$\begin{figure} \par\includegraphics[width=7cm,clip]{9805fig01.eps}\end{figure}$ Figure 1: Microlensing optical depth towards the LMC as a function of the limiting magnitude. Solid and open squares represent the CO and ONe white-dwarf populations, respectively. Red dwarfs are represented using open triangles, while the entire population is shown using open circles.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{9805fig03.eps}\end{figure}$ Figure 3: Fraction of microlenses with respect to the entire population, as a function of the magnitude cut.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{9805fig04.eps}\end{figure}$ Figure 4: Differential event rate normalized to unit area as a function of the Einstein crossing-time for the populations under study and different magnitude cuts (solid lines). The observational event distribution from Alcock et al. (2000) is represented as a dotted line in each panel.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9805fig05.eps}\end{figure}$ Figure 5: Halo dark-matter fraction as a function of the mass lens. We plot, using a solid line, the $95\%$ confidence-level curve for the MACHO experiment and the $95\%$ confidence-level upper-limit for the EROS experiment.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{9805fig01.eps}\end{figure}$	Figure 1: Microlensing optical depth towards the LMC as a function of the limiting magnitude. Solid and open squares represent the CO and ONe white-dwarf populations, respectively. Red dwarfs are represented using open triangles, while the entire population is shown using open circles.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{9805fig02.eps}\end{figure}$	Figure 2: Contribution to the optical depth as a function of lens mass.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{9805fig03.eps}\end{figure}$	Figure 3: Fraction of microlenses with respect to the entire population, as a function of the magnitude cut.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{9805fig04.eps}\end{figure}$	Figure 4: Differential event rate normalized to unit area as a function of the Einstein crossing-time for the populations under study and different magnitude cuts (solid lines). The observational event distribution from Alcock et al. (2000) is represented as a dotted line in each panel.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{9805fig05.eps}\end{figure}$	Figure 5: Halo dark-matter fraction as a function of the mass lens. We plot, using a solid line, the $95\%$ confidence-level curve for the MACHO experiment and the $95\%$ confidence-level upper-limit for the EROS experiment.
Open with DEXTER