\begin{table}%t5
\caption{\label{pulsar_comparison}Characteristics of the three young ($<$10 kyr) X-ray and $\gamma$-ray emitting pulsars in comparison with the middle-aged Vela pulsar 
(PSR B0833-045).}
\par
%\centerline
{\small
\begin{tabular}{lcccccccccc}
\hline\hline\noalign{\smallskip}
Source               &  $d$   &  $P$   &  $\tau$ & $L_{\rm sd}$ & $F_{\rm x}$\tablefootmark{a}         & $F_{\gamma}$\tablefootmark{b} & $L_{\rm x}$\tablefootmark{a}   & $\eta_{\rm x}$\tablefootmark{a} & $L_{\gamma}$\tablefootmark{b} & $\eta_{\gamma}$\tablefootmark{b}\\
                     &[kpc] & [ms] &  [ky]   & [erg/s]  & [erg/cm$^2$ s] & [erg/cm$^2$ s] & [erg/s] &          &  [erg/s]     &                \\
\hline\noalign{\smallskip}
B0531+21   &  2.0     &  29.7   &  1.3         &4.4E+38 & $(5.68\pm 0.05)$E-09 & $(1.3\pm0.1)$E-09$^{\ }$ & $(2.72\pm0.02)$E+36 & $6.2$E-3 & $(6.1\pm0.3)$E+35$^{\ }$ & $1.4$E-3$^{\ }$\\
B1509-58   &  5.8     & 151.5   &  1.6         &1.7E+37 & $(1.46\pm 0.02)$E-10 & $(5.1\pm2.5)$E-11\tablefootmark{c} & $(5.88\pm0.08)$E+35 & $3.5$E-2 & $(2.1\pm1.0)$E+35\tablefootmark{c} & $1.2$E-2\tablefootmark{c}\\
J0205+6449 &  3.2     &  65.7   &  5.4         &2.7E+37 & $(0.36\pm 0.02)$E-11 & $(6.7\pm0.5)$E-11$^{\ }$ & $(4.45\pm0.20)$E+33 & $1.7$E-4 & $(8.2\pm0.6)$E+34$^{\ }$ & $3.0$E-3$^{\ }$\\
B0833-045  &  0.287   &  89.3   & 11.4         &6.9E+36 & $(0.88\pm 0.29)$E-11 & $(7.9\pm0.3)$E-09$^{\ }$ & $(8.67\pm2.85)$E+31 & $1.3$E-5 & $(7.8\pm0.3)$E+34$^{\ }$ & $1.1$E-2$^{\ }$\\
\hline
\end{tabular}}
\tablefoot{The luminosities of the pulsed emission $L$ are calculated as $L = 4\pi d^2Ff_{\Omega}$ with values for the distance $d$ taken from the table, and the beaming fraction $f_\Omega$ set to 1. $F$ represent the pulsed flux.
\tablefoottext{a}{Luminosities, fluxes, and efficiencies labeled with $x$ are evaluated for the 2--100~keV band.} 
\tablefoottext{b}{Luminosities, fluxes, and efficiencies labeled with $\gamma$ are evaluated for the 0.1--10~GeV band.}
\tablefoottext{c}{The $\gamma$-ray energy flux of PSR B1509-58 in the 0.1--10~GeV band has been derived from the (total) photon flux values for the 100--300 and 300--1000~MeV bands as given in \citet{kuiper1999} assuming a power-law shape with photon index of $2.5$, and should be considered as an upper-limit to the pulsed flux of PSR B1509-58 in the 0.1--10~GeV band.}}
\end{table}