All Figures

$\begin{figure} \par\resizebox{15cm}{!}{\includegraphics[bb=24 250 550 780,clip]{5602fig1.eps}}\end{figure}$ Figure 1: Celestial polar projection of the stars observed in SACY. Stars classified as young according to their Li I equivalent width (see Sect. 4.2) are plotted as filled circles. More evolved stars are indicated as open circles. The transverse curve represents the Galactic plane.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{5602fg2a.eps}}\vspace*{3.5mm} \par\resizebox{8.8cm}{!}{\includegraphics{5602fg2b.eps}}\end{figure}$ Figure 2: Comparison of our derived radial velocities and $V\sin~(i)$ with those derived by Nordström et al. (2004). Top: Radial velocities obtained with FEROS are shown as filled circles whereas those obtained with the coudé are seen as filled squares. The continuous line is the one-to-one relation and the two dashed-dotted lines delimit a $\pm$ 5 km s^-1 region around the continuous line. Bottom: Again, the one-to-one relation is shown as a continuous line whereas the dashed-dotted lines mark the $V\sin~(i)$ errors of 2 km s^-1 for $V\sin~i\le20$ km s^-1 and 10% of the observed $V\sin~(i)$ for $V\sin~i>20$ km s^-1. Multiple stars are shown as encircled symbols.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{5602fig3.eps}\end{figure}$ Figure 3: Our spectral types as a function of the $(V-I)_{\rm C}$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[bb=50 269 530 769,clip]{5602fig4.eps}}\end{figure}$ Figure 4: Distribution of Li equivalent width as a function of the $(V-I)_{\rm C}$ . The lines represents the upper and lower limits for Pleiades members.
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In the text

$\begin{figure} \par\mbox{\parbox{8.5cm} {\raggedleft\resizebox{8.5cm}{!}{\includ... ...}{ \includegraphics[bb=108 222 474 574,clip]{5602fig5.eps} }} } \par\end{figure}$ Figure 5: The convergence method. Left: As a first step, a concentration around a point in the UVW-space is found. The position of the stars defining this concentration at the HR diagram and their Li equivalent width give a first estimation for the age of the association. Right: Starting with an age and an initial ( UVW)₀ determined in step 1, we look for the stars in the young sample which fit the association.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{5602fig6.eps}}\end{figure}$ Figure 6: HR diagram from the proposed members of the $\beta$ Pic Association. The isochrones over-plotted are those from Siess et al. (2000). The dotted and dashed lines correspond to the isochrones for 5 Myr and 50 Myr, respectively. The isochrone for 10 Myr is shown as thick solid line whereas the observational isochrone is represented as a thick dotted-dashed line.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{5602fig7.eps}}\end{figure}$ Figure 7: Correlation between the X-position and U-component of space velocity vector showing an expansion of the members of the $\beta$ Pic Association. Objects whose parallaxes are from Hipparcos Catalogue are overplotted with squares.
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In the text

$\begin{figure} \par\begin{tabular}{c} \resizebox{17.8cm}{!}{\includegraphics{560... ...aphics{5602fg8e.eps}\includegraphics{5602fg8f.eps}}\\ \end{tabular}\end{figure}$ Figure 8: Combinations of the sub-spaces of the UVWXYZ-space showing a well defined clustering in both kinematical and spatial coordinates.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{5602fig9.eps}}\end{figure}$ Figure 9: Distribution of Li equivalent width as a function of the $(V-I)_{\rm C}$ for the proposed members of the $\beta$ Pic Association shown in Table 6. The hatched area shows the Li equivalent width range observed for the Pleiades members.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{5602fg10.eps}}\end{figure}$ Figure 10: Distribution of Li abundances as a function of the effective temperature for the proposed members of the $\beta$ Pic Association (Table 7). The hatched area shows the Li abundances with range observed for the Pleiades members.
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In the text

$\begin{figure} \par\resizebox{15cm}{!}{\includegraphics[bb=24 250 550 780,clip]{5602fig1.eps}}\end{figure}$	Figure 1: Celestial polar projection of the stars observed in SACY. Stars classified as young according to their Li I equivalent width (see Sect. 4.2) are plotted as filled circles. More evolved stars are indicated as open circles. The transverse curve represents the Galactic plane.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{5602fig3.eps}\end{figure}$	Figure 3: Our spectral types as a function of the $(V-I)_{\rm C}$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[bb=50 269 530 769,clip]{5602fig4.eps}}\end{figure}$	Figure 4: Distribution of Li equivalent width as a function of the $(V-I)_{\rm C}$ . The lines represents the upper and lower limits for Pleiades members.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{5602fig6.eps}}\end{figure}$	Figure 6: HR diagram from the proposed members of the $\beta$ Pic Association. The isochrones over-plotted are those from Siess et al. (2000). The dotted and dashed lines correspond to the isochrones for 5 Myr and 50 Myr, respectively. The isochrone for 10 Myr is shown as thick solid line whereas the observational isochrone is represented as a thick dotted-dashed line.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{5602fig7.eps}}\end{figure}$	Figure 7: Correlation between the X-position and U-component of space velocity vector showing an expansion of the members of the $\beta$ Pic Association. Objects whose parallaxes are from Hipparcos Catalogue are overplotted with squares.
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$\begin{figure} \par\begin{tabular}{c} \resizebox{17.8cm}{!}{\includegraphics{560... ...aphics{5602fg8e.eps}\includegraphics{5602fg8f.eps}}\\ \end{tabular}\end{figure}$	Figure 8: Combinations of the sub-spaces of the UVWXYZ-space showing a well defined clustering in both kinematical and spatial coordinates.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{5602fig9.eps}}\end{figure}$	Figure 9: Distribution of Li equivalent width as a function of the $(V-I)_{\rm C}$ for the proposed members of the $\beta$ Pic Association shown in Table 6. The hatched area shows the Li equivalent width range observed for the Pleiades members.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{5602fg10.eps}}\end{figure}$	Figure 10: Distribution of Li abundances as a function of the effective temperature for the proposed members of the $\beta$ Pic Association (Table 7). The hatched area shows the Li abundances with range observed for the Pleiades members.
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