  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 a
galaxy, which is a key to understand its recent chemical evolution. However,
evolved SNRs in the so-called Sedov phase are dominated by the swept-up
interstellar medium (ISM), making it difficult to determine their ejecta
composition and thus SN type. Here we present a systematic X-ray study of nine
evolved 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, using
archival data of the Suzaku satellite. Although Suzaku does not spatially
resolve the SN ejecta from the swept-up ISM due to the limited angular
resolution, its excellent energy resolution has enabled clear separation of
emission 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 still
significantly contributed by emission from the ejecta at the energies around 1
keV. The Fe/Ne mass ratios, determined mainly from the well-resolved Fe L-shell
and Ne K-shell lines, clearly divide the observed SNRs into the Type Ia and
core-collapse groups, confirming some previous typing made by Chandra
observations that had utilized its extremely high angular resolution. This
demonstrates that spatially-integrated X-ray spectra of old SNRs can also be
used to discriminate their progenitor type, which would be helpful for future
systematic studies of extragalactic SNRs with ASTRO-H and beyond.
