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

High Energy Astrophysical Phenomena