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abstract: 'Though the neutrino-driven convection model for the core-collapse explosion mechanism has received strong support in recent years, there are still many uncertainties in the explosion parameters – such as explosion energy, remnant mass, and end-of-life stellar abundances as initial conditions. Using a broad set of spherically symmetric core-collapse simulations we examine the effects of these key parameters on explosive nucleosynthesis and final explosion yields. Post-bounce temperature and density evolution of ZAMS 15, 20, and 25 solar mass progenitors are post-processed through the Nucleosynthesis Grid (NuGrid) nuclear network to obtain detailed explosive yields. In particular, this study focuses on radio-isotopes that are of particular interest to the next generation of gamma-ray astronomical observations; $\isotope[43]{K}$, $\isotope[47]{Ca}$, $\isotope[44]{Sc}$, $\isotope[47]{Sc}$, $\isotope[48]{V}$, $\isotope[48]{Cr}$, $\isotope[51]{Cr}$, $\isotope[52]{Mn}$, $\isotope[59]{Fe}$, $\isotope[56]{Co}$, $\isotope[57]{Co}$, and $\isotope[57]{Ni}$. These nuclides may be key in advancing our understanding of the inner workings of core-collapse supernovae by probing the parameters of the explosion engine. We find that the isotopes that are strong indicators of explosion energy are , , , , and , those that are dependent on the progenitor structure are , , and , and those that probe neither are , , , and . We discuss prospects of observing these 