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We present a Chandra and XMM-Newton imaging and spectroscopic study of thesupernova remnant (SNR) RCW 103 (G332.4-00.4) containing the Central CompactObject 1E 161348-5055. The high resolution Chandra X-ray images reveal enhancedemission in the south-eastern and north-western regions. Equivalent width lineimages of Fe L, Mg, Si, and S using XMM-Newton data were used to map thedistribution of ejecta. The SNR was sectioned into 56 regions bestcharacterized by two-component thermal models. The harder component (kT~0.6keV) is adequately fitted by the VPSHOCK non-equilibrium ionization model withan ionization timescale ~ 1E11-1E12 cm^-3 s, and slightly enhanced abundancesover solar values. The soft component (kT~0.2 keV), fitted by the APEC model,is well described by plasma in collisional ionization equilibrium withabundances consistent with solar values. Assuming a distance of 3.1 kpc and aSedov phase of expansion into a uniform medium, we estimate an SNR age of 4.4kyr, a swept-up mass M_sw=16 f_s^{-1/2} D_{3.1}^{5/2} solar masses, and a lowexplosion energy E=3.7E49 f_s^{-1/2} D_{3.1}^{5/2} erg. This energy could be anorder of magnitude higher if we relax the Sedov assumption, the plasma has alow filling factor, the plasma temperature is under-estimated, or if the SNR isexpanding into the progenitor's wind-blown bubble. Standard explosion modelsdid not match the ejecta yields. By comparing the fitted abundances to the mostrecent core-collapse nucleosynthesis models, our best estimate yields alow-mass progenitor around 12-13 solar masses, lower than previously reported.We discuss degeneracies in the model fitting, particularly the effect ofaltering the explosion energy on the progenitor mass estimate.

monthly notices of the royal astronomical society

Progenitors and Explosion Properties of Supernova Remnants Hosting  Central Compact Objects: I. RCW 103 Associated with the Peculiar Source 1E  161348-5055