  PSR B0355+54 is one of the handful of pulsars that has been observed with
both Chandra and XMM-Newton. The analysis of the archival data has revealed the
pulsar and a ~30 arcsec compact nebula surrounding it. XMM-Newton also has
detected a trail which extends ~6 arcmin and similar to the compact nebula is
also counter-aligned with the proper motion of the pulsar. The spectrum of both
the pulsar and the extended emission are well described by an absorbed
power-law model. The measured flux corresponds to an efficiency of converting
the spin-down luminosity into X-rays in the 2-10 keV band of ~0.01% and ~1% for
the pulsar and the extended emission, respectively. From the XMM-Newton data we
have detected pulsations at the expected radio period. The energetic and the
extent of the extended emission can be explained by a Bow-shock formed by the
motion of the pulsar through the interstellar medium.
