All Tables

Table 1: Parameters of PSR B0540-69.3 (Manchester et al. 1993a, unless specified otherwise).
Table 2: Log of VLT observations of PSR B0540-69.3 on 2002 January 9.
Table 3: Broad-band fluxes^a from PSR B0540-69.3.
Table 4: Broad-band fluxes from a 10 pixel aperture around PSR B0540-69.3.
Table 5: Parameters of the power law spectral fits ( $F_{\nu }=F_{\nu _0}(\nu /\nu _0)^{-\alpha _{\nu }}$ ) of the pulsar data shown in Fig. 4.
Table 6: Broad-band fluxes and power-law fit ( $F_{\nu }=F_{\nu _0}(\nu /\nu _0)^{-\alpha _{\nu }}$ ) parameters of the emission from different regions of the PWN marked in Fig. 5. Their offsets from the pulsar and areas are given in the 2nd and 3rd columns. Upper and lower values for each entry of the fluxes are the measured and dereddened fluxes with E(B-V)=0.20 (A_V=0.62), respectively.
Table 7: Coordinates of PSR B0540-69.3.
Table 8: Comparison of the optical and X-ray spectral indices ( ${\rm\alpha ^{O}_{\nu }}$ , ${\rm\alpha ^{X}_{\nu }}$ ), luminosities ( ${L^{\rm O}}$ , ${L^{\rm X}}$ ), efficiencies ( ${ \rm\eta ^{O} }$ , ${ \rm\eta ^{X} }$ ), and a weighted ratio ( ${L^{\rm O}\Delta E^{\rm X}/L^{\rm X}\Delta E^{\rm O}}$ ) of the two young pulsars, Crab and PSR B0540-69.3, and the older Vela pulsar. Here $\Delta E^{\rm O}$ and $\Delta E^{\rm X}$ are the energy intervals in the optical^a and X-rays^b, respectively, used for the frequency integration to obtain ${L^{\rm O}}$ and ${L^{\rm X}}$ . Information on the period P, dynamical age ${\rm\tau }$ , spindown luminosity $\dot E$ , and distance d for each pulsar is included.
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.