All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1074fig1.ps}\end{figure}$ Figure 1: Far-infrared (IRAS, $100\mu$ ) map of the $10\hbox {$^\circ $ }\times 10\hbox {$^\circ $ }$ region around the Large Magellanic Cloud. Circles show fields of view of the XMM-Newton observations used for the analysis.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1074fig2.ps}\end{figure}$ Figure 2: The survey area as a function of 2-10 keV flux, calculated as described in Sect. 2.3.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1074fig3.ps}\end{figure}$ Figure 3: Cumulative $\log(N){-}\log(S)$ distribution of detected point-like sources, excluding several known foreground stars and rotation powered pulsars (Sect. 3). The thin and thick histograms show, respectively, the observed distribution and the distribution corrected for the incompleteness effects, as described in Sect. 2.3. The thick grey line shows the $\log(N){-}\log(S)$ of CXB sources according to Moretti et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1074f4r.ps}\hspace*{4mm} \includegraphics[width=7.5cm,clip]{1074f4d.ps}\end{figure}$ Figure 4: Left: ratio of the actual number of matches between the X-ray source list and USNO-B catalog to the the expected number of chance coincidences, as a function of the search radius. Right: difference between the number of matches and the expected number of chance coincidences. The vertical dashed line in both panels shows the search radius of 3.6 arcsec. The shaded area indicates the Poisson uncertainty, computed from the square root of the actual number of matches.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1074fig5.ps}\end{figure}$ Figure 5: The incompleteness-corrected XLF of HMXB candidates in LMC. The upper histogram shows all sources from Table 3, except two in the 30 Dor region; the lower one shows likely HMXB candidates (upper part of Table 3). These two histograms provide upper and lower limits for the true HMXB XLF. The upper grey line and shaded area show the luminosity distribution predicted from the "universal'' XLF of Grimm et al. (2003) extrapolated towards low luminosities and its uncertainty. The lower solid and dashed lines show the same XLF modified by the "propeller effect'' assuming the black hole fraction of $f_{\rm BH}=0$ and $f_{\rm BH}=0.3$ respectively (Sect. 6).
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In the text

$\begin{figure} \par\hbox{ \includegraphics[width=8cm,clip]{1074fig6.ps} } \end{figure}$ Figure 6: Cumulative $\log N{-}\log S$ distribution of CXB sources, obtained after removal of HMXB candidates. The solid line shows the distribution from Moretti et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1074f7p.ps}\hspace*{4mm} \includegraphics[width=8cm,clip]{1074f7h.ps}\end{figure}$ Figure 7: Distribution of spin periods ( left) and magnetic field strength ( right, Coburn et al. 2002) in high mass X-ray binaries. The spin period distributions are shown separately for the Milky Way (Liu et al. 2000) and SMC (Corbet et al. 2004) sources. The SMC distribution is shifted along the x axis by 0.2 dex for clarity. The smooth solid lines in both panels show the model distributions used for calculation of the propeller effect.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1074fig8.ps}\end{figure}$ Figure 8: Impact of the propeller effect on the luminosity distribution of high mass X-ray binaries with a neutron star primary. The straight line shows the initial power law distribution with differential slope 1.6. The curved lines show the luminosity function modified by the propeller effect for different parameters of the distributions of the neutron star spin and magnetic field. The neutron star mass and radius are $M_{\rm NS}=1.4~M_\odot$ and $R_{\rm NS}=13$ km. The dashed line corresponds to our sensitivity limit.
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In the text

$\begin{figure} {\hbox{ \includegraphics[width=7.5cm,clip]{1074fig9.ps} }} \end{figure}$ Figure 9: The $H_{\alpha }$ map of LMC (greyscale image). The overlayed symbols are: "+''(magenta) - all known HMXBs from the catalog of Liu et al. (2000) and HMXB candidates discovered by ROSAT (Kahabka 2002); "x'' (blue) - likely HMXB candidates (upper part of Table 3). Large circles indicate fields of view of XMM observations. The oval-shaped region in the north-east shows the location of the LMC 4 supergiant shell. The region of the highest surface brightness, located to the south of Dec $=-69\hbox {$^\circ $ }$ , is the 30 Doradus HII region.
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In the text

$\begin{figure} \par\hbox{ \includegraphics[width=8cm,clip]{1074f10.ps} } \end{figure}$ Figure 10: The time dependence of the specific number of HMXBs, $\eta _{\rm HMXB}(\tau )$ . The point with error bars and the upper limit are data on the LMC 4 supergiant shell and R136 star cluster (Table 4). The solid line shows the simple model described in Sect. 7.3 with the normalization determined from the $N_{\rm HMXB}-$ SFR relation from Grimm et al. (2003).
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In the text

$\begin{figure} \par\hbox{ \includegraphics[width=8cm,clip]{1074f11.ps} } \end{figure}$ Figure 11: The $\log(N){-}\log(S)$ distribution of X-ray sources in the LMC field. The different histograms show the distribution of all sources, high mass X-ray binaries and CXB sources. The shaded area in the distribution of HMXBs corresponds to the range of uncertainties discussed in Sect. 5.1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1074fig1.ps}\end{figure}$	Figure 1: Far-infrared (IRAS, $100\mu$ ) map of the $10\hbox {$^\circ $ }\times 10\hbox {$^\circ $ }$ region around the Large Magellanic Cloud. Circles show fields of view of the XMM-Newton observations used for the analysis.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1074fig2.ps}\end{figure}$	Figure 2: The survey area as a function of 2-10 keV flux, calculated as described in Sect. 2.3.
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$\begin{figure} \par\hbox{ \includegraphics[width=8cm,clip]{1074fig6.ps} } \end{figure}$	Figure 6: Cumulative $\log N{-}\log S$ distribution of CXB sources, obtained after removal of HMXB candidates. The solid line shows the distribution from Moretti et al. (2003).
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$\begin{figure} \par\hbox{ \includegraphics[width=8cm,clip]{1074f10.ps} } \end{figure}$	Figure 10: The time dependence of the specific number of HMXBs, $\eta _{\rm HMXB}(\tau )$ . The point with error bars and the upper limit are data on the LMC 4 supergiant shell and R136 star cluster (Table 4). The solid line shows the simple model described in Sect. 7.3 with the normalization determined from the $N_{\rm HMXB}-$ SFR relation from Grimm et al. (2003).
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$\begin{figure} \par\hbox{ \includegraphics[width=8cm,clip]{1074f11.ps} } \end{figure}$	Figure 11: The $\log(N){-}\log(S)$ distribution of X-ray sources in the LMC field. The different histograms show the distribution of all sources, high mass X-ray binaries and CXB sources. The shaded area in the distribution of HMXBs corresponds to the range of uncertainties discussed in Sect. 5.1.
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