All Figures

$\begin{figure} \par\resizebox{7cm}{!}{\includegraphics{7720fig1.eps}}\end{figure}$ Figure 1: 3D volumic density of the Local Bubble from the iso equivalent width contours for W = 20 mÅ and 50 mÅ (from Lallement et al. 2003).
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In the text

$\begin{figure} \par\mbox{\resizebox{8.5cm}{!}{\includegraphics{7720fig2a.eps}}\h... ...5cm} \resizebox{8.5cm}{!}{\includegraphics{7720fig2b.eps}} } \hfill \end{figure}$ Figure 2: Locations of the young local associations projected onto the Galactic ( left) and meridian ( right) planes. The size of the ellipses represents the projected dimension of the associations (more than 90% of the stars inside the plotted area). $\xi '$ is pointing to the Galactic anti-centre, $\eta '$ is the direction of Galactic rotation and $\zeta '$ is pointing to the north Galactic pole.
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In the text

$\begin{figure} \par\mbox{\resizebox{6cm}{!}{\includegraphics{7720fig3a.eps}}\hsp... ...\hspace*{4mm} \resizebox{6cm}{!}{\includegraphics{7720fig3c.eps}} } \end{figure}$ Figure 3: Distribution in the (U-V) [ left], (U-W) [ middle] and (V-W) [ right] planes of heliocentric velocity components for YLA member stars whose complete kinematic data are available. A kernel estimator was used to indicate the isocontours.
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In the text

$\begin{figure} \par\mbox{\resizebox{6cm}{!}{\includegraphics{7720fig4a.eps}}\hsp... ...\hspace*{4mm} \resizebox{6cm}{!}{\includegraphics{7720fig4f.eps}} } \end{figure}$ Figure 4: Distribution in the (U, V) [ top row] and (U, W) [ bottom row] planes of heliocentric velocity components for those stars with complete kinematic data belonging to the TW Hya association ( left column), the Tuc-Hor/GAYA association ( middle column) and the $\beta$ Pic-Cap moving group ( right column).
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics{7720fig5.eps}}\end{figure}$ Figure 5: Mean helicocentric velocity components of the YLA (indicating their 1 $\sigma$ error bars; standard deviation) and position in the (U, V) plane of those stars (with complete kinematic data) belonging to the TW Hya association.
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In the text

$\begin{figure} \par\resizebox{6.8cm}{!}{\includegraphics{7720fig6.ps}}\end{figure}$ Figure 6: Heliocentric coordinates ( $\xi ,\eta ,\zeta$ ) and ( $\xi ^\prime ,\eta ^\prime ,\zeta ^\prime$ ) (from Asiain 1998; see also Asiain et al. 1999b).
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In the text

$\begin{figure} \par\resizebox{15.7cm}{!}{\includegraphics{7720fig7.eps}}\end{figure}$ Figure 7: Positions and orbits in the Galactic plane ( $\xi ^\prime ,\eta ^\prime$ ) of YLA and the Sco-Cen complex going back in time to their individual ages. The orbits are also shown (small dots) as far back as -20 Myr. The grey areas show the expected positional errors at birth due to kinematic observational errors. The centre of the ( $\xi ^\prime ,\eta ^\prime$ ) coordinate system is comoving with the LSR.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{NEW-7720fig8.eps}}\end{figure}$ Figure 8: Present positions and orbits in the Galactic planes ( $\xi^\prime,~\zeta^\prime$ ) ( top) and ( $\eta^\prime,~\zeta^\prime$ ) ( bottom) for YLA and the Sco-Cen complex. The error areas (not shown) are of similar size as in Fig. 7. (See comments at Fig. 7.)
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics{7720fig9a.eps}}\par\vspace{0.5cm} \resizebox{8.8cm}{!}{\includegraphics{7720fig9b.eps}}\end{figure}$ Figure 9: Orbits in the Galactic plane ( $X^{\prime }$ - $Y^{\prime }$ ) integrated back in time to t = -30 Myr for YLA and the three associations of the Sco-Cen complex (below, only the orbits for Sco-Cen). The thick-dashed line shows the position of the minimum of the spiral potential (Fernández et al. 2001). The thin-dashed line is the position of the phase of the spiral structure $\psi = 10$ $^\circ$ .
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In the text

