All Figures

$\begin{figure} \par\includegraphics[width=13.35cm,clip]{7091fg01.ps}\end{figure}$ Figure 1: Spatial distribution in Galactic coordinates of sources detected so far by ISGRI. The figure at the top presents the distributions of HMXBs (stars), LMXBs (squares) and miscellaneous sources (triangles). The figure at the bottom displays extragalactic sources (circles) and unclassified sources (crosses). The directions to the spiral arm tangents and other areas of interest are indicated, as are the cumulative exposure times at each location (from public data in revs. 30-484). The number of sources in each class is listed in Table 2.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{7091fg02.ps}\end{figure}$ Figure 2: Galactic distribution of HMXBs (49, circles), LMXBs (74, squares), miscellaneous sources (37, triangles), and unclassified sources (3, inverted triangles). Filled symbols represent IGR sources. Also plotted is the 4-arm Galactic spiral model from Russeil (2003) with the Sun located at 8.5 kpc from the centre. The concentric circles indicate radii of 1, 3, 5,..., kpc from the centre.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{7091fg03.ps}\end{figure}$ Figure 3: Distribution of galactocentric distances of HMXBs (49, shaded histogram) and LMXBs (74, thick histogram). The dashed histogram represents OB star-forming complexes from Russeil (2003) (divided by 2).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{7091fg04.ps}\end{figure}$ Figure 4: Galactic distribution of HMXBs whose distance are known (49, star symbols) and the locations of star-forming complexes from Russeil (2003) (464, circles). The symbol size of the latter is proportional to the activity of the complex. HMXBs whose distances are unknown have been placed at 8.5 kpc (23, pentagons).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{7091fg05.ps}\end{figure}$ Figure 5: Histograms of Galactic longitudes integrated over the latitude for HMXBs with $\vert b\vert<6^{\circ }$ (shaded histogram) and star-forming regions from Russeil (2003) (thick histogram, divided by 3) and from Bronfman et al. (1996) (dashed histogram, divided by 10). The vertical lines indicate the tangential directions of the 4-arm spiral model from Russeil (2003).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7091fg06.ps}\end{figure}$ Figure 6: Angular distribution (in degrees, for $\vert b\vert < 20^{\circ }$ ) from the Galactic plane of sources that have been detected by ISGRI. Shaded histograms are HMXBs ( left) and AGN ( right), and the clear histograms represent LMXBs ( left) and miscellaneous sources ( right). The dashed histogram denotes unclassified sources. The distributions have been summed over the northern and southern Galactic hemispheres. The curves represent fits to the data from the model and parameters described in the text.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{7091fg07.ps}\end{figure}$ Figure 7: Vertical scale height (in kpc) from the Galactic plane of HMXBs, LMXBs and miscellaneous sources whose distances are known. The distributions have been summed over the northern and southern Galactic hemispheres. Sources from the Magellanic Clouds are excluded. The curves represent the exponential model described in the text fit to the data (see Table 3 for parameters).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7091fg08.ps}\end{figure}$ Figure 8: The distribution of reported column densities ( $N_{{\rm H}}$ ) for Galactic sources (including sources in the Magellanic Clouds) detected by ISGRI that were previously known (152, clear histogram) and for IGRs (41, shaded histogram).
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In the text

$\begin{figure} \par\includegraphics[width=12.9cm,clip]{7091fg09.ps}\end{figure}$ Figure 9: Spatial distribution, in Galactic coordinates, of all sources detected by ISGRI for which $N_{{\rm H}}$ has been reported. The symbol size is proportional to the published column density. The figure at the top shows the whole sky and includes extragalactic sources, while the figure at the bottom focuses on the Bulge region (boxed region in the figure at the top) and excludes extragalactic sources. Contours denote Galactic absorption levels of 10²¹, 5 $\times$ 10²¹, and 10²² cm^-2 (Dickey & Lockman 1990).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7091fg10.ps}\end{figure}$ Figure 10: Spin periods reported for sources detected by ISGRI that were previously known (92, clear histogram) and for IGRs (18, shaded histogram).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7091fg11.ps}\end{figure}$ Figure 11: Published orbital periods of sources detected by ISGRI. The clear histogram represents sources that were previously known (84) while the shaded histogram represents IGRs (14).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7091fg12.ps}\end{figure}$ Figure 12: Distribution of orbital periods of HMXBs (43, shaded histogram) compared with LMXBs and Miscellaneous sources (54, clear histogram).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7091fg13.ps}\end{figure}$ Figure 13: Corbet diagram of spin vs. orbital period of HMXBs detected by ISGRI whose companions are OB supergiants (17, filled circles) or Be stars (15, empty circles). IGRs are boxed.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{7091fg14.ps}\end{figure}$ Figure 14: Spin period as a function of reported $N_{{\rm H}}$ value (normalised by the expected Galactic value from (Dickey & Lockman 1990)) for HMXBs detected by ISGRI whose companions are OB supergiants (16, filled circles), Be stars (19, empty circles), or unclassified (2, crosses). IGRs are boxed and Magellanic Cloud sources are excluded.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{7091fg15.ps}\end{figure}$ Figure 15: Orbital period versus reported $N_{{\rm H}}$ value (normalised by the expected Galactic value from (Dickey & Lockman 1990)) for HMXBs detected by ISGRI whose companions are OB supergiants (20, filled circles), Be stars (15, empty circles) or unclassified (1, cross). IGRs are boxed and Magellanic Cloud sources are excluded.
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In the text

