  Stellar evolution models require an initial isotopic abundance set as input,
but these abundances have not been thoroughly established outside of our sun.
Nucleosynthesis studies require reliable isotopic abundances which are
challenging to infer from elemental observations and are galaxy specific.
Despite the challenges, accurate GCE models for dSphs can provide significant
insight on the galactic hierarchy. We present an isotopic history model for the
Sculptor dSph galaxy based on astrophysical processes, which is a complementary
approach to GCE models. We estimate the isotopic composition of Sculptor's late
stage evolution using OMEGA, and we use BBN as the other boundary condition.
Each astrophysical process was assigned a parametric function with free
parameters according to the underlying physics that dictate their average
chemical evolution. The isotopic yields were summed into elemental yields and
fit to observational Sculptor abundance data to fix the free parameters. This
procedure gives an average isotopic history of Sculptor for massive star, Type
1a SNe, main s-process peak, and r-process contributions, which can be compared
with the chemical history of the MW. We find that Type 1a SNe contribute
approximately 86 per cent to the late stage evolution Fe abundance, which is
greater than typical MW solar values of approximately 70 per cent, and in
agreement with other dSph chemical evolution studies. The model also finds that
NSMs only contribute approximately 30 per cent to the late stage evolution Eu
abundance, further suggesting that CCSNe are the more dominant r-process
progenitor in dSphs.