$\begin{figure} \par\resizebox{5cm}{!}{\includegraphics{7720fig10a.eps}}\par\resizebox{5cm}{!}{\includegraphics{7720fig10b.eps}}\end{figure}$ Figure 10: Variation of the velocity vector of a test particle when it hits the shock wave (solid line) in the vicinity of the centre of a spiral arm (shadow) and in a region inside ( top) and outside ( bottom) the corotation radius (in a reference frame in which the arms are fixed).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7720fig11.eps}}\end{figure}$ Figure 11: Distances between the centres of YLA and the centres of the Sco-Cen associations as a function of time, using the Sco-Cen kinematics in S03.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7720fig12.eps}}\end{figure}$ Figure 12: Error in distance ( left) and proper motion ( right) for stars with Hipparcos parallaxes belonging to YLA.
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In the text

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{7720fig13.eps}}\end{figure}$ Figure 13: Orbits of YLA and the Sco-Cen associations back in time to their individual ages (in a system comoving with the LSR; see Fig. 7) superimposed on the LB structure from Lallement et al. (2003, see Fig. 1). This structure has been rotated 90 $^\circ$ with respect to the orientation shown in Fig. 1.
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In the text

$\begin{figure} \par\resizebox{7cm}{!}{\includegraphics{7720fig1.eps}}\end{figure}$	Figure 1: 3D volumic density of the Local Bubble from the iso equivalent width contours for W = 20 mÅ and 50 mÅ (from Lallement et al. 2003).
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$\begin{figure} \par\mbox{\resizebox{6cm}{!}{\includegraphics{7720fig3a.eps}}\hsp... ...\hspace*{4mm} \resizebox{6cm}{!}{\includegraphics{7720fig3c.eps}} } \end{figure}$	Figure 3: Distribution in the (U-V) [ left], (U-W) [ middle] and (V-W) [ right] planes of heliocentric velocity components for YLA member stars whose complete kinematic data are available. A kernel estimator was used to indicate the isocontours.
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$\begin{figure} \par\mbox{\resizebox{6cm}{!}{\includegraphics{7720fig4a.eps}}\hsp... ...\hspace*{4mm} \resizebox{6cm}{!}{\includegraphics{7720fig4f.eps}} } \end{figure}$	Figure 4: Distribution in the (U, V) [ top row] and (U, W) [ bottom row] planes of heliocentric velocity components for those stars with complete kinematic data belonging to the TW Hya association ( left column), the Tuc-Hor/GAYA association ( middle column) and the $\beta$ Pic-Cap moving group ( right column).
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$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics{7720fig5.eps}}\end{figure}$	Figure 5: Mean helicocentric velocity components of the YLA (indicating their 1 $\sigma$ error bars; standard deviation) and position in the (U, V) plane of those stars (with complete kinematic data) belonging to the TW Hya association.
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$\begin{figure} \par\resizebox{6.8cm}{!}{\includegraphics{7720fig6.ps}}\end{figure}$	Figure 6: Heliocentric coordinates ( $\xi ,\eta ,\zeta$ ) and ( $\xi ^\prime ,\eta ^\prime ,\zeta ^\prime$ ) (from Asiain 1998; see also Asiain et al. 1999b).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{NEW-7720fig8.eps}}\end{figure}$	Figure 8: Present positions and orbits in the Galactic planes ( $\xi^\prime,~\zeta^\prime$ ) ( top) and ( $\eta^\prime,~\zeta^\prime$ ) ( bottom) for YLA and the Sco-Cen complex. The error areas (not shown) are of similar size as in Fig. 7. (See comments at Fig. 7.)
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$\begin{figure} \par\resizebox{5cm}{!}{\includegraphics{7720fig10a.eps}}\par\resizebox{5cm}{!}{\includegraphics{7720fig10b.eps}}\end{figure}$	Figure 10: Variation of the velocity vector of a test particle when it hits the shock wave (solid line) in the vicinity of the centre of a spiral arm (shadow) and in a region inside ( top) and outside ( bottom) the corotation radius (in a reference frame in which the arms are fixed).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7720fig11.eps}}\end{figure}$	Figure 11: Distances between the centres of YLA and the centres of the Sco-Cen associations as a function of time, using the Sco-Cen kinematics in S03.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7720fig12.eps}}\end{figure}$	Figure 12: Error in distance ( left) and proper motion ( right) for stars with Hipparcos parallaxes belonging to YLA.
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$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{7720fig13.eps}}\end{figure}$	Figure 13: Orbits of YLA and the Sco-Cen associations back in time to their individual ages (in a system comoving with the LSR; see Fig. 7) superimposed on the LB structure from Lallement et al. (2003, see Fig. 1). This structure has been rotated 90 $^\circ$ with respect to the orientation shown in Fig. 1.
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