All Figures

$\begin{figure} \par\includegraphics[clip,width=8cm]{h4505_f1.eps} % \end{figure}$ Figure 1: Measured noise level in V filter (instrumental magnitudes) measured over seven nights from the NOT01 data set. The reductions were made with ISIS (Alard & Lupton 1998). The dashed lines mark the photon noise and the aperture noise while the solid line is the quadratic combination of these two.
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In the text

$\begin{figure} \par\hskip -0.5cm \includegraphics[clip,width=8cm]{h4505_f2.eps} \end{figure}$ Figure 2: The calibrated colour-magnitude diagram of NGC 6791. The inserted plot shows the turnoff region: notice the narrow main sequence and the binary sequence.
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In the text

$\begin{figure} \includegraphics[clip,width=8.3cm]{h4505_f3.eps} \end{figure}$ Figure 3: Colour-magnitude diagram of NGC 6791 with standard V and $V-I_{\rm c}$ magnitudes from Stetson et al. (2003). The transit candidates (triangles) and the eclipsing binaries (circles) are marked. The stars with the best photometry are also plotted to emphasize the location of the main sequence, the turnoff, and the red giant branch.
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In the text

$\begin{figure} \includegraphics[clip,width=17cm]{h4505_f4.eps} \end{figure}$ Figure 4: Light curves of transit candidates. Black and grey symbols are V and I measurements, respectively, and the noise level is given as $\sigma _V$ and $\sigma _I$ . The time t₀ in each panel corresponds to the time HJD-2 452 000 of the tick-mark at 0.0. Note that T6 has two transits-like events but of very different duration.
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In the text

$\begin{figure} \par\hskip -0.5cm \includegraphics[clip,width=8.1cm]{h4505_f5.eps} \end{figure}$ Figure 5: Colour-magnitude diagram of NGC 6791 with standard V and $V-I_{\rm c}$ magnitudes from Stetson et al. (2003). The 22 newly discovered variables have been marked. Only the stars with the best photometry are plotted to emphasize the location of the main sequence, the turnoff, and the red giant branch.
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In the text

$\begin{figure} \par\includegraphics[clip,width=15.6cm]{h4505_f6.eps} \end{figure}$ Figure 6: Phased light curves in the V filter for some of the known variables in NGC 6791. In most panels only the NOT01 data (+ symbols) are plotted due to the much lower noise level compared to MOCH01 (triangle symbols) and SMR95 (box symbols). Notice the change in the light curve of V4.
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In the text

$\begin{figure} \par\includegraphics[clip,width=15.6cm]{h4505_f7.eps} \end{figure}$ Figure 7: Phased light curves of some of the new low-amplitude variables. Only the NOT01 data are plotted. The ID number is given in the top left corner of each panel and correspond to Stetson et al. (2003). The period (in days) is given in the lower left corner. More details are given in Table 4.
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In the text

$\begin{figure} \par\mbox{\includegraphics[clip,width=8.6cm]{h4505f8a.eps} \includegraphics[clip,width=8.6cm]{h4505f8b.eps} } \end{figure}$ Figure 8: Phased light of the RS CV-type variable V9 in NGC 6791 in the V ( left plot) and I filter ( right plot). The black + symbols are data from NOT01 while the grey symbols are from either SMR95 (box symbol) or MOCH01 (filled grey symbols) The MOCH01 data are not plotted in the right plot since Mochejska et al. (2002) did not observe in I.
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In the text

$\begin{figure} \par\includegraphics[clip,width=8.8cm]{h4505f9a.eps} % \vskip 0.2... ... \includegraphics[clip,width=8.8cm]{h4505f9c.eps} % \vskip 0.15cm \end{figure}$ Figure 9: Light curves of three eclipsing binary stars. The time corresponding to 0.0 on the abscissa is HJD-2 452 000 and is given at the bottom of each panel as t₀. One or more nights without eclipses are shown for comparison. Black and grey symbols are V and I measurements, while the open circles are R measurements from MOCH01.
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In the text

