2008ApJ...684..532S

PSR J1119-6127 is a high magnetic field (B=4.1x10¹³ G), young (≤1700 year old), and slow (P=408 ms) radio pulsar associated with the supernova remnant (SNR) G292.2-0.5. In 2003, Chandra allowed the detection of the X-ray counterpart of the radio pulsar and provided the first evidence for a compact and faint pulsar wind nebula (PWN). We here present new Chandra observations that allowed for the first time an imaging and spectroscopic study of the pulsar and PWN independently of each other. The PWN is only evident in the hard band (above ∼2 keV) and consists of jetlike structures extending at least 7" from the pulsar, with the southern ``jet'' being longer than the northern ``jet.'' The spectrum of the PWN is described by a power law with a photon index Γ∼1.1 for the compact PWN and ∼1.4 for the southern long jet (at a column density N_H=1.8x10²²/cm2), and a total luminosity L_X(0.5-7.0 keV)∼4x10³² ergs/s, 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 Γ∼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{dot}, into nonthermal X-ray emission from the pulsar and PWN is ~5x10^–4, comparable to other rotation-powered pulsars with a similar E{dot}. 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.