  Core-collapse supernovae (CCSNe) are the extremely energetic deaths of
massive stars. They play a vital role in the synthesis and dissemination of
many heavy elements in the universe. In the past, CCSN nucleosynthesis
calculations have relied on artificial explosion methods that do not adequately
capture the physics of the innermost layers of the star. The PUSH method,
calibrated against SN1987A, utilizes the energy of heavy-flavor neutrinos
emitted by the proto-neutron star (PNS) to trigger parametrized explosions.
This makes it possible to follow the consistent evolution of the PNS and to
ensure a more accurate treatment of the electron fraction of the ejecta. Here,
we present the Iron group nucleosynthesis results for core-collapse supernovae,
exploded with PUSH, for two different progenitor series. Comparisons of the
calculated yields to observational metal-poor star data are also presented.
Nucleosynthesis yields will be calculated for all elements and over a wide
range of progenitor masses. These yields can be immensely useful for models of
galactic chemical evolution.
