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$\begin{figure} \par\includegraphics[height=7.5cm,width=7.6cm,clip]{1080fig1.ps}\end{figure}$ Figure 1: Tangential velocity distributions, $\psi (V_{\alpha },V_{\delta })$ , toward the direction ( $l=143^\circ$ , $b=-57^\circ$ ) of WD0135-039 (solid circle). The ellipses show the iso-probability contours (2 $\sigma$ , 3 $\sigma$ ) of the thin disk, thick disk, and local halo populations based on the kinematic parameters from Binney & Merrifield (1998), Soubiran et al. (2003) and Casertano et al. (1990), respectively. The three concentric circles indicate the velocity thresholds, $V_{\rm min} = 4.74 \mu _{\rm lim} r$ , for the OHDHS survey ( $\mu _{\rm lim}=0.33''$ yr^-1) at the distances r=40 pc, 80 pc and 120 pc.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{1080fig2.ps} \end{figure}$ Figure 2: Left panel: iso-probability contours (1 $\sigma$ , 2 $\sigma$ , 3 $\sigma$ ) of $\psi (V_{\alpha },V_{\delta })$ compared to a Montecarlo simulation (dots) of the thick disk stars in the direction ( $l=226\hbox{$.\!\!^\circ$ } 34$ , $b=-64\hbox{$.\!\!^\circ$ }27$ ) of LHS 1447 (solid circle) drawn from the kinematically selected distribution, $h(V_{\alpha },V_{\delta })$ . Right panel: iso-probability contours (confidence levels of 40%, 70%, 95% and 99%) of $h(V_{\alpha },V_{\delta })$ .
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=13cm,clip]{1080fig3.ps} \end{figure}$ Figure 3: Left panel: iso-probability contours (1 $\sigma$ , 2 $\sigma$ , 3 $\sigma$ ) of $\psi (V_{\alpha },V_{\delta })$ compared to a Montecarlo simulation (dots) of the thick disk stars in the direction ( $l=226\hbox{$.\!\!^\circ$ } 34$ , $b=-64\hbox{$.\!\!^\circ$ }27$ ) of LHS 1447 (solid circle) drawn from the kinematically selected distribution, $t(V_{\alpha },V_{\delta }\vert r)$ . Right panel: iso-probability contours (confidence levels of 40%, 70%, 95% and 99%) of $t(V_{\alpha },V_{\delta }\vert r)$ .
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{1080fig4.ps} \end{figure}$ Figure 4: Velocity distribution (U,V,W) of the subsample of 15 stars with available radial velocity (dots with 1 $\sigma$ error bars) from Salim et al. (2004). The objects selected by means of the distributions $h(V_{\alpha },V_{\delta })$ and $t(V_{\alpha },V_{\delta }\vert r)$ with a 95% confidence level (Table 4) are marked with circle and diamond symbols, respectively. The ellipses show the $3\sigma$ iso-probability contours of the thick disk and halo velocity distribution.
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In the text