All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{7075fig1}\end{figure}$ Figure 1: Projected on M 31, we display the boundaries of the two 13' $\times$ 12.6'monitored fields (inner contours), together with the larger INT fields and the centre M 31 (cross). The filled circle marks the position of the Nova variable detected (Sect. 3.3).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{7075fig2}\end{figure}$ Figure 2: $R(\Delta \phi )$ vs. period for short-period ( $P < 30~{\rm d}$ ) variable stars reported in the POINT-AGAPE catalogue (top panel shows the subset with $\log(L_f)<-30$ ), where filled circles indicate the flux variations identified within the OAB data set.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7075fig3}\end{figure}$ Figure 3: The light curve of a POINT-AGAPE flux variation (P=11.14 days and $R(\Delta \phi )=21.1$ ), together with its extension in the OAB data. Top to bottom, the INT R and color light curves, folded by their period (for visual aid, two cycles are plotted); and the OAB R and color light curves. The "color'' is evaluated as $-2.5 \log(\phi_r/\phi_i)$ , where $\phi$ is the observed flux. Flux is in ADU s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{7075fig4}\end{figure}$ Figure 4: The light curve of the POINT-AGAPE PA-S3 microlensing candidate (Paulin-Henriksson et al. 2003; Calchi Novati et al. 2005) together with its extension in the OAB data. In the INT data the dotted line is the best Paczynski (1986) fit; in the OAB data, the solid lines indicate the background level, while the dotted lines represent the flux deviation corresponding to the observed flux deviation at maximum for the POINT-AGAPE variation. The ordinate axis units are flux in ADU s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{7075fig5}\end{figure}$ Figure 5: The light curve of the Nova detected within the OAB data. Top to bottom, R, I bands and color data (as defined in Fig. 3) are shown. The solid lines (R and I data) indicate the estimate of the background level.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7075fig6}\end{figure}$ Figure 6: Results of the Monte Carlo simulation: from top to bottom we show the histograms of the expected flux deviation at maximum, duration distribution for self-lensing events, and the distance (from the M 31 center) distributions for self-lensing and for MACHOs. The units on the ordinate axes are the number of events.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{7075fig1}\end{figure}$	Figure 1: Projected on M 31, we display the boundaries of the two 13' $\times$ 12.6'monitored fields (inner contours), together with the larger INT fields and the centre M 31 (cross). The filled circle marks the position of the Nova variable detected (Sect. 3.3).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{7075fig2}\end{figure}$	Figure 2: $R(\Delta \phi )$ vs. period for short-period ( $P < 30~{\rm d}$ ) variable stars reported in the POINT-AGAPE catalogue (top panel shows the subset with $\log(L_f)<-30$ ), where filled circles indicate the flux variations identified within the OAB data set.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{7075fig5}\end{figure}$	Figure 5: The light curve of the Nova detected within the OAB data. Top to bottom, R, I bands and color data (as defined in Fig. 3) are shown. The solid lines (R and I data) indicate the estimate of the background level.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7075fig6}\end{figure}$	Figure 6: Results of the Monte Carlo simulation: from top to bottom we show the histograms of the expected flux deviation at maximum, duration distribution for self-lensing events, and the distance (from the M 31 center) distributions for self-lensing and for MACHOs. The units on the ordinate axes are the number of events.
Open with DEXTER