order Cash-Karp type Runge Kutta integrator [@Cash1990a]. For more information about the microphysics (e.g. sources for reaction rates, reverse rates, screening etc) we refer the reader to @jones2019a and @jones2019b.

Network Comparison
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![Comparison of the basic composition following the explosion of the 15 solar mass model M15aE2.47 between the [@Fryer_2018] work (dashed lines) and this work (solid lines). These differences originate from the more detailed presupernova composition used in the present work, as well as the different reaction rates and more detailed isotope list in the post-processing network. The differences are most evident in the differences in the C/O layer. Though the Fe peak is in good agreement, the details of the elemental abundances differ due to sensitivity to the initial conditions.[]{data-label="fig:yieldcomp"}](yieldcomp.pdf){width="\linewidth"}

In this study, we use the same progenitor star and explosion trajectories as [@Fryer_2018], but we use different methods in the nucleosynthesis calculations. In [@Fryer_2018], the yields at collapse were taken directly from the KEPLER simulation using a reduced network [@heger05]. These initial abundances were then evolved using the Torch [@Timmes_2000] nuclear network with 640 isotopes. The nucleosynthetic yields presented in this paper use the same progenitor and explosion evolution, but instead use the NuGrid network with 