RA: Right ascension (hours minutes seconds)
Dec: Declination (degrees minutes seconds)
P0: Barycentric period of the pulsar (s)
DM: Dispersion measure (cm-3 pc)
W50: Width of pulse at 50% of peak (ms)
W10: Width of pulse at 10% of peak (ms)
S400: Mean flux density at 400 MHz (mJy)
Scintillation effects are relatively benign for this pulsar - variations due to diffractive scintillation occur in a much shorter time frame than typical observation times and so such variations average out. Longer terms diffractive and refractive effects have a low modulation index (variations are not large: generally limited less than 3 dB) making the day-to-day variations relatively small compared with, say, B0329+54.
One notable characteristic is that the radiation from the Vela pulsar is almost completely polarised - predominantly linear, but with some degree of circular polarisation. This is an important factor as using a linearly-polarised antenna could result in periods of cross-polarisation leading to loss in signal strength. This consideration drove the adoption of a circularly-polarised antenna system. Dual orthogonal linear probes could have been used, but that would require a duplication of the receiver chain - a complication not attractive at this stage.