$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1518fig2.eps} \end{figure}$ Figure 2: Local coordinate distributions of, a) azimuth " $\phi$ '' and b) zenith "z'' angles of logged EAS events.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{1518fig4.eps} \end{figure}$ Figure 4: Exposure map of simulated events in 1 $^{\circ }\times 1^{\circ }$ bins base on the general parameters of the total distribution of EAS events in galactic coordinates.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{1518fig5.eps} \end{figure}$ Figure 5: Corrected exposure map extracted by pixel-by-pixel division of the data map (Fig. 3) by the exposure map (Fig. 4).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1518fig6.eps} \end{figure}$ Figure 6: Distribution of frequency of a) 98 000 virtual random sources and b) 98 EGRET sources in the FOV of our array in galactic coordinates versus their statistical significance. $a_{\sigma }$ , $b_{\sigma }$ and $c_{\sigma }$ are described in Eq. (14).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1518fig7.eps} \end{figure}$ Figure 7: Distribution of mean count per pixel of a) 98 000 virtual random sources and b) 10 EGRET sources of Table 1 versus error radial distance from the centre of the related sources.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{1518fig8.eps} \end{figure}$ Figure 8: Map of EGRET sources with statistical significance more than 1.5 in galactic coordinates. The numbered sources are listed in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{1518fig1.eps} \end{figure}$	Figure 1: Experimental set up and electronic circuits.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1518fig2.eps} \end{figure}$	Figure 2: Local coordinate distributions of, a) azimuth " $\phi$ '' and b) zenith "z'' angles of logged EAS events.
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$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{1518fig3.eps} \end{figure}$	Figure 3: EAS events map in 1 $^{\circ }\times 1^{\circ }$ bin galactic coordinates.
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$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{1518fig4.eps} \end{figure}$	Figure 4: Exposure map of simulated events in 1 $^{\circ }\times 1^{\circ }$ bins base on the general parameters of the total distribution of EAS events in galactic coordinates.
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$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{1518fig5.eps} \end{figure}$	Figure 5: Corrected exposure map extracted by pixel-by-pixel division of the data map (Fig. 3) by the exposure map (Fig. 4).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1518fig6.eps} \end{figure}$	Figure 6: Distribution of frequency of a) 98 000 virtual random sources and b) 98 EGRET sources in the FOV of our array in galactic coordinates versus their statistical significance. $a_{\sigma }$ , $b_{\sigma }$ and $c_{\sigma }$ are described in Eq. (14).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1518fig7.eps} \end{figure}$	Figure 7: Distribution of mean count per pixel of a) 98 000 virtual random sources and b) 10 EGRET sources of Table 1 versus error radial distance from the centre of the related sources.
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$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{1518fig8.eps} \end{figure}$	Figure 8: Map of EGRET sources with statistical significance more than 1.5 in galactic coordinates. The numbered sources are listed in Table 1.
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