All Figures

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1793fig1.ps} \end{figure}$ Figure 1: CMD of single H IPPARCOS stars with $\Delta (B-V)\leq 0.025$ and $\frac{\Delta \pi}{\pi}\leq20\%$ . The stars inside the window are our selected RHB candidates. The window borders are: $(B-V)\geq 0.5$ , $M_V\in\{-0.5~1.8\}$ , $M_V\leq -2.8+7\cdot (B-V)$ , $M_V\leq 7.3-6.2\cdot (B-V)$ . The dash-dotted line marks the window separation border of Sect. 4.4.3 while the dashed line marks the alternative cut-off of Sect. 4.4.2.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{1793fig2.ps} \end{figure}$ Figure 2: The Toomre diagram of our $\frac{\Delta \pi}{\pi}$ $\leq$ 30% sample. The circles show the peculiar velocity $v_{\rm pec}=\sqrt {\Phi ^2+W^2+(\Theta -\Theta _{{\rm LSR}})^2}$ with respect to the LSR. Up to a peculiar velocity of 50 ${\rm km~s^{-1}}$ the sample is distributed rather evenly. Upwards of these values the stars fall short in orbital velocity. These objects are halo and thick disk stars.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1793fig3.ps} \end{figure}$ Figure 3: The Bottlinger diagram of our $\frac{\Delta \pi}{\pi}$ $\leq$ 30% sample. The panels at right show the enlarged regions marked by squares in the left panels. Heavier points are for the Halo Population Sample (HPS) stars. The circle symbols denote solar values. Note the two groups of stars in the more detailed $\Theta ,\Phi$ panel.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{1793fig4.ps} \end{figure}$ Figure 4: Meridian plots of some of the calculated orbits in a model by Allen & Santillan (1991). The top row shows orbits of HPS stars. The middle row shows the orbit of the fastrunner star HIP 98269 ( left) while the other two are thick disk candidates. The bottom row depicts thin disk orbits.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1793fig5.ps} \end{figure}$ Figure 5: Logarithmic histograms, that show the complete $\frac{\Delta \pi}{\pi}$ $\leq$ 30% sample (gray) and the contribution of our HPS stars (black). We have added a constant offset for visibility reasons. The ecc-histogram shows a separation of populations around 0.45. As expected, the halo stars show much higher eccentricities than the disk stars. In the nze-histogram the halo stars do not only build the tail of the distibution, but also account for low values. The peak on the right side of the diagram includes the stars with higher normalized z-extent than plotted.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1793fig6.ps} \end{figure}$ Figure 6: Diagram of $\Theta$ (gray triangles) and $\Theta _{\rm med}$ (black squares) against total kinetic energy and median kinetic energy, respectively. Filled symbols are stars of the HPS. The parabolas are isovelocity lines for $v_{\perp }$ , which is orthogonal to $\Theta$ . Medianised values lie on an almost straight line pointing from the LSR data point towards lower $E_{\rm kin,med}$ and $\Theta _{\rm med}$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.3cm,clip]{1793fig7.ps} \end{figure}$ Figure 7: The z-probability distribution of our $\frac{\Delta \pi}{\pi}$ $\leq$ 30% stars with a two-component and a three-component z-distribution exponential fit, shown in the left and right halves of the diagram, respectively. Fitted curves are: thin dashed ones the individual population components (see Sect. 4.3), thick dashed ones are the complete fits. Note that the three-component fit is a better approximation of the actual distribution.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{1793fig8.ps} \end{figure}$ Figure 8: Meridian plots of some of the calculated orbits in the "2b'' potential by Dehnen & Binney (1998). The same stars as in Fig. 4 were used to allow comparisons. The orbits shown are the ones differing most between the AS and DB potential models (see Sect. 5).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1793fig9.ps} \end{figure}$ Figure 9: Comparison of the eccentricities a) and normalized z-extents b) of our stars in the potential of Allen & Santillan (AS) and the "2b'' potential of Dehnen & Binney (DB). The HPS stars are given as filled symbols, the others as grey open circles. Orbits are less eccentric in the DB than in the AS potential. In nze there is a large scatter in the differences.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.4cm,clip]{1793fi10.ps} \end{figure}$ Figure 10: The z-distribution of our $\frac{\Delta \pi}{\pi}$ $\leq$ 30% RHB sample in the "2b'' potential by DB. The maximum |Z| values are roughly 18 kpc, which is lower than in a potential from AS. This flatter distribution of the halo group is reflected in the fit parameters: $h_{\rm thin}=0.12$ kpc; $N_{\rm thin}(0)=4.8$ $\times$ 10⁶; $h_{\rm thick}=0.58$ kpc; $N_{\rm thick}(0)=51~000$ ; $h_{\rm halo}=3.4$ kpc; $N_{\rm halo}(0)=1700$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1793fig3.ps} \end{figure}$	Figure 3: The Bottlinger diagram of our $\frac{\Delta \pi}{\pi}$ $\leq$ 30% sample. The panels at right show the enlarged regions marked by squares in the left panels. Heavier points are for the Halo Population Sample (HPS) stars. The circle symbols denote solar values. Note the two groups of stars in the more detailed $\Theta ,\Phi$ panel.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{1793fig4.ps} \end{figure}$	Figure 4: Meridian plots of some of the calculated orbits in a model by Allen & Santillan (1991). The top row shows orbits of HPS stars. The middle row shows the orbit of the fastrunner star HIP 98269 ( left) while the other two are thick disk candidates. The bottom row depicts thin disk orbits.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{1793fig8.ps} \end{figure}$	Figure 8: Meridian plots of some of the calculated orbits in the "2b'' potential by Dehnen & Binney (1998). The same stars as in Fig. 4 were used to allow comparisons. The orbits shown are the ones differing most between the AS and DB potential models (see Sect. 5).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1793fig9.ps} \end{figure}$	Figure 9: Comparison of the eccentricities a) and normalized z-extents b) of our stars in the potential of Allen & Santillan (AS) and the "2b'' potential of Dehnen & Binney (DB). The HPS stars are given as filled symbols, the others as grey open circles. Orbits are less eccentric in the DB than in the AS potential. In nze there is a large scatter in the differences.
Open with DEXTER