$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig03.ps} \end{figure}$ Figure 3: Microlensing optical depth towards the LMC as a function of the limiting magnitude for several IMFs.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig04.ps} \end{figure}$ Figure 4: Distribution of Einstein crossing times for the microlensing events towards the LMC of the 40 independent realizations of the simulated population (solid lines) for several IMFs, and of the observational data (dashed lines).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig05.ps} \end{figure}$ Figure 5: Distribution of the whole white dwarf population - solid lines - and of the white dwarfs responsible for microlensing events towards the LMC - dashed lines - as a function of their visual magnitude for several IMFs.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig06.ps} \end{figure}$ Figure 6: Theoretical color-magnitude diagram of a typical Monte Carlo realization of the HDF for several IMFs.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig07.ps} \end{figure}$ Figure 7: Simulation of the HDF. The box represents the observational selection criteria of Ibata et al. (1999).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0541fig09.ps} \end{figure}$ Figure 9: The halo white dwarf luminosity function obtained when assuming that all the reported microlensing optical depth is due to lenses in the form of white dwarfs - solid line - compared to the observation luminosity functions of the disk - top dotted line - and of the halo - bottom dotted line.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0541fig10.ps} \end{figure}$ Figure 10: The density profiles used in the simulations. The top panel shows the density profiles from the center of the Galaxy, whereas the bottom panel shows the density profiles towards the direction of the LMC.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig01.ps} \end{figure}$	Figure 1: Luminosity function of halo white dwarfs for several limiting magnitudes.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig02.ps} \end{figure}$	Figure 2: Luminosity function of halo white dwarfs for several IMFs.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig03.ps} \end{figure}$	Figure 3: Microlensing optical depth towards the LMC as a function of the limiting magnitude for several IMFs.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig04.ps} \end{figure}$	Figure 4: Distribution of Einstein crossing times for the microlensing events towards the LMC of the 40 independent realizations of the simulated population (solid lines) for several IMFs, and of the observational data (dashed lines).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig05.ps} \end{figure}$	Figure 5: Distribution of the whole white dwarf population - solid lines - and of the white dwarfs responsible for microlensing events towards the LMC - dashed lines - as a function of their visual magnitude for several IMFs.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig06.ps} \end{figure}$	Figure 6: Theoretical color-magnitude diagram of a typical Monte Carlo realization of the HDF for several IMFs.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig07.ps} \end{figure}$	Figure 7: Simulation of the HDF. The box represents the observational selection criteria of Ibata et al. (1999).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0541fig08.ps} \end{figure}$	Figure 8: Simulation of the EROS results. See text for a detailed description.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0541fig09.ps} \end{figure}$	Figure 9: The halo white dwarf luminosity function obtained when assuming that all the reported microlensing optical depth is due to lenses in the form of white dwarfs - solid line - compared to the observation luminosity functions of the disk - top dotted line - and of the halo - bottom dotted line.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0541fig10.ps} \end{figure}$	Figure 10: The density profiles used in the simulations. The top panel shows the density profiles from the center of the Galaxy, whereas the bottom panel shows the density profiles towards the direction of the LMC.
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