All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{5149f1} \end{figure}$ Figure 1: Scheme of a section of the microlensing tube with indicated the positions of the vectors and the angles involved.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5149f2} \end{figure}$ Figure 2: Normalised differential rate $({\rm d}\Gamma /{\rm d}T_{\rm E})_\varepsilon$ for both MW and LMC halos for 0.2 and 0.5 $M_\odot$ , dashed and solid lines, respectively. Superimposed is the value of the observed durations. The y-axis values are in 10^-2 units.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5149f3} \end{figure}$ Figure 3: Kolmogorov-Smirnov and $\alpha$ coefficients as a function of the MACHO mass, with $\alpha$ the ratio of the MW over the total number of dark matter halo events.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5149f4} \end{figure}$ Figure 4: Normalised expected number profiles along the axis, pointing south-west, orthogonal to the line of nodes and passing through the LMC centre, for different lens populations: self lensing, dot dashed line; MW MACHO, solid line; LMC MACHO, dashed line. Values on the $\xi$ axis are in kpc.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5149f5} \end{figure}$ Figure 5: Location of the 30 MACHO fields in a reference frame centred in the LMC centre with the x-axis antiparallel to the right ascension, the y-axis parallel to the declination, and the z-axis (not shown) pointing towards the observer. The location of the 13 microlensing candidates, a subset of the original set B of MACHO candidates that we use in thepresent analysis (Sect. 4.1), is shown. Also shown is the position of the line of nodes and the central band around it, which we exclude inthe asymmetry analysis.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=5.7cm,clip]{5149f6a}\includegrap... ...cm,clip]{5149f6c}\includegraphics[width=5.7cm,clip]{5149f6d} } \par \end{figure}$ Figure 6: Probability isocontours with 34%, 68% and 90% regions for the LMC and MW dark matter halo fraction for four values of the MACHO mass.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5149f7} \end{figure}$ Figure 7: MW and LMC dark matter halo fraction, median value with 68% CL errors, as a function of the MACHO mass.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5149f1} \end{figure}$	Figure 1: Scheme of a section of the microlensing tube with indicated the positions of the vectors and the angles involved.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5149f2} \end{figure}$	Figure 2: Normalised differential rate $({\rm d}\Gamma /{\rm d}T_{\rm E})_\varepsilon$ for both MW and LMC halos for 0.2 and 0.5 $M_\odot$ , dashed and solid lines, respectively. Superimposed is the value of the observed durations. The y-axis values are in 10^-2 units.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5149f3} \end{figure}$	Figure 3: Kolmogorov-Smirnov and $\alpha$ coefficients as a function of the MACHO mass, with $\alpha$ the ratio of the MW over the total number of dark matter halo events.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5149f4} \end{figure}$	Figure 4: Normalised expected number profiles along the axis, pointing south-west, orthogonal to the line of nodes and passing through the LMC centre, for different lens populations: self lensing, dot dashed line; MW MACHO, solid line; LMC MACHO, dashed line. Values on the $\xi$ axis are in kpc.
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$\begin{figure} \par\mbox{\includegraphics[width=5.7cm,clip]{5149f6a}\includegrap... ...cm,clip]{5149f6c}\includegraphics[width=5.7cm,clip]{5149f6d} } \par \end{figure}$	Figure 6: Probability isocontours with 34%, 68% and 90% regions for the LMC and MW dark matter halo fraction for four values of the MACHO mass.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5149f7} \end{figure}$	Figure 7: MW and LMC dark matter halo fraction, median value with 68% CL errors, as a function of the MACHO mass.
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