$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig1.eps} \end{figure}$ Figure 1: Finding chart for QW Ser covering a region of $6.5 \times 6.5$ arcmin. The position of the comparison star is shown. North is up, East is left.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{fig2.eps} \end{figure}$ Figure 2: The general photometric behavior of QW Ser during its 2003 superoutburst. Visual estimates collected in the VSNET archive are shown as open circles and CCD observations described in this paper as dots.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig4.eps} \end{figure}$ Figure 4: The light curves of QW Ser observed during the eight longest runs from period Mar. 07/08-May 04/05.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig5.eps} \end{figure}$ Figure 5: ANOVA power spectrum of the light curve of QW Ser. The inset shows the magnification of the power spectrum around main frequency.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig6.eps} \end{figure}$ Figure 6: ANOVA power spectrum of the light curve of QW Ser from the period Mar. 07/08 - May 04/05.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig7.eps} \end{figure}$ Figure 7: Stolz & Schoembs relation for 44 ordinary SU UMa stars (open circles) and 10 stars other than dwarf novae (filled circles). The position of QW Ser is denoted by the solid triangle.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig1.eps} \end{figure}$	Figure 1: Finding chart for QW Ser covering a region of $6.5 \times 6.5$ arcmin. The position of the comparison star is shown. North is up, East is left.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{fig2.eps} \end{figure}$	Figure 2: The general photometric behavior of QW Ser during its 2003 superoutburst. Visual estimates collected in the VSNET archive are shown as open circles and CCD observations described in this paper as dots.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{fig3.eps} \end{figure}$	Figure 3: The light curves of QW Ser observed during four consecutive nights in February 2003.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig4.eps} \end{figure}$	Figure 4: The light curves of QW Ser observed during the eight longest runs from period Mar. 07/08-May 04/05.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig5.eps} \end{figure}$	Figure 5: ANOVA power spectrum of the light curve of QW Ser. The inset shows the magnification of the power spectrum around main frequency.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig6.eps} \end{figure}$	Figure 6: ANOVA power spectrum of the light curve of QW Ser from the period Mar. 07/08 - May 04/05.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig7.eps} \end{figure}$	Figure 7: Stolz & Schoembs relation for 44 ordinary SU UMa stars (open circles) and 10 stars other than dwarf novae (filled circles). The position of QW Ser is denoted by the solid triangle.
Open with DEXTER