Table 9: Same as in Table 8 but for the PWNs of the same pulsars. Information on the PWN size and the ratios of the pulsar to PWN luminosities in the optical and X-rays for each pulsar is included.
PWN size $ {\rm\alpha ^{O}_{\nu }}$ ${L^{\rm O,a}}$ ${ \rm\eta ^{O} } $ ${\alpha^{\rm X}_{\nu}}$ ${L^{\rm X,b}}$ ${ \rm\eta ^{X} } $ ${L^{\rm O}\Delta E^{\rm X} \over L^{\rm X}\Delta E^{\rm O}}$ ${L^{\rm O}_{\rm psr}/L^{\rm O}_{\rm pwn}}$ ${L^{\rm X}_{\rm psr}/L^{\rm X}_{\rm pwn}}$
  pc   ${\rm 10^{33}~erg~s^{-1}} $ ${\rm 10^{-5} } $   ${\rm 10^{36}~erg~s^{-1}} $ ${\rm 10^{-3} } $      
Crab 1.5 0.92c 4240c 920 1.14b 21.8d 47.5 867 0.0017 0.046
0540 0.6-0.9 1.5e 366e 245 1.04b 12d 79.7 136 0.03 0.26
Vela 0.14 - - - 0.5f ${\rm 6.8^d\times 10^{-4}}$ ${\rm 9.8\times 10^{-2}}$ - - 0.34
a For the optical range 1.57-3.68 eV. e This paper.
b For the X-ray range 0.6-10 keV. f From Pavlov et al. (2001b); $ {L^{\rm X}} $ rescaled to the 0.6-10 keV
c Optical fluxes are taken from Veron-Cety & Woltjer (1993). range and d=0.29 kpc.
d Kaaret et al. (2001); $ {L^{\rm X}} $ rescaled to the 0.6-10 keV range.  

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