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Supernova remnants (SNRs) retain crucial information about both their parentexplosion and circumstellar material left behind by their progenitor. However,the complexity of the interaction between supernova ejecta and ambient mediumoften blurs this information, and it is not uncommon for the basic progenitortype (Ia or core-collapse) of well-studied remnants to remain uncertain. Herewe present a powerful new observational diagnostic to discriminate betweenprogenitor types and constrain the ambient medium density of SNRs solely usingFe K-shell X-ray emission. We analyze all extant Suzaku observations of SNRsand detect Fe K alpha emission from 23 young or middle-aged remnants, includingfive first detections (IC 443, G292.0+1.8, G337.2-0.7, N49, and N63A). The Fe Kalpha centroids clearly separate progenitor types, with the Fe-rich ejecta inType Ia remnants being significantly less ionized than in core-collapse SNRs.Within each progenitor group, the Fe K alpha luminosity and centroid are wellcorrelated, with more luminous objects having more highly ionized Fe. Ourresults indicate that there is a strong connection between explosion type andambient medium density, and suggest that Type Ia supernova progenitors do notsubstantially modify their surroundings at radii of up to several parsecs. Wealso detect a K-shell radiative recombination continuum of Fe in W49B and IC443, implying a strong circumstellar interaction in the early evolutionaryphases of these core-collapse remnants.

Discriminating the Progenitor Type of Supernova Remnants with Iron K-Shell Emission