All Figures

$\begin{figure} \par\includegraphics[angle=270,width=5cm,clip]{1393_f01.ps}\par\v... ...space*{2mm} \includegraphics[angle=270,width=5cm,clip]{1393_f05.ps} \end{figure}$ Figure 1: The distribution of observed $(b-r)_{\rm C}$ colors in the fields. The dotted line shows the color cut between halo and disk. Note that the ordinate has not the same scale in all cases, whereas the dotted line extends to 20 in each plot. The maxima are not located at the same colors, but depend on the direction of the field.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{1393_f06.ps} \end{figure}$ Figure 2: The stars in the five fields in a two color diagram ((b-r) versus (r-i)). The spread becomes significant at $(b-r) \geq 1.0$ . The solid line is the mean main sequence track, onto which the (b-r) colours of the stars are projected along the R isophotes of varying metallicity (dotted lines). For some extremely red stars, photometric errors are plotted.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=12.4cm,clip]{1393_f07.ps} \end{figure}$ Figure 3: Spatial distribution of metallicity corrected $(b-r)_{{\rm corr}}$ . The solid line represents the distance dependent upper color limit at $R=23^{\rm mag}$ , the dashed line is the lower limit due to the selection criterium of the fields (no star brighter than $R\approx 15.5$ ). Since the metal-poor halo stars are intrinsically fainter, the color limits are shifted accordingly. The horizontal line at $(b-r)_{\rm corr}=0.75$ denotes the cut between halo and disk stars in the 13h field (which is why stars can be found "outside the boundaries'': the color cut is different in each field, see Fig. 1), the dashed-dotted line indicates the cutoff at $(b-r)_{{\rm corr}}=1.8$ due to the metallicity correction. The different symbols refer to the different fields: squares - 1 h field, triangles - 9 h field, dots - 13 h field, open circles - 16 h field, crosses - 23 h field.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1393_f08.ps}\hspace*{3mm} \i... ...f12.ps}\hspace*{3mm} \includegraphics[width=7cm,clip]{1393_f13.ps} \end{figure}$ Figure 4: $\chi ^2$ plane for the parameters h₂ and n₂/(n₁+n₂) for the fit of the measured density distribution in the five fields, and the mean $\chi ^2$ of all five ones ( bottom right). The scalelength is assumed to be h_r=3.5 kpc, and the values of h₁ are given in Table 2. The contour lines show the $1\sigma$ , $2\sigma$ and $3\sigma$ confidence levels.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=5cm,clip]{1393_f14.ps}\par\v... ...ce*{2.5mm}% \includegraphics[angle=270,width=5cm,clip]{1393_f18.ps} \end{figure}$ Figure 5: Density distribution of the stars in the disk. The solid line is the best fit for a sum of two exponentials.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=5cm,clip]{1393_f19.ps}\par\v... ...space*{3mm} \includegraphics[angle=270,width=5cm,clip]{1393_f23.ps} \end{figure}$ Figure 6: Density distribution of all stars. The solid lines are the best fits for the disk (as in Fig. 5) and a spherical halo, the dashed line is the fit for a flattened halo with axial ratio (c/a)=0.6. The corresponding exponents $\alpha$ are given in Table 3). The dotted line is the sum of disk and spherical halo (which is slightly favoured by the fit).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.4cm,clip]{1393_f24.ps}\par... ...ace*{2mm} \includegraphics[angle=270,width=6.4cm,clip]{1393_f26.ps} \end{figure}$ Figure 7: Upper panel: the mean SLF of the five CADIS fields (solid line). For the calculation of the effective volumes we used the fitted values of h₁ (see Table 2). The dotted and dashed lines are the determination for h₁=0.250 kpc, and for h₁=0.350 kpc, respectively. Middle panel: The solid line is our current measurement, as in the upper panel. The dotted line is our first measurement as published in Paper I, the dashed line is the local SLF (Jahreiß & Wielen 1997), which is based on HIPPARCOS parallaxes. Lower panel: weighted mean of CADIS and local SLF, in comparison with a photometric SLF which is based on HST observations (Gould et al. 1998).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1393_f27.ps}\hspace*{2mm} \i... ..._f31.ps}\hspace*{2mm} \includegraphics[width=7cm,clip]{1393_f32.ps} \end{figure}$ Figure 8: The C planes of the five fields for the parameter h₂ and n₂/(n₁+n₂) (with h_r=3500 pc, h₁=300 pc, (c/a)=0.6,and $\alpha =2.5$ ). The plot in the lower right corner is the mean of the five indidual fields. The contour lines show the $1\sigma$ , $2\sigma$ , and $3\sigma$ confidence levels.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{1393_f33.ps}\hspace*{3mm} ... ...}\par\vspace*{3mm} \includegraphics[width=5.5cm,clip]{1393_f37.ps} \end{figure}$ Figure 9: The number density of stars in the (b-r)_C- $R_{\rm C}$ plane, for the five fields. The densities are normalised to the total number of stars in each field. The images have been rebinned in steps of 0.1 in both color and magnitude. The contours overlaid are the simulated data for h_r=3500 pc, h₁=300 pc, h₂=900 pc, n₂/(n₁+n₂)=0.09, (c/a)=0.6and $\alpha =2.5$ , also normalised to the number of simulated stars. The contours are plotted for $0.001 \leq N \leq 0.015$ in steps of 0.001.
