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Feedback from core collapse supernovae (SNe), the final stage of evolution ofmassive stars, is a key element in galaxy formation theory. The energy budgetof SN feedback, as well as the duration over which SNe occur, are constrainedby stellar lifetime models and the minimum mass star that ends its life as aSN. Simplifying approximations for this SN rate are ubiquitous in simulationstudies. We show here how the choice of SN budget and timings ($t_0$ for thedelay between star formation and the first SN, $\tau_{\rm SN}$ for the durationof SN injection, and the minimum SN progenitor mass) drive changes in theregulation of star formation and outflow launching. Extremely long delays forinstantaneous injection of SN energy $(t_0 << 20\;\rm{Myr})$ reduces starformation and drive stronger outflows compared smaller delays. This effect isprimarily driven by enhanced clustering of young stars. With continuousinjection of energy, longer SN durations results in a larger fraction of SNenergy deposited in low ambient gas densities, where cooling losses are lower.This is effect is particularly when driven by the choice of the minimum SNprogenitor mass, which also sets the total SN energy budget. These underlyinguncertainties mean that despite advances in the sub-grid modeling of SNfeedback, serious difficulties in constraining the strength of SN feedbackremain. We recommend future simulations use realistic SN injection durations,and bound their results using SN energy budgets and durations for minimum SNprogenitors of $7M_\odot$ and $9M_\odot$.

Uncertainties in supernova input rates drive qualitative differences in simulations of galaxy evolution