All Figures

$\begin{figure} \center \includegraphics[width=14.5cm]{6199fg1.eps}\end{figure}$ Figure 1: Comparison of the photometric precision for aperture photometry with neighbor subtraction (Ap) and for PSF fitting photometry (PSF) as a function of the apparent visual magnitude for CFHT, SPM, Loiano and NOT images. The short dashed line indicates the N/S considering only the star photon noise, the long dashed line is the N/S due to the sky photon noise and the detector noise. The continuous line is the total N/S.
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In the text

$\begin{figure} \par\includegraphics[width=15cm]{6199fg2.eps}\end{figure}$ Figure 2: Comparison of the photometric precision for image subtraction (ISIS) and for psf fitting photometry (PSF) as function of the apparent visual magnitude for CFHT, SPM, Loiano, and NOT images.
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In the text

$\begin{figure} \center \includegraphics[width=15cm]{6199fg3.eps}\end{figure}$ Figure 3: The expected rms noise for the observations taken at the different sites as a function of the visual apparent magnitude, is compared with the rms of the observed light curves obtained with the image subtraction technique.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{6199fg4.eps}\end{figure}$ Figure 4: rms noise for the San Pedro Mártir observations with the aperture error (triangles) as estimated by Eq. (3).
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{6199fg5.eps}\end{figure}$ Figure 5: The NGC 6791 CMD highlighting the selection region of the main sequence stars (blue circles).
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm]{6199fg6.eps}\end{figure}$ Figure 6: False Alarm Probability (FAR) in %, against the DSP parameter given by the algorithm. The points indicate the results of our simulations on constant light curves, the solid line is our assumed best fit.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{6199fg7.eps}\end{figure}$ Figure 7: CMD diagram of NGC6791 with the best fit Z=0.030 isochrone (dashed line), and the best fit Z=0.046 isochrone (from Carraro et al. 2006, solid line). Photometry: Stetson et al. (2003)
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In the text

$\begin{figure} \par\includegraphics[width=4.4cm]{6199fg8a.eps}\includegraphics[width=4.4cm]{6199fg8b.eps}\end{figure}$ Figure 8: Left: $M_{i}/M_{\odot }$ vs. visual apparent magnitude. Right: $R_{i}/R_{\odot }$ vs. visual apparent magnitude, from our best fit isochrone (dashed line) and from the Z=0.046 isochrone (solid line) applied to the stars of NGC 6791.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{6199fg9.eps}\end{figure}$ Figure 9: Continuous line: adopted distribution for planet periods. Histogram: RV surveys data (from the Extrasolar Planets Encyclopaedia).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{6199fg10.eps}\end{figure}$ Figure 10: Top: constant light curve. Bottom: the same light curve after inserting the simulated transit with limb-darkening (black points). The solid line shows the theoretical light curve of the transit.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm]{6199fg11.eps}\end{figure}$ Figure 11: TDE as a function of the stellar magnitude for various assumptions on planetary radii distribution. From the top to the bottom: 1) Dashed line, $R=(1.4~\pm~0.1)~R_{\rm J}$ ; 2) Solid line, $R=(1.0~\pm~0.2)~R_{\rm J}$ ; 3) Dotted line, $R=(0.7~\pm~0.1)~R_{\rm J}$ . The adopted threshold for the DSP in this figure is 4.3. The normalization is respect to the whole number of transiting planets.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{6199fg12.eps} \end{figure}$ Figure 12: ( Upper left) Distributions of transit depths measured by the BLS algorithm on the artificial constant-light-curves (lc); ( upper right) transit depths measured on artificial light curves with transits added; ( lower left) input transit depths used to generate artificial light curves with transits; ( lower right) relative difference between the transit depth recovered by BLS and its input value. Empty histograms refer to distributions relative to all light curves, filled ones to light curves with totally and partially recovered transits. Histograms are normalized to all light curves with transiting planets, or, for the upper left panel to all constant light curves. This figure is relative to CFHT data, and the assumed planetary radii distribution is $R=(1.0~\pm~0.2)$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{6199fg13.eps}\end{figure}$ Figure 13: The same as Fig. 12 for the transit periods.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{6199fg14.eps}\end{figure}$ Figure 14: The same as Fig.12 for the transit durations.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{6199fg15.eps}\end{figure}$ Figure 15: Composite light curve of candidate 6598. In ordinate is reported the calibrated V magnitude and in abscissa the observing epoch, (in days), where 0 corresponds to ${\rm JD}=52099$ . Filled circles indicate CFHT data, crosses SPM data, open triangles Loiano data, open circles NOT data in the V filter and open squares NOT data in the I filter. Light blue symbols highlight regions which were flagged by the BLS.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm]{6199fg16.eps}\end{figure}$ Figure 16: Composite light curve of candidate 4304.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm]{6199fg17.eps}\end{figure}$ Figure 17: Composite light curve of candidate 4699.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm]{6199fg18.eps}\end{figure}$ Figure 18: CFHT light curve for candidate 1239.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{6199fg19.eps}\end{figure}$ Figure 19: CFHT light curve for candidate 4300.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{6199fg20.eps}\end{figure}$ Figure 20: CFHT light curve for candidate 7591.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{6199fg21.eps}\end{figure}$ Figure 21: Composite light curve for candidate 3671 correspondent to T5 of BO3. Different symbols have the same meaning of Fig. 15.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{6199fg22.eps}\end{figure}$ Figure 22: Composite light curve for candidate 3723 correspondent to T7 of BO3.
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In the text

