All Figures

$\begin{figure} \par\includegraphics[width=16cm,clip]{5696f1.ps} \end{figure}$ Figure 1: Galactic distribution of the fields of the XBSS (Della Ceca et al. 2004): circles, triangles, and squares are used to represent observations carried out using the Thin, Medium, and Thick filters in MOS2, respectively. Filled symbols are plotted for those fields where stellar counterparts have been identified. The position of the Gould Belt is shown (continuous line), with a width of $\pm$ $5^\circ$ (dashed lines).
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8cm]{5696f2a.ps}\hspace{3mm} \includegraphics[width=8cm,clip]{5696f2b.ps} } \end{figure}$ Figure 2: a) Colour-colour NIR diagram for the stars in the BSS. Dashed and dotted lines are the main-sequence track and the giant branch defined by Bessell & Brett (1989) transformed here to the 2MASS system (see text). Spectral types of the main sequence are labelled with roman font, at the corresponding J-H value but offset in $H-K_{\rm s}$ . Similarly, italic font has been utilised for labelling the spectral types of the giant branch. b) $J-K_{\rm s}$ distribution of the sources in a).
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{5696f3.ps} \end{figure}$ Figure 3: a) Temperature distribution for the sources where a 1T-model has been fitted. b) Distribution of T₁ and T₂ of the stars where two thermal components have been fitted. c) Distribution of EM₁/EM₂ of the stars in Fig. b.
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In the text

$\begin{figure} \par\mbox{ \includegraphics{5696f4a.ps}\hspace{0.3cm} \includegr... ... {\hspace*{4.8cm}\includegraphics{5696f4e.ps}\hspace*{4.8cm}} \end{figure}$ Figure 4: X-ray light curves of the most prominent variable sources in our sample ( E = 0.5-10 keV). The curves have been corrected for background (see text for details), GTI, and dead-time effects. EPIC-PN data were used except for XBS J014100.6-675328 (BL Hyi), where we chose EPIC-MOS1 data to also show the first emission decay.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=4cm,clip]{5696f5a.ps} \includegr... ...clip]{5696f5c.ps} \includegraphics[width=4cm,clip]{5696f5d.ps} } \end{figure}$ Figure 5: Colour distributions predicted by XCOUNT (continuous line) compared with the observed one (dashed line) for different stellar birthrates assuming an exponential law $\Psi = A {\rm e}^{-t/\tau }$ .
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=7.8cm,clip]{5696f6a.ps} \include... ...ip]{5696f6c.ps} \includegraphics[width=7.8cm,clip]{5696f6d.ps} } \end{figure}$ Figure 6: Colour distributions predicted by XCOUNT for different stellar birthrates assuming an exponential law $\Psi = A {\rm e}^{-t/\tau }$ . The contribution of different age-subgroups to the total source counts is shown in each plot.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5696f7.ps} \end{figure}$ Figure 7: Log N-Log S predicted assuming $\tau = \infty$ , +15, +5, and -15 Gyr, compared with the BSS results (thick solid line) for the fields observed with the medium filter (energy band 0.5-4.5 keV). For the comparison we used a standard high latitude direction $b = 60^\circ$ .
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{5696f3.ps} \end{figure}$	Figure 3: a) Temperature distribution for the sources where a 1T-model has been fitted. b) Distribution of T₁ and T₂ of the stars where two thermal components have been fitted. c) Distribution of EM₁/EM₂ of the stars in Fig. b.
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$\begin{figure} \par\mbox{ \includegraphics{5696f4a.ps}\hspace{0.3cm} \includegr... ... {\hspace{4.8cm}\includegraphics{5696f4e.ps}\hspace{4.8cm}} \end{figure}$	Figure 4: X-ray light curves of the most prominent variable sources in our sample ( E = 0.5-10 keV). The curves have been corrected for background (see text for details), GTI, and dead-time effects. EPIC-PN data were used except for XBS J014100.6-675328 (BL Hyi), where we chose EPIC-MOS1 data to also show the first emission decay.
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$\begin{figure} \par\mbox{\includegraphics[width=4cm,clip]{5696f5a.ps} \includegr... ...clip]{5696f5c.ps} \includegraphics[width=4cm,clip]{5696f5d.ps} } \end{figure}$	Figure 5: Colour distributions predicted by XCOUNT (continuous line) compared with the observed one (dashed line) for different stellar birthrates assuming an exponential law $\Psi = A {\rm e}^{-t/\tau }$ .
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$\begin{figure} \par\mbox{\includegraphics[width=7.8cm,clip]{5696f6a.ps} \include... ...ip]{5696f6c.ps} \includegraphics[width=7.8cm,clip]{5696f6d.ps} } \end{figure}$	Figure 6: Colour distributions predicted by XCOUNT for different stellar birthrates assuming an exponential law $\Psi = A {\rm e}^{-t/\tau }$ . The contribution of different age-subgroups to the total source counts is shown in each plot.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5696f7.ps} \end{figure}$	Figure 7: Log N-Log S predicted assuming $\tau = \infty$ , +15, +5, and -15 Gyr, compared with the BSS results (thick solid line) for the fields observed with the medium filter (energy band 0.5-4.5 keV). For the comparison we used a standard high latitude direction $b = 60^\circ$ .
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