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Typing the origin (i.e., Type Ia or core-collapse) of supernova remnants(SNRs) is crucial to determine the rates of supernova (SN) explosions in agalaxy, which is a key to understand its recent chemical evolution. However,evolved SNRs in the so-called Sedov phase are dominated by the swept-upinterstellar medium (ISM), making it difficult to determine their ejectacomposition and thus SN type. Here we present a systematic X-ray study of nineevolved SNRs in the Magellanic Clouds, DEM L238, DEM L249, 0534-69.9,0548-70.4, B0532-71.0, B0532-67.5, 0103-72.6, 0049-73.6, and 0104-72.3, usingarchival data of the Suzaku satellite. Although Suzaku does not spatiallyresolve the SN ejecta from the swept-up ISM due to the limited angularresolution, its excellent energy resolution has enabled clear separation ofemission lines in the soft X-ray band. This leads to the finding that the`spatially-integrated' spectra of the evolved (~10^4 yr) SNRs are stillsignificantly contributed by emission from the ejecta at the energies around 1keV. The Fe/Ne mass ratios, determined mainly from the well-resolved Fe L-shelland Ne K-shell lines, clearly divide the observed SNRs into the Type Ia andcore-collapse groups, confirming some previous typing made by Chandraobservations that had utilized its extremely high angular resolution. Thisdemonstrates that spatially-integrated X-ray spectra of old SNRs can also beused to discriminate their progenitor type, which would be helpful for futuresystematic studies of extragalactic SNRs with ASTRO-H and beyond.

A Systematic Study of Evolved Supernova Remnants in the Large and Small Magellanic Clouds with Suzaku