Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{1385fig1.eps} \end{figure}$ Figure 1: Spatial distribution of the simulated $\gamma$ -ray pulsars with ages of $\leq$ $2\times 10^7$ yr in the Galaxy. The birth rate of neutron stars is assumed to be 1/100 yr and the $\gamma$ -ray sensitivity is the EGRET sensitivity. Open (solid) circles represent radio quite (radio loud) $\gamma$ -ray pulsars.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1385fig2.eps} \end{figure}$ Figure 2: Spatial distribution of the simulated $\gamma$ -ray pulsars with ages of $\leq$ $5\times 10^6$ yr in the Gould belt. The birth rate of neutron stars is assumed to be 20 Myr^-1 and $\gamma$ -ray sensitivity is the EGRET sensitivity. Open (solid) circles represent radio quite (radio loud) $\gamma$ -ray pulsars.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{1385fig3.eps} \end{figure}$ Figure 3: Plot of $\gamma$ -ray luminosity vs. spin-down luminosity for the simulated $\gamma$ -ray pulsars in the Galaxy. The EGRET sensitivity has been used. Open and solid circles represent the radio quiet and radio loud $\gamma$ -ray pulsars respectively. Long dashed line and short dashed line are corresponding best fits.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{1385fig4.eps} \end{figure}$ Figure 4: Plot of $\gamma$ -ray luminosity vs. spin-down luminosity for the simulated $\gamma$ -ray pulsars in the Gould belt. The EGRET sensitivity has been used. Open and solid circles represent the radio quiet and radio loud $\gamma$ -ray pulsars respectively. The long dashed line and short dashed line are corresponding best fits.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{1385fig5.eps} \end{figure}$ Figure 5: Plot of $\gamma$ -ray luminosity vs. spin-down luminosity for thesimulated $\gamma$ -ray pulsars in both the Galaxy and Gould belt. The EGRET sensitivity has been used. Open and solid circles representthe radio quiet and radio loud $\gamma$ -ray pulsars respectively. the long dashed line and short dashed line are corresponding best fits.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{1385fig6.eps} \end{figure}$ Figure 6: Variation of parameter $\delta$ with galactic latitude. The parameter $\delta$ is defined as $L_{\gamma }\propto L^{\delta }_{\rm sd}$ . For the EGRET sensitivity, the results are shown by open boxes. For the GLAST sensitivity, solid boxes represent values of $\delta$ at different galactic latitude regions for all $\gamma$ -ray pulsars.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{1385fig7.eps} \end{figure}$ Figure 7: Ratio of $\gamma$ -ray pulsars at different galactic latitude regions to total $\gamma$ -ray pulsars for the EGRET sensitivity. Solid line represents the ratio in the Galaxy and dashed line in the Gould belt.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{1385fig8.eps} \end{figure}$ Figure 8: Ratio of $\gamma$ -ray pulsars with ages of $\le$ $\times 10^6$ yr to $\gamma$ -ray pulsars at different galactic latitude regions for the EGRET (short dashed line) and the GLAST (long dashed line) sensitivities, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1385fig1.eps} \end{figure}$	Figure 1: Spatial distribution of the simulated $\gamma$ -ray pulsars with ages of $\leq$ $2\times 10^7$ yr in the Galaxy. The birth rate of neutron stars is assumed to be 1/100 yr and the $\gamma$ -ray sensitivity is the EGRET sensitivity. Open (solid) circles represent radio quite (radio loud) $\gamma$ -ray pulsars.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{1385fig2.eps} \end{figure}$	Figure 2: Spatial distribution of the simulated $\gamma$ -ray pulsars with ages of $\leq$ $5\times 10^6$ yr in the Gould belt. The birth rate of neutron stars is assumed to be 20 Myr^-1 and $\gamma$ -ray sensitivity is the EGRET sensitivity. Open (solid) circles represent radio quite (radio loud) $\gamma$ -ray pulsars.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6cm,clip]{1385fig3.eps} \end{figure}$	Figure 3: Plot of $\gamma$ -ray luminosity vs. spin-down luminosity for the simulated $\gamma$ -ray pulsars in the Galaxy. The EGRET sensitivity has been used. Open and solid circles represent the radio quiet and radio loud $\gamma$ -ray pulsars respectively. Long dashed line and short dashed line are corresponding best fits.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6cm,clip]{1385fig4.eps} \end{figure}$	Figure 4: Plot of $\gamma$ -ray luminosity vs. spin-down luminosity for the simulated $\gamma$ -ray pulsars in the Gould belt. The EGRET sensitivity has been used. Open and solid circles represent the radio quiet and radio loud $\gamma$ -ray pulsars respectively. The long dashed line and short dashed line are corresponding best fits.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6cm,clip]{1385fig5.eps} \end{figure}$	Figure 5: Plot of $\gamma$ -ray luminosity vs. spin-down luminosity for thesimulated $\gamma$ -ray pulsars in both the Galaxy and Gould belt. The EGRET sensitivity has been used. Open and solid circles representthe radio quiet and radio loud $\gamma$ -ray pulsars respectively. the long dashed line and short dashed line are corresponding best fits.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6cm,clip]{1385fig6.eps} \end{figure}$	Figure 6: Variation of parameter $\delta$ with galactic latitude. The parameter $\delta$ is defined as $L_{\gamma }\propto L^{\delta }_{\rm sd}$ . For the EGRET sensitivity, the results are shown by open boxes. For the GLAST sensitivity, solid boxes represent values of $\delta$ at different galactic latitude regions for all $\gamma$ -ray pulsars.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6cm,clip]{1385fig7.eps} \end{figure}$	Figure 7: Ratio of $\gamma$ -ray pulsars at different galactic latitude regions to total $\gamma$ -ray pulsars for the EGRET sensitivity. Solid line represents the ratio in the Galaxy and dashed line in the Gould belt.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6cm,clip]{1385fig8.eps} \end{figure}$	Figure 8: Ratio of $\gamma$ -ray pulsars with ages of $\le$ $\times 10^6$ yr to $\gamma$ -ray pulsars at different galactic latitude regions for the EGRET (short dashed line) and the GLAST (long dashed line) sensitivities, respectively.
Open with DEXTER