2}\times 1.41=12.7$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{8373fig9.ps}\end{figure}$ Figure 9: H I emission at negative velocities $-50<V_{\rm LSR}<-20~{\rm ~ km ~ {s}^{-1}}$ in direction of the Sco-Cen association. H I observations from Bajaja et al. (2005) and Kalberla et al. (2005). The position of HD 102065 and the US (Upper-Scorpius), UCL (Upper Centaurus Lupus) and LCC (Lower Centaurus Crux) sub-groups of the OB association are marked. The black area indicates the region where the selected range of negative velocities overlaps with the Galactic rotational velocities of distant gas. The electronic version is in color.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8373fig4.ps}\end{figure}$	Figure 4: Highly-ionized species observed with STIS. As an indication, consistent absorption line profiles for gas at a temperature of 900 000 K and at the velocity of component 4 are superimposed.
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$\begin{figure} \par\includegraphics[width=8.8cm]{8373fig5.ps}\end{figure}$	Figure 5: H I emission line in the direction of HD 102065 derived from the IAR Southern Sky survey. The thick line represents the difference with respect to a reference position outside of the Blue cloud.
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