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In the text

$\begin{figure} \par {\psfig{figure=1393_f38.ps,angle=270,clip=t,width=5.6cm} } \... ...e*{2mm} {\psfig{figure=1393_f42.ps,angle=270,clip=t,width=5.6cm} }\end{figure}$ Figure 10: Comparison of absolute V band magnitudes of the simulation (dotted line) with the CADIS data (solid line), for the best fit case.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=5cm,clip]{1393_f01.ps}\par\v... ...space*{2mm} \includegraphics[angle=270,width=5cm,clip]{1393_f05.ps} \end{figure}$	Figure 1: The distribution of observed $(b-r)_{\rm C}$ colors in the fields. The dotted line shows the color cut between halo and disk. Note that the ordinate has not the same scale in all cases, whereas the dotted line extends to 20 in each plot. The maxima are not located at the same colors, but depend on the direction of the field.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{1393_f06.ps} \end{figure}$	Figure 2: The stars in the five fields in a two color diagram ((b-r) versus (r-i)). The spread becomes significant at $(b-r) \geq 1.0$ . The solid line is the mean main sequence track, onto which the (b-r) colours of the stars are projected along the R isophotes of varying metallicity (dotted lines). For some extremely red stars, photometric errors are plotted.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{1393_f08.ps}\hspace{3mm} \i... ...f12.ps}\hspace{3mm} \includegraphics[width=7cm,clip]{1393_f13.ps} \end{figure}$	Figure 4: $\chi ^2$ plane for the parameters h₂ and n₂/(n₁+n₂) for the fit of the measured density distribution in the five fields, and the mean $\chi ^2$ of all five ones ( bottom right). The scalelength is assumed to be h_r=3.5 kpc, and the values of h₁ are given in Table 2. The contour lines show the $1\sigma$ , $2\sigma$ and $3\sigma$ confidence levels.
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$\begin{figure} \par\includegraphics[angle=270,width=5cm,clip]{1393_f14.ps}\par\v... ...ce*{2.5mm}% \includegraphics[angle=270,width=5cm,clip]{1393_f18.ps} \end{figure}$	Figure 5: Density distribution of the stars in the disk. The solid line is the best fit for a sum of two exponentials.
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$\begin{figure} \par\includegraphics[angle=270,width=5cm,clip]{1393_f19.ps}\par\v... ...space*{3mm} \includegraphics[angle=270,width=5cm,clip]{1393_f23.ps} \end{figure}$	Figure 6: Density distribution of all stars. The solid lines are the best fits for the disk (as in Fig. 5) and a spherical halo, the dashed line is the fit for a flattened halo with axial ratio (c/a)=0.6. The corresponding exponents $\alpha$ are given in Table 3). The dotted line is the sum of disk and spherical halo (which is slightly favoured by the fit).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{1393_f27.ps}\hspace{2mm} \i... ..._f31.ps}\hspace{2mm} \includegraphics[width=7cm,clip]{1393_f32.ps} \end{figure}$	Figure 8: The C planes of the five fields for the parameter h₂ and n₂/(n₁+n₂) (with h_r=3500 pc, h₁=300 pc, (c/a)=0.6,and $\alpha =2.5$ ). The plot in the lower right corner is the mean of the five indidual fields. The contour lines show the $1\sigma$ , $2\sigma$ , and $3\sigma$ confidence levels.
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$\begin{figure} \par {\psfig{figure=1393_f38.ps,angle=270,clip=t,width=5.6cm} } \... ...e*{2mm} {\psfig{figure=1393_f42.ps,angle=270,clip=t,width=5.6cm} }\end{figure}$	Figure 10: Comparison of absolute V band magnitudes of the simulation (dotted line) with the CADIS data (solid line), for the best fit case.
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