Using Chandra to Unveil the High‐Energy Properties of the High Magnetic Field Radio Pulsar J1119−6127

Abstract

PSR J1119-6127 is a high magnetic field (B=4.1◊1013 G), young (H=1.8◊1022 cm-2), and a total luminosity LX(0.5-7.0 keV)~4◊1032 ergs s-1, at a distance of 8.4 kpc. We rule out a single blackbody model for the pulsar and present the first evidence of nonthermal emission that dominates above ~3 keV. A two-component model consisting of a power-law component (with photon index Gamma~1.5-2.0) plus a thermal component provides the best fit. The thermal component can be fit by either a blackbody model with a temperature kT~0.21 keV, or a neutron star atmospheric model with a temperature kT~0.14 keV. The efficiency of the pulsar in converting its rotational power, E, into nonthermal X-ray emission from the pulsar and PWN is ~5◊10-4, comparable to other rotation-powered pulsars with a similar E. We discuss our results in the context of the X-ray manifestation of high magnetic field radio pulsars in comparison with rotation-powered pulsars and magnetars.