All Figures

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{Famaey_scale4_background.ps}\end{figure}$ Figure 1: Contours and wavelet coefficients in the [U,V] plane for the Famaey et al. (2005) sample. Black: isocontours of the velocity distribution smoothed over 14 km s^-1. The color scales with the wavelet coefficients at scale 4 (14 km s^-1) after thresholding. The four structures observed in the wavelet space correspond to the Hercules stream ( bottom green structures), Pleiades and Hyades ( middle red structures from right to left), and Sirius (yellow, top). The limit of the structures in the wavelet space are used to select the samples for further analysis.
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{histoU_Pleiades.eps}\vspac... ...}\vspace*{3mm} \includegraphics[width=6.3cm,clip]{histoU_Sirius.eps}\end{figure}$ Figure 2: Top: U distribution of stars from the Famaey et al. (2005) sample for the Pleiades strip $-28 \le V$ (km s^-1) $\le$ -18. The thick solid line is a fit to the observed distribution, resulting from the superposition of three Gaussians (with parameters listed in Table 1), corresponding to the background component (thin solid line), to the full Pleiades component and partial Hyades component (thin dashed lines). Middle: same as top for the Hyades strip $-24 \le V$ (km s^-1) $\le$ -12 (with parameters listed in Table 2). Bottom: same as top and middle for the Sirius strip $-5 \le V$ (km s^-1) $\le$ 8 (with parameters listed in Table 3).
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{HR_Pleiades_gaussian.eps}\... ...ace*{2mm} \includegraphics[width=6.3cm,clip]{HR_Sirius_gaussian.eps}\end{figure}$ Figure 3: Top: comparison of the 100 Myr isochrone (Z=0.02) from Schaller et al. (1992) and Lejeune & Schaerer (2001), with the stars kinematically associated with the Pleiades cluster/moving group. Note that absolute magnitudes have been derived from a simple inversion of the parallax, and are thus biased, which is not a problem for the subsequent analysis done in parallax space. Stars whose parallax is within $2\sigma$ of the isochrone parallax are marked with filled circles while others are marked with open circles. Middle: same for the stars kinematically associated with the Hyades cluster/moving group and the 600 Myr isochrone. The effect of metallicity is also shown. Bottom: same for the stars kinematically associated with the Sirius cluster/moving group and the 300 Myr isochrone.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{boxgauss_Pleiades.eps}\end{figure}$ Figure 4: Histogram of $\delta$ (see Eq. (7)) for the Pleiades moving group, together with the Gaussian $\tilde{N}$ (see Eq. (8)) expected for the Pleiades moving group if all stars in the group were on the 100 Myr isochrone. The subtraction of $\tilde{N}$ from the observed histogram is negative (significantly with respect to Poissonian errors) at $\delta =0$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{boxgauss_Hyades.eps}\end{figure}$ Figure 5: Same as Fig. 4 for the Hyades moving group and the 600 Myr isochrone.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{compa_Hyades.eps}\end{figure}$ Figure 6: The shaded area is the histogram of $\delta$ for the 600 Myr isochrone in the comparison box U=[21,35], V=[-24,-12], compared with ( top) the histogram of $\delta$ in the Hyades box (background+moving group), and ( bottom) the histogram of $\delta$ expected for the background, if all stars of the Hyades overdensity were coeval (600 Myr), after subtracting the $\tilde{N}$ histogram of Fig. 5. All histograms are normalized to the number of stars in the comparison box.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{boxgauss_Sirius.eps}\end{figure}$ Figure 7: Same as Figs. 4 and 5 for the Sirius moving group and the 300 Myr isochrone.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{compa_Sirius.eps}\end{figure}$ Figure 8: The shaded area is the histogram of $\delta$ for the 300 Myr isochrone in the comparison box U=[-16,2], V=[-5,8], compared with ( top) the histogram of $\delta$ in the Sirius box (background+moving group); and ( bottom) the histogram of $\delta$ expected for the background if all stars of the Sirius overdensity were coeval (300 Myr), after subtracting the $\tilde{N}$ histogram of Fig. 7. All histograms are normalized to the number of stars in the comparison box.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{boxgauss_Pleiades.eps}\end{figure}$	Figure 4: Histogram of $\delta$ (see Eq. (7)) for the Pleiades moving group, together with the Gaussian $\tilde{N}$ (see Eq. (8)) expected for the Pleiades moving group if all stars in the group were on the 100 Myr isochrone. The subtraction of $\tilde{N}$ from the observed histogram is negative (significantly with respect to Poissonian errors) at $\delta =0$ .
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$\begin{figure} \par\includegraphics[width=6.2cm,clip]{boxgauss_Hyades.eps}\end{figure}$	Figure 5: Same as Fig. 4 for the Hyades moving group and the 600 Myr isochrone.
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$\begin{figure} \par\includegraphics[width=6.2cm,clip]{boxgauss_Sirius.eps}\end{figure}$	Figure 7: Same as Figs. 4 and 5 for the Sirius moving group and the 300 Myr isochrone.
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