  The minimum initial mass required for a star to explode as an Fe core
collapse supernova, typically denoted $M_\text{mas}$, is an important quantity
in stellar evolution because it defines the border between intermediate mass
and massive stellar evolutionary paths. The precise value of $M_\text{mas}$
carries implications for models of galactic chemical evolution and the
calculation of star formation rates. Despite the fact that stars with super
solar metallicities are commonplace within spiral and some giant elliptical
galaxies, there are currently no studies of this mass threshold in super
metal-rich models with $Z>0.05$. Here, we study the minimum mass necessary for
a star to undergo an Fe core collapse supernova when its initial metal content
falls in the range $2.5\times 10^{-3} \leq Z \leq 0.10$. Although an increase
in initial $Z$ corresponds to an increase in the Fe ignition threshold for $Z
\approx 1\times 10^{-3}$ to $Z\approx0.04$, we find that there is a steady
reversal in trend that occurs for $Z > 0.05$. Our super metal-rich models thus
undergo Fe core collapse at lower initial masses than those required at solar
metallicity. Our results indicate that metallicity--dependent curves extending
to $Z=0.10$ for the minimum Fe ignition mass should be utilised in galactic
chemical evolution simulations to accurately model supernovae rates as a
function of metallicity, particularly for simulations of metal-rich spiral and
elliptical galaxies.
