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The minimum initial mass required for a star to explode as an Fe corecollapse supernova, typically denoted $M_\text{mas}$, is an important quantityin stellar evolution because it defines the border between intermediate massand massive stellar evolutionary paths. The precise value of $M_\text{mas}$carries implications for models of galactic chemical evolution and thecalculation of star formation rates. Despite the fact that stars with supersolar metallicities are commonplace within spiral and some giant ellipticalgalaxies, there are currently no studies of this mass threshold in supermetal-rich models with $Z>0.05$. Here, we study the minimum mass necessary fora star to undergo an Fe core collapse supernova when its initial metal contentfalls in the range $2.5\times 10^{-3} \leq Z \leq 0.10$. Although an increasein 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 steadyreversal in trend that occurs for $Z > 0.05$. Our super metal-rich models thusundergo Fe core collapse at lower initial masses than those required at solarmetallicity. Our results indicate that metallicity--dependent curves extendingto $Z=0.10$ for the minimum Fe ignition mass should be utilised in galacticchemical evolution simulations to accurately model supernovae rates as afunction of metallicity, particularly for simulations of metal-rich spiral andelliptical galaxies.

Bridging the Gap between Intermediate and Massive Stars II: $M_\text{mas}$ for the most metal-rich stars and implications for Fe CCSNe rates