All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1355fig1.eps}\end{figure}$ Figure 1: The mean impact parameter maps $\langle u_{\rm T}(x,y) \rangle _{\phi}$ and $\langle u_{\rm T}^{~2}(x,y) \rangle _{\phi}$ towards M 31 are given, for selected directions towards M 31 corresponding to different (x,y)coordinates (in units of arcmin) centered on M 31 and aligned along the major and minor axes of the projected light profile.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1355fig2.eps}\end{figure}$ Figure 2: The mean impact parameter $\langle u_{\rm T}(x,y) \rangle _{\phi}$ is given as a function of the background photon counts $N_{\rm sky}$ in a pixel, for selected directions towards M 31 corresponding to different (x,y)coordinates (in units of arcmin) in the sky plane. Thin lines, from the bottom to the upper part of the figure, refer to (8,0), (16,0) and (32,0); thick lines are for (0,-2), (0,-4) and (0,-8) coordinates, respectively.
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In the text

$\begin{figure} \par$\begin{array}{c@{\hspace{0.4in}}c} \epsfxsize=3.25in \epsfys... ...3b.eps}\\ [0.cm] \mbox{\bf a)} & \mbox{\bf b)} \end{array}$\par \par\end{figure}$ Figure 3: Mean optical depth $\langle \tau_{\rm c}(x,y)\rangle$ maps (in units of 10^-6) towards M 31 are given for selected source and lens populations. The first index refers to the source stars (1 for M 31 bulge, 2 for M 31 disk) while the second one refers to the lens populations (1 and 2 as above, 3 for MACHOs in the M 31 halo). Optical depth maps for lenses belonging to the MW disk and halo populations are not given since the obtained results are almost constant in any direction.
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In the text

$\begin{figure} \par$\begin{array}{c@{\hspace{0.4in}}c} \epsfxsize=3.25in \epsfys... ...55fig4b.eps}\\ [0.cm] \mbox{\bf a)} & \mbox{\bf b)} \end{array}$\par\end{figure}$ Figure 4: In panel a), the mean classical optical depth $\langle \tau_{\rm c}(x,y)\rangle$ maps (in units of 10^-6) towards M 31 are given for self, dark and total lensing. In panel b), the mean pixel lensing optical depth $\langle \tau_{\rm p}(x,y)\rangle$ maps are given, in the same cases.
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In the text

$\begin{figure} \par$\begin{array}{c@{\hspace{0.4in}}c} \epsfxsize=3.25in \epsfys... ...55fig5b.eps}\\ [0.cm] \mbox{\bf a)} & \mbox{\bf b)} \end{array}$\par\end{figure}$ Figure 5: In panel a), the instantaneous pixel lensing event number density $\langle IE_{\rm p}(x,y) \rangle$ maps (events per arcmin²) towards M 31 are given for self, dark and total lensing. In panel b) maps of pixel lensing event rate $\langle E_{\rm p}(x,y)\rangle$ (events per year and per arcmin²) are given, in the same cases.
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In the text

$\begin{figure} \par$\begin{array}{c@{\hspace{0.4in}}c} \epsfxsize=3.25in \epsfys... ...55fig6b.eps}\\ [0.cm] \mbox{\bf a)} & \mbox{\bf b)} \end{array}$\par\end{figure}$ Figure 6: In panel a), mean classical event duration time $\langle t_{\rm c}(x,y)\rangle$ (in days) maps towards M 31 are given for self, dark and total lensing. In panel b) for pixel lensing, maps of $\langle t_{\rm p}(x,y) \rangle$ are given, in the same cases.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1355fig7.eps}\end{figure}$ Figure 7: The projected (along the xaxis) mean event number $\langle E_{\rm p}(y) \rangle _x$ is given as a function of the coordinate y for the Reference model. The dashed line refers to dark lensing events by MACHOs in M 31 and MW halos while the solid line is for self-lensing events by stars in M 31 bulge and disk.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1355fig8.eps}\end{figure}$ Figure 8: The pixel lensing event duration $\langle t_{\rm p}(y) \rangle _x$ averaged along the xdirection is given as a function of the y coordinate. The dashed line refers to dark lensing events by MACHOs in M 31 and MW halos while the solid line is for self-lensing events by stars in M 31 bulge and disk.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1355fig1.eps}\end{figure}$	Figure 1: The mean impact parameter maps $\langle u_{\rm T}(x,y) \rangle _{\phi}$ and $\langle u_{\rm T}^{~2}(x,y) \rangle _{\phi}$ towards M 31 are given, for selected directions towards M 31 corresponding to different (x,y)coordinates (in units of arcmin) centered on M 31 and aligned along the major and minor axes of the projected light profile.
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$\begin{figure} \par$\begin{array}{c@{\hspace{0.4in}}c} \epsfxsize=3.25in \epsfys... ...55fig4b.eps}\\ [0.cm] \mbox{\bf a)} & \mbox{\bf b)} \end{array}$\par\end{figure}$	Figure 4: In panel a), the mean classical optical depth $\langle \tau_{\rm c}(x,y)\rangle$ maps (in units of 10^-6) towards M 31 are given for self, dark and total lensing. In panel b), the mean pixel lensing optical depth $\langle \tau_{\rm p}(x,y)\rangle$ maps are given, in the same cases.
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$\begin{figure} \par$\begin{array}{c@{\hspace{0.4in}}c} \epsfxsize=3.25in \epsfys... ...55fig5b.eps}\\ [0.cm] \mbox{\bf a)} & \mbox{\bf b)} \end{array}$\par\end{figure}$	Figure 5: In panel a), the instantaneous pixel lensing event number density $\langle IE_{\rm p}(x,y) \rangle$ maps (events per arcmin²) towards M 31 are given for self, dark and total lensing. In panel b) maps of pixel lensing event rate $\langle E_{\rm p}(x,y)\rangle$ (events per year and per arcmin²) are given, in the same cases.
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$\begin{figure} \par$\begin{array}{c@{\hspace{0.4in}}c} \epsfxsize=3.25in \epsfys... ...55fig6b.eps}\\ [0.cm] \mbox{\bf a)} & \mbox{\bf b)} \end{array}$\par\end{figure}$	Figure 6: In panel a), mean classical event duration time $\langle t_{\rm c}(x,y)\rangle$ (in days) maps towards M 31 are given for self, dark and total lensing. In panel b) for pixel lensing, maps of $\langle t_{\rm p}(x,y) \rangle$ are given, in the same cases.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1355fig7.eps}\end{figure}$	Figure 7: The projected (along the xaxis) mean event number $\langle E_{\rm p}(y) \rangle _x$ is given as a function of the coordinate y for the Reference model. The dashed line refers to dark lensing events by MACHOs in M 31 and MW halos while the solid line is for self-lensing events by stars in M 31 bulge and disk.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1355fig8.eps}\end{figure}$	Figure 8: The pixel lensing event duration $\langle t_{\rm p}(y) \rangle _x$ averaged along the xdirection is given as a function of the y coordinate. The dashed line refers to dark lensing events by MACHOs in M 31 and MW halos while the solid line is for self-lensing events by stars in M 31 bulge and disk.
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