All Figures

$\begin{figure} \par\includegraphics[width=17.2cm,clip]{9592fig1.eps} \end{figure}$ Figure 1: Eight nova candidates in M 81: example of high-quality narrow-band H $_{\alpha }$ image used in our search for novae. Original images were obtained under excellent seeing by Sorensen using the 2.54-m Isaac Newton Telescope at La Palma. Raw images downloaded from the Isaac Newton Group Archive were processed using standard reduction procedures and co-added; spatial median filter was then applied on co-added image. Image presented here has 1800 s of total exposure time and shows 7 $^\prime$ $\times$ 7 $^\prime$ of the central region of M 81. Each of eight classical nova candidates recorded on this image are marked by two perpendicular lines.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9592fig2.eps} \end{figure}$ Figure 2: Light curve of an exceptionally bright nova M 81N 2007-04b. Filled and open circles indicate measurements with an uncertainty $\leq$ 0.2 mag and >0.2 mag, respectively.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9592fig3.eps} \end{figure}$ Figure 3: Light curve of classical nova candidate M 81N 2003-05c: a typical light curve for a slow nova with long-lasting raise phase >25 days in H $_{\alpha }$ showing its raise phase.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9592fig4.eps} \end{figure}$ Figure 4: Cumulative radial number distribution of nova candidates. See text for details.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{9592fig5.eps} \end{figure}$ Figure 5: The cumulative radial distribution of nova candidates, corrected for effective coverage, compared with the components of galaxy light. See text for details.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{9592fig6.eps} \end{figure}$ Figure 6: Effective coverage of the images used in this work. Outer boundary of the M 81 galaxy and its major axis are plotted as solid line. The classical nova candidates from this work plus 9 novae found by Neill & Shara (2004) are plotted as white circles. See text for details.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{9592fig7.eps}\par \end{figure}$ Figure 7: Spatial distribution of 84 classical nova candidates in M 81: classical nova candidates found by Shara et al. (1999), by Neill & Shara (2004) and from this work.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{9592fig8.eps} \end{figure}$ Figure 8: Probability of nondetection of novae in our images covering the outer regions of the galaxy depending on number of novae explosions which really occured. Novae with mean lifetime of 100 and 40 days are plotted with solid and dotted lines, respectively.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9592fig2.eps} \end{figure}$	Figure 2: Light curve of an exceptionally bright nova M 81N 2007-04b. Filled and open circles indicate measurements with an uncertainty $\leq$ 0.2 mag and >0.2 mag, respectively.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm]{9592fig3.eps} \end{figure}$	Figure 3: Light curve of classical nova candidate M 81N 2003-05c: a typical light curve for a slow nova with long-lasting raise phase >25 days in H $_{\alpha }$ showing its raise phase.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm]{9592fig4.eps} \end{figure}$	Figure 4: Cumulative radial number distribution of nova candidates. See text for details.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm]{9592fig5.eps} \end{figure}$	Figure 5: The cumulative radial distribution of nova candidates, corrected for effective coverage, compared with the components of galaxy light. See text for details.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm]{9592fig6.eps} \end{figure}$	Figure 6: Effective coverage of the images used in this work. Outer boundary of the M 81 galaxy and its major axis are plotted as solid line. The classical nova candidates from this work plus 9 novae found by Neill & Shara (2004) are plotted as white circles. See text for details.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=11cm,clip]{9592fig7.eps}\par \end{figure}$	Figure 7: Spatial distribution of 84 classical nova candidates in M 81: classical nova candidates found by Shara et al. (1999), by Neill & Shara (2004) and from this work.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm]{9592fig8.eps} \end{figure}$	Figure 8: Probability of nondetection of novae in our images covering the outer regions of the galaxy depending on number of novae explosions which really occured. Novae with mean lifetime of 100 and 40 days are plotted with solid and dotted lines, respectively.
Open with DEXTER