We report on the emission properties of PSR B1929 + 10 and its putative trail from a multi-wavelength study performed using optical , X-ray and radio data .
XMM-Newton observations confirm the existence of the diffuse emission with a trail morphology lying in a direction opposite to the transverse motion of the pulsar .
The trail spectrum is non-thermal and produced by electron-synchrotron emission in the shock between the pulsar wind and the surrounding medium .
Radio data from the Effelsberg 11cm radio continuum survey show an elongated feature which roughly coincides with the X-ray trail .
Three not fully resolved radio sources seen in the NVSS survey data at 1.4 GHz match with part of the elongated radio feature seen at 11cm .
The emission properties observed from PSR B1929 + 10 are in excellent agreement with a non-thermal and , thus , magnetospheric radiation dominated emission scenario .
The pulsar ’ s X-ray spectrum is best described by a single power law model with a photon index of 2.72 ^ { +0.12 } _ { -0.09 } .
A flux contribution from the thermal emission of heated polar caps of at most \sim 7 \% is inferred from a best fitting composite Planckian and power law spectral model .
A pure thermal emission spectrum consisting of two Planckian spectra is regarded as unlikely .
A broken power law spectral model with E _ { break } = 0.83 ^ { +0.05 } _ { -0.03 } \mbox { keV } and the photon-indexes \alpha _ { 1 } = 1.12 ^ { +0.02 } _ { -0.03 } and \alpha _ { 2 } = 2.48 ^ { +0.08 } _ { -0.07 } can describe the optical and X-ray data entirely in terms of a non-thermal magnetospheric origin .
The X-ray pulse profile observed in the 0.2 - 10 keV band is found to be markedly different from the broad sinusoidal pulse profile seen in the low statistic ROSAT data .
Fitting Gaussians to the X-ray light curve indicates the possible existence of three pulse components .
A small narrow pulse , characterized by energies greater than 1 keV , is found to lead the radio main pulse by \sim 20 ^ { \circ } .
The fraction of pulsed photons in the 0.2 - 10 keV band is 32 \pm 4 \% .
For the sub-bands 0.2 - 1.0 keV and 1.0 - 2.1 keV the pulsed fraction is 24 \pm 5 \% and 44 \pm 6 \% , respectively , indicating a mild energy dependence at a \sim 2 \sigma level .
Simulations in the framework of an outer-gap emission model are able to reproduce the observed X-ray pulse profile and its phase shift relative to the radio pulse .