All Figures

$\begin{figure} \par\includegraphics[width=7.35cm,clip]{6146fig1.ps}\end{figure}$ Figure 1: Examples of typical spectra for different spectral types obtained with the NOT telescope.
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{6146fig2.ps}\end{figure}$ Figure 2: Spectral type distribution of the stellar population of the NEP stars predicted with XCOUNT (shaded histogram). Empty hystogram marks the actual observed stars.
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{6146fig3.ps}\end{figure}$ Figure 3: Age distribution of the stellar population of the NEP stars predicted with XCOUNT. The predicted stellar population is equally dominated by intermediate-age and old stars.
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{6146fig4.ps}\end{figure}$ Figure 4: ${\rm Log}~(N)-{\rm Log}~(S)$ predicted with XCOUNT toward the NEP. Flux is expressed in ROSAT/PSPC count rate. Short dashed, long-dashed, and solid lines are the contributions of young, intermediated and old stars, respectively. Vertical dashed lines mark the range of limiting sensitivity of the survey. At the NEP sensitivity, intermediate and old populations dominate the stellar sources. At higher fluxes also the youngest stars give a large contribution, while at faint fluxes the stellar population is largely dominated by oldest stars.
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{6146fig5.ps}\end{figure}$ Figure 5: ${\rm Log}~(N)-{\rm Log}~(S)$ predicted with XCOUNT toward the NEP. Flux is expressed in ROSAT/PSPC count rate as in Fig. 4. Figure shows the contribution from dA, dF, dG, dK, and dM stars (going from the lower contribution to the the largest). Vertical dashed lines mark the range of limiting sensitivity of the survey.
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{6146fig6.ps}\end{figure}$ Figure 6: Observed and predicted ${\rm Log}~(N)-{\rm Log}~(S)$ toward the NEP. Flux is expressed in ROSAT/PSPC count rate as in Fig. 5. The upper line is the total expected $\log N-\log S$ and the points are the observations. The lower line represents the predictions for A and early F(label "A'') stars, while the two dotted overimposed lines are the predictions for G-K and dM stars, respectively (labels "G'' and "M''). The observed A and early F stars are marked by the lower irregular line, while observed dM stars are the intermediate irregular line, and the upper one is the observed $\log N-\log S$ of dG and dK stars.
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In the text

$\begin{figure} \par\includegraphics[width=7.35cm,clip]{6146fig1.ps}\end{figure}$	Figure 1: Examples of typical spectra for different spectral types obtained with the NOT telescope.
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$\begin{figure} \par\includegraphics[width=6.4cm,clip]{6146fig2.ps}\end{figure}$	Figure 2: Spectral type distribution of the stellar population of the NEP stars predicted with XCOUNT (shaded histogram). Empty hystogram marks the actual observed stars.
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$\begin{figure} \par\includegraphics[width=6.4cm,clip]{6146fig3.ps}\end{figure}$	Figure 3: Age distribution of the stellar population of the NEP stars predicted with XCOUNT. The predicted stellar population is equally dominated by intermediate-age and old stars.
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$\begin{figure} \par\includegraphics[width=7.15cm,clip]{6146fig5.ps}\end{figure}$	Figure 5: ${\rm Log}~(N)-{\rm Log}~(S)$ predicted with XCOUNT toward the NEP. Flux is expressed in ROSAT/PSPC count rate as in Fig. 4. Figure shows the contribution from dA, dF, dG, dK, and dM stars (going from the lower contribution to the the largest). Vertical dashed lines mark the range of limiting sensitivity of the survey.
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