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Chandra Detection of the X-ray counterpart of the High-magnetic field Radio Pulsar J1119-6127 in the Supernova Remnant G292.2-0.5

Marjorie Gonzalez·Samar Safi-Harb
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Abstract

We report the Chandra Advanced CCD Imaging Spectrometer detection of the X-ray counterpart of the high magnetic field, ~1600 year-old, 407 ms radio pulsar J1119-6127 associated with the supernova remnant G292.2-0.5. The powerful imaging capability of Chandra also unveiled, for the first time, a faint 3"x6" pulsar wind nebula (PWN) at energies above ~1.2 keV. The X-ray emission from the pulsar and its associated nebula is well described by an absorbed power law model with a photon index of 2.2 (1.9-2.8). The corresponding 0.5-10 keV unabsorbed X-ray luminosity is 5.5(2.2-15.5)x10^32 ergs/s (at 6 kpc). When compared to two other pulsars with similar spin and magnetic properties, J1119-6127 stands out as being the least efficient at turning rotational kinetic energy into X-ray emission. This study shows that high magnetic field radio pulsars can be significant X-ray emitters and Chandra is needed to study the emission properties of the pulsars and associated faint PWNe.

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Marjorie Gonzalez, Samar Safi-Harb. 2003-05-26. Chandra Detection of the X-ray counterpart of the High-magnetic field Radio Pulsar J1119-6127 in the Supernova Remnant G292.2-0.5. https://doi.org/10.1086/377070

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