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We present the first detailed imaging and spatially resolved spectroscopicstudy of the Galactic supernova remnant G292.2-0.5, associated with thehigh-magnetic field radio pulsar J1119-6127, using Chandra and XMM-Newton. Thehigh-resolution X-ray images reveal a partially limb-brightened morphology inthe west, with diffuse emission concentrated towards the interior of theremnant unlike the complete shell-like morphology observed at radiowavelengths. The spectra of most of the diffuse emission regions within theremnant are best described by a thermal+non-thermal model. The thermalcomponent is described by a plane-parallel, non-equilibrium ionization plasmamodel with a temperature ranging from 1.3 keV in the western side of theremnant to 2.3 keV in the east, a column density increasing from 1.0e22 cm^-2in the west to 1.8e22 cm^-2 in the east, and a low ionization timescale rangingfrom 5.7e9 cm^-3 s in the SNR interior to 3.6e10 cm^-3 s in the western side -suggestive of expansion of a young remnant in a low-density medium. The spatialand spectral differences across the SNR are consistent with the presence of adark cloud in the eastern part of the SNR, absorbing the soft X-ray emission.The spectra from some of the regions also show slightly enhanced metalabundances from Ne, Mg and Si, hinting at the first evidence for ejecta heatedby the reverse shock. Comparing our inferred metal abundances to core-collapsenucleosynthesis models yields, we estimate a high progenitor mass of ~30 solarmass suggesting a type Ib/c supernova. We confirm the presence of non-thermalhard X-ray emission from regions close to the pulsar. We estimate an SNR agerange between 4.2 kyr (free expansion phase) and 7.1 kyr (Sedov phase), afactor of a few higher than the measured pulsar's age upper limit of 1.9 kyr.

Chandra and XMM-Newton studies of the supernova remnant G292.2-0.5 associated with the pulsar J1119-6127