All Figures

$\begin{figure} \par\includegraphics[angle=0,width=13.5cm]{2911fig1.ps} \end{figure}$ Figure 1: Distribution of nearby halo stars in velocity space for our selected sample with ${\rm [Fe/H]\le -1.5}$ dex within 1 kpc of the Sun. ( a)-c)) Velocity projections in the (U, V, W) space; d) Velocity direction: the position of each particle is given by the spherical angular coordinates ${\mbox{\boldmath $\alpha$ }}=(\phi, \theta)$ of the velocity vector. Of the 192 stars present in this volume, the 5% fastest are highlighted as light color dots. Among them, the asterisks identify those objects/groups with velocity difference less than ${\rm 42~km~s^{-1}}$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90,width=8.8cm]{2911fig2.ps}} \end{figure}$ Figure 2: $(\phi,~\theta)$ -space number counts for a partition with 24 cells with $\Delta \theta =45^\circ$ (mean value $\theta _{\rm c}$ ) and $\Delta \phi =45^\circ /90^\circ$ for the stripes along the equator and close to the poles, respectively. The solid line corresponds to the selected sample within 1 kpc of the Sun and the dashed histogram to the average number of counts in our Monte Carlo simulations. Error bars are based on Poisson statistics.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90,width=8.8cm]{2911fig3.ps}} \end{figure}$ Figure 3: Two-point velocity correlation function for our selected sample within 1 kpc (asterisks) and for the 5% fastest moving stars (diamonds). In both cases, there is a signal at small velocity differences indicative of the presence of streams. The error bars are based on Poisson counts.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=13cm]{2911fig4.ps}\end{figure}$ Figure 4: Distribution of 2348 dark matter particles from a CDM simulation located in a sphere of 2 kpc radius centered at 8 kpc from the Galaxy center. ( a)-c)) Velocity projections in the (v₁, v₂, v₃) space; d) Velocity directions. The solid gray circles denote the 5% most energetic particles, while the asterisks identify those subsets whose velocity difference is less than 42 km s^-1. The kinematics characteristics observed in this set of plots are representative of what is seen in other similar volumes.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90,width=8.8cm]{2911fig5.ps}}\end{figure}$ Figure 5: Velocity correlation function $\xi (v)$ for the volume shown in Fig. 4. Asterisks and diamonds correspond to $\xi$ for the full sample and for the subset of 5% fastest moving particles, respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=13cm]{2911fig6.ps} \end{figure}$ Figure 6: Distribution of the selected sample of 410 stars with D<2 kpc in the space of adiabatic invariants. The asterisks denote our kinematic group (RHLS), and the grey diamonds the clump identified by Helmi et al. (1999) (HWdZZ). These stars are used to define a region (limited by the dashed lines in the left panel), which also encompasses other stars with similar angular momenta and which are indicated as diamonds in both panels. CD - 80 328, the candidate from the Nordström et al. (2004) catalog, has been added and is shown as a triangle.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90,width=8.8cm]{2911fig3.ps}} \end{figure}$	Figure 3: Two-point velocity correlation function for our selected sample within 1 kpc (asterisks) and for the 5% fastest moving stars (diamonds). In both cases, there is a signal at small velocity differences indicative of the presence of streams. The error bars are based on Poisson counts.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90,width=8.8cm]{2911fig5.ps}}\end{figure}$	Figure 5: Velocity correlation function $\xi (v)$ for the volume shown in Fig. 4. Asterisks and diamonds correspond to $\xi$ for the full sample and for the subset of 5% fastest moving particles, respectively.
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