\begin{table}%T2
\caption{\label{tab2}Comparison of observed and theoretical $\gamma$-ray
luminosity for confirmed high-energy $\gamma$-ray pulsars. }
 \small%\centerline
{
\begin{tabular}{cccccccc}
\hline\hline \noalign{\smallskip}
PSR & $P$ & $B_{12}$ & $d$  & $\alpha$& $f(\bar{r})$&
$\eta^{\rm th}_{\gamma}$ & $\eta^{\rm ob}_{\gamma} $
\\
& (s) & (G) & (kpc)& (deg.)& & (\%) & (\%)\\\hline
B0531+21&0.033&  7.53& $  2.0 $  & $\sim$$72$&0.04  &0.006  & $0.013\pm0.006$ \\
B0833-45&0.089&  6.75& $  0.3 $  & $\sim$$ 28$&0.10 &0.102  & $0.065\pm0.025$ \\
B0633+17&0.237&  3.28& $  0.16$  & $\sim$$ 40$&0.53 &15.0  & $5.0\pm4.0$\\
B1706-44&0.1025&  6.25& $  1.82 $& $\sim$$60$&0.15  &0.35  &$0.72\pm0.47$ \\
B1951+32&0.0395&  0.97& $  2.5 $ & $\sim$$ 58$&0.13 &0.23  & $0.26\pm0.17$ \\
B1046-58&0.124&  6.98& $  2.98$  & $\sim$$68$&0.20  &0.82  &$1.1\pm 0.3$ \\
B1055-52&0.197&  2.17& $ 1.53$   & $\sim$$63$&0.64 &25.6  &$15\pm 7$ \\
\hline
\end{tabular}}
\smallskip
Note: the inclination angle for each pulsar is estimated by using
X-ray observed data in the frame of our model.
\end{table}