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In this fourth paper of the series, we use the parametrized, sphericallysymmetric explosion method PUSH to perform a systematic study of two sets ofnon-rotating stellar progenitor models. Our study includes pre-explosion modelswith metallicities Z=0 and Z=Z$_{\odot}\times 10^{-4}$ and covers a progenitormass range from 11 up to 75 M$_\odot$. We present and discuss the explosionproperties of all models and predict remnant (neutron star or black hole) massdistributions within this approach. We also perform systematic nucleosynthesisstudies and predict detailed isotopic yields as function of the progenitor massand metallicity. We present a comparison of our nucleosynthesis results withobservationally derived $^{56}$Ni ejecta from normal core-collapse supernovaeand with iron-group abundances for metal-poor star HD~84937. Overall, ourresults for explosion energies, remnant mass distribution, $^{56}$Ni mass, andiron group yields are consistent with observations of normal CCSNe. We findthat stellar progenitors at low and zero metallicity are more prone to BHformation than those at solar metallicity, which allows for the formation ofBHs in the mass range observed by LIGO/VIRGO.

astrophysical journal/the astrophysical journal

PUSHing core-collapse supernovae to explosions in spherical symmetry IV:  Explodability, remnant properties and nucleosynthesis yields of low  metallicity stars