Chandra and XMM-Newton study of the supernova remnant Kes 73 hosting the magnetar 1E 1841-045.
KUMAR H.S., SAFI-HARB S., SLANE P.O. and GOTTHELF E.V.
Abstract (from CDS):
We present a Chandra and XMM-Newton study of the supernova remnant (SNR) Kes 73 hosting the anomalous X-ray pulsar 1E 1841-045. The Chandra image reveals clumpy structures across the remnant with enhanced emission along the western rim. The X-ray emission fills the radio shell and spatially correlates with the infrared image. The global X-ray spectrum is described by a two-component thermal model with a column density NH= 2.6–0.3+0.41022/cm2 and a total luminosity of LX= 3.3–0.5+0.71037 erg/s (0.5-10 keV, at an assumed distance of 8.5 kpc). The soft component is characterized by a temperature kTs= 0.5–0.2+0.1 keV, a high ionization timescale, and enhanced Si and S abundances, suggesting emission that is dominated by shocked ejecta. The hard component has a temperature kTh= 1.6–0.7+0.8 keV, a relatively low ionization timescale, and mostly solar abundances suggesting emission that is dominated by interstellar/circumstellar shocked material. A spatially resolved spectroscopy study reveals no significant variations in the spectral properties. We infer an SNR age ranging between 750 yr and 2100 yr, an explosion energy of 3.0_-1.8+2.8 x 1050 erg and a shock velocity of (1.2±0.3)x103 km/s (under the Sedov phase assumption). We also discuss the possible scenario for Kes 73 expanding into the late red-supergiant wind phase of its massive progenitor. Comparing the inferred metal abundances to core-collapse nucleosynthesis model yields, we estimate a progenitor mass ≳ 20 M☉, adding a candidate to the growing list of highly magnetized neutron stars proposed to be associated with very massive progenitors.