$\begin{figure} \center \includegraphics[width=7.5cm]{6199fg23.eps}\end{figure}$ Figure 23: Composite light curve for candidate 12390 correspondent to T9 of BO3.
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In the text

$\begin{figure} \par\includegraphics[width=15cm]{6199fg2.eps}\end{figure}$	Figure 2: Comparison of the photometric precision for image subtraction (ISIS) and for psf fitting photometry (PSF) as function of the apparent visual magnitude for CFHT, SPM, Loiano, and NOT images.
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$\begin{figure} \center \includegraphics[width=15cm]{6199fg3.eps}\end{figure}$	Figure 3: The expected rms noise for the observations taken at the different sites as a function of the visual apparent magnitude, is compared with the rms of the observed light curves obtained with the image subtraction technique.
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$\begin{figure} \par\includegraphics[width=8cm]{6199fg4.eps}\end{figure}$	Figure 4: rms noise for the San Pedro Mártir observations with the aperture error (triangles) as estimated by Eq. (3).
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$\begin{figure} \par\includegraphics[width=8cm]{6199fg5.eps}\end{figure}$	Figure 5: The NGC 6791 CMD highlighting the selection region of the main sequence stars (blue circles).
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$\begin{figure} \par\includegraphics[width=7.2cm]{6199fg6.eps}\end{figure}$	Figure 6: False Alarm Probability (FAR) in %, against the DSP parameter given by the algorithm. The points indicate the results of our simulations on constant light curves, the solid line is our assumed best fit.
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$\begin{figure} \par\includegraphics[width=8.8cm]{6199fg7.eps}\end{figure}$	Figure 7: CMD diagram of NGC6791 with the best fit Z=0.030 isochrone (dashed line), and the best fit Z=0.046 isochrone (from Carraro et al. 2006, solid line). Photometry: Stetson et al. (2003)
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$\begin{figure} \par\includegraphics[width=4.4cm]{6199fg8a.eps}\includegraphics[width=4.4cm]{6199fg8b.eps}\end{figure}$	Figure 8: Left: $M_{i}/M_{\odot }$ vs. visual apparent magnitude. Right: $R_{i}/R_{\odot }$ vs. visual apparent magnitude, from our best fit isochrone (dashed line) and from the Z=0.046 isochrone (solid line) applied to the stars of NGC 6791.
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$\begin{figure} \par\includegraphics[width=8.8cm]{6199fg9.eps}\end{figure}$	Figure 9: Continuous line: adopted distribution for planet periods. Histogram: RV surveys data (from the Extrasolar Planets Encyclopaedia).
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$\begin{figure} \par\includegraphics[width=8.8cm]{6199fg10.eps}\end{figure}$	Figure 10: Top: constant light curve. Bottom: the same light curve after inserting the simulated transit with limb-darkening (black points). The solid line shows the theoretical light curve of the transit.
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$\begin{figure} \par\includegraphics[width=8cm]{6199fg13.eps}\end{figure}$	Figure 13: The same as Fig. 12 for the transit periods.
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$\begin{figure} \par\includegraphics[width=8cm]{6199fg14.eps}\end{figure}$	Figure 14: The same as Fig.12 for the transit durations.
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$\begin{figure} \par\includegraphics[width=7.1cm]{6199fg16.eps}\end{figure}$	Figure 16: Composite light curve of candidate 4304.
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$\begin{figure} \par\includegraphics[width=7.1cm]{6199fg17.eps}\end{figure}$	Figure 17: Composite light curve of candidate 4699.
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$\begin{figure} \par\includegraphics[width=7.1cm]{6199fg18.eps}\end{figure}$	Figure 18: CFHT light curve for candidate 1239.
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$\begin{figure} \par\includegraphics[width=7.5cm]{6199fg19.eps}\end{figure}$	Figure 19: CFHT light curve for candidate 4300.
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$\begin{figure} \par\includegraphics[width=7.5cm]{6199fg20.eps}\end{figure}$	Figure 20: CFHT light curve for candidate 7591.
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$\begin{figure} \par\includegraphics[width=7.5cm]{6199fg21.eps}\end{figure}$	Figure 21: Composite light curve for candidate 3671 correspondent to T5 of BO3. Different symbols have the same meaning of Fig. 15.
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$\begin{figure} \par\includegraphics[width=7.5cm]{6199fg22.eps}\end{figure}$	Figure 22: Composite light curve for candidate 3723 correspondent to T7 of BO3.
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$\begin{figure} \center \includegraphics[width=7.5cm]{6199fg23.eps}\end{figure}$	Figure 23: Composite light curve for candidate 12390 correspondent to T9 of BO3.
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