X- AND γ-RAY PULSATIONS OF THE NEARBY RADIO-FAINT PSR J1741–2054

We report the results of a deep XMM-Newton observation of the radio-faint γ -ray pulsar J1741−2054 and its nebula together with the analysis of five years ofFermi Large Area Telescope (LAT) data. The X-ray spectrum of the pulsar is consistent with an absorbed power law plus a blackbody, originating at least partly from the neutron star cooling. The nebular emission is consistent with that of a synchrotron pulsar wind nebula, with hints of spatial spectral variation. We extended the available Fermi LAT ephemeris and folded the γ -ray and X-ray data. We detected X-ray pulsations from the neutron star: both the thermal and non-thermal components are ∼35%–40% pulsed, with phase-aligned maxima. A sinusoid fits the thermal-folded profile well. A 10 bin phase-resolved analysis of the X-ray emission shows softening of the non-thermal spectrum during the on-pulse phases. The radio, X-ray, and γ -ray light curves are single-peaked, not phase-aligned, with the X-ray peak trailing the γ -ray peak by more than half a rotation. Spectral considerations suggest that the most probable pulsar distance is in the 0.3–1.0 kpc range, in agreement with the radio dispersion measure.