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In the late stages of stellar core-collapse, prior to core bounce, electroncaptures on medium-heavy nuclei drive deleptonization and simulations requirethe use of accurate reaction rates. Nuclei with neutron number near $N=50$,just above atomic number $Z=28$, play an important role, but rates used inastrophysical simulations rely primarily on a relatively simple single-stateapproximation. In order to improve the accuracy of astrophysical simulations,experimental data are needed to test the electron-capture rates and to guidethe development of better theoretical models. This work presents the results ofthe $^{86}$Kr($t$,$^{3}$He+$\gamma$) experiment at the NSCL, from which anupper limit for the Gamow-Teller strength up to an excitation energy in$^{86}$Br of 5 MeV is extracted. The derived upper limit for theelectron-capture rate on $^{86}$Kr indicates that the rate estimated