$\begin{figure} \par\includegraphics[width=6.45cm,clip]{7091fg16.ps}\end{figure}$ Figure 16: Distribution of reported $N_{{\rm H}}$ ( top), pulse periods ( middle), and orbital periods ( bottom) among HMXBs detected by ISGRI whose companions are OB supergiants (shaded histograms) or Be stars (clear histograms). Magellanic Cloud sources are excluded.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{7091fg02.ps}\end{figure}$	Figure 2: Galactic distribution of HMXBs (49, circles), LMXBs (74, squares), miscellaneous sources (37, triangles), and unclassified sources (3, inverted triangles). Filled symbols represent IGR sources. Also plotted is the 4-arm Galactic spiral model from Russeil (2003) with the Sun located at 8.5 kpc from the centre. The concentric circles indicate radii of 1, 3, 5,..., kpc from the centre.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{7091fg03.ps}\end{figure}$	Figure 3: Distribution of galactocentric distances of HMXBs (49, shaded histogram) and LMXBs (74, thick histogram). The dashed histogram represents OB star-forming complexes from Russeil (2003) (divided by 2).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{7091fg04.ps}\end{figure}$	Figure 4: Galactic distribution of HMXBs whose distance are known (49, star symbols) and the locations of star-forming complexes from Russeil (2003) (464, circles). The symbol size of the latter is proportional to the activity of the complex. HMXBs whose distances are unknown have been placed at 8.5 kpc (23, pentagons).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{7091fg05.ps}\end{figure}$	Figure 5: Histograms of Galactic longitudes integrated over the latitude for HMXBs with $\vert b\vert<6^{\circ }$ (shaded histogram) and star-forming regions from Russeil (2003) (thick histogram, divided by 3) and from Bronfman et al. (1996) (dashed histogram, divided by 10). The vertical lines indicate the tangential directions of the 4-arm spiral model from Russeil (2003).
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{7091fg07.ps}\end{figure}$	Figure 7: Vertical scale height (in kpc) from the Galactic plane of HMXBs, LMXBs and miscellaneous sources whose distances are known. The distributions have been summed over the northern and southern Galactic hemispheres. Sources from the Magellanic Clouds are excluded. The curves represent the exponential model described in the text fit to the data (see Table 3 for parameters).
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7091fg08.ps}\end{figure}$	Figure 8: The distribution of reported column densities ( $N_{{\rm H}}$ ) for Galactic sources (including sources in the Magellanic Clouds) detected by ISGRI that were previously known (152, clear histogram) and for IGRs (41, shaded histogram).
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7091fg10.ps}\end{figure}$	Figure 10: Spin periods reported for sources detected by ISGRI that were previously known (92, clear histogram) and for IGRs (18, shaded histogram).
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7091fg11.ps}\end{figure}$	Figure 11: Published orbital periods of sources detected by ISGRI. The clear histogram represents sources that were previously known (84) while the shaded histogram represents IGRs (14).
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7091fg12.ps}\end{figure}$	Figure 12: Distribution of orbital periods of HMXBs (43, shaded histogram) compared with LMXBs and Miscellaneous sources (54, clear histogram).
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7091fg13.ps}\end{figure}$	Figure 13: Corbet diagram of spin vs. orbital period of HMXBs detected by ISGRI whose companions are OB supergiants (17, filled circles) or Be stars (15, empty circles). IGRs are boxed.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{7091fg14.ps}\end{figure}$	Figure 14: Spin period as a function of reported $N_{{\rm H}}$ value (normalised by the expected Galactic value from (Dickey & Lockman 1990)) for HMXBs detected by ISGRI whose companions are OB supergiants (16, filled circles), Be stars (19, empty circles), or unclassified (2, crosses). IGRs are boxed and Magellanic Cloud sources are excluded.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{7091fg15.ps}\end{figure}$	Figure 15: Orbital period versus reported $N_{{\rm H}}$ value (normalised by the expected Galactic value from (Dickey & Lockman 1990)) for HMXBs detected by ISGRI whose companions are OB supergiants (20, filled circles), Be stars (15, empty circles) or unclassified (1, cross). IGRs are boxed and Magellanic Cloud sources are excluded.
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$\begin{figure} \par\includegraphics[width=6.45cm,clip]{7091fg16.ps}\end{figure}$	Figure 16: Distribution of reported $N_{{\rm H}}$ ( top), pulse periods ( middle), and orbital periods ( bottom) among HMXBs detected by ISGRI whose companions are OB supergiants (shaded histograms) or Be stars (clear histograms). Magellanic Cloud sources are excluded.
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