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We investigate a progenitor mass distribution of core-collapse supernovaremnants (CCSNRs) in our Galaxy and the Large and Small Magellanic Clouds, forthe first time. We count the number of CCSNRs in three mass ranges divided bythe zero-age main-sequence mass, $M_{\rm ZAMS}$; A: $M_{\rm ZAMS} < 15\ {\rmM}_\odot$, B: $15\ {\rm M}_\odot < M_{\rm ZAMS} < 22.5\ {\rm M}_\odot$, C:$M_{\rm ZAMS} > 22.5\ {\rm M}_\odot$. Simple compilation of progenitor massesin the literature yields a progenitor mass distribution of $f_{\rm A}: f_{\rmB}: f_{\rm C} =0.24:0.28:0.48$, where $f$ is the number fraction of theprogenitors. The distribution is inconsistent with any standard initial massfunctions. We notice, however, that previous mass estimates are subject tolarge systematic uncertainties because most of the relative abundances (X/Si)are not really good probe for the progenitor masses. Instead, we propose torely only on the Fe/Si ratio which is sensitive to the CO core mass ($M_{\rmCOcore}$) and $M_{\rm ZAMS}$. Comparing Fe/Si ratios in SNRs in the literaturewith the newest theoretical model, we estimate 33 $M_{\rm COcore}$ and $M_{\rmZAMS}$, leading to a revised progenitor mass distribution of $f_{\rm A}: f_{\rmB}: f_{\rm C} = 0.47: 0.32 : 0.21$. This is consistent with the standardSalpeter initial mass function. However, the relation between $M_{\rm COcore}$and $M_{\rm ZAMS}$ could be affected by binary evolution, which is not takeninto account in this study and should be considered in the future work toderive a better progenitor mass distribution estimate.

Progenitor Mass Distribution of Core-Collapse Supernova Remnants in Our Galaxy and Magellanic Clouds based on Elemental Abundances