$\begin{figure} \par\includegraphics[clip,width=7.6cm]{h4505f10.eps} %\end{figure}$ Figure 10: The I vs. V-I colour-magnitude diagram of NGC 6791 on the standard system. The location of the eclipsing binary V20 above the turnoff is shown with a star symbol. To find the possible positions of the two components of the binary V20, we assume that the primary star is on the solid black curve and calculate the corresponding colour and magnitude for the secondary component which is given as the dashed line. For three points we have shown the location of the primary and secondary star, i.e., for the primary star being at the turnoff (TO), further down the main sequence (MS), and the point where the dashed curve intersects the main sequence (Bin).
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In the text

$\begin{figure} \par\includegraphics[clip,width=8cm]{h4505_f1.eps} % \end{figure}$	Figure 1: Measured noise level in V filter (instrumental magnitudes) measured over seven nights from the NOT01 data set. The reductions were made with ISIS (Alard & Lupton 1998). The dashed lines mark the photon noise and the aperture noise while the solid line is the quadratic combination of these two.
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$\begin{figure} \par\hskip -0.5cm \includegraphics[clip,width=8cm]{h4505_f2.eps} \end{figure}$	Figure 2: The calibrated colour-magnitude diagram of NGC 6791. The inserted plot shows the turnoff region: notice the narrow main sequence and the binary sequence.
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$\begin{figure} \includegraphics[clip,width=8.3cm]{h4505_f3.eps} \end{figure}$	Figure 3: Colour-magnitude diagram of NGC 6791 with standard V and $V-I_{\rm c}$ magnitudes from Stetson et al. (2003). The transit candidates (triangles) and the eclipsing binaries (circles) are marked. The stars with the best photometry are also plotted to emphasize the location of the main sequence, the turnoff, and the red giant branch.
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$\begin{figure} \includegraphics[clip,width=17cm]{h4505_f4.eps} \end{figure}$	Figure 4: Light curves of transit candidates. Black and grey symbols are V and I measurements, respectively, and the noise level is given as $\sigma _V$ and $\sigma _I$ . The time t₀ in each panel corresponds to the time HJD-2 452 000 of the tick-mark at 0.0. Note that T6 has two transits-like events but of very different duration.
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$\begin{figure} \par\hskip -0.5cm \includegraphics[clip,width=8.1cm]{h4505_f5.eps} \end{figure}$	Figure 5: Colour-magnitude diagram of NGC 6791 with standard V and $V-I_{\rm c}$ magnitudes from Stetson et al. (2003). The 22 newly discovered variables have been marked. Only the stars with the best photometry are plotted to emphasize the location of the main sequence, the turnoff, and the red giant branch.
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$\begin{figure} \par\includegraphics[clip,width=15.6cm]{h4505_f6.eps} \end{figure}$	Figure 6: Phased light curves in the V filter for some of the known variables in NGC 6791. In most panels only the NOT01 data (+ symbols) are plotted due to the much lower noise level compared to MOCH01 (triangle symbols) and SMR95 (box symbols). Notice the change in the light curve of V4.
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$\begin{figure} \par\includegraphics[clip,width=15.6cm]{h4505_f7.eps} \end{figure}$	Figure 7: Phased light curves of some of the new low-amplitude variables. Only the NOT01 data are plotted. The ID number is given in the top left corner of each panel and correspond to Stetson et al. (2003). The period (in days) is given in the lower left corner. More details are given in Table 4.
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$\begin{figure} \par\mbox{\includegraphics[clip,width=8.6cm]{h4505f8a.eps} \includegraphics[clip,width=8.6cm]{h4505f8b.eps} } \end{figure}$	Figure 8: Phased light of the RS CV-type variable V9 in NGC 6791 in the V ( left plot) and I filter ( right plot). The black + symbols are data from NOT01 while the grey symbols are from either SMR95 (box symbol) or MOCH01 (filled grey symbols) The MOCH01 data are not plotted in the right plot since Mochejska et al. (2002) did not observe in I.
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$\begin{figure} \par\includegraphics[clip,width=8.8cm]{h4505f9a.eps} % \vskip 0.2... ... \includegraphics[clip,width=8.8cm]{h4505f9c.eps} % \vskip 0.15cm \end{figure}$	Figure 9: Light curves of three eclipsing binary stars. The time corresponding to 0.0 on the abscissa is HJD-2 452 000 and is given at the bottom of each panel as t₀. One or more nights without eclipses are shown for comparison. Black and grey symbols are V and I measurements, while the open circles are R measurements from MOCH01.
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