  We provide yields from 189 neutrino-driven core-collapse supernova (CCSN)
simulations covering zero-age main sequence masses between 11 and 75 solar
masses and three different metallicities. Our CCSN simulations have two main
advantages compared to previous methods used for applications in Galactic
chemical evolution (GCE). Firstly, the mass cut between remnant and ejecta
evolves naturally. Secondly, the neutrino luminosities and thus the electron
fraction are not modified. Both is key to obtain an accurate nucleosynthesis.
We follow the composition with an in-situ nuclear reaction network including
the 16 most abundant isotopes and use the yields as input in a GCE model of the
Milky Way. We adopt a GCE which takes into account infall of gas as well as
nucleosynthesis from a large variety of stellar sources. The GCE model is
calibrated to reproduce the main features of the solar vicinity. For the CCSN
models, we use different calibrations and propagate the uncertainty. We find a
big impact of the CCSN yields on our GCE predictions. We compare the abundance
ratios of C, O, Ne, Mg, Si, S, Ar, Ca, Ti, and Cr with respect to Fe to an
observational data set as homogeneous as possible. From this, we conclude that
at least half of the massive stars have to explode to match the observed
abundance ratios. If the explosions are too energetic, the high amount of iron
will suppress the abundance ratios. With this, we demonstrate how GCE models
can be used to constrain the evolution and deaths of massive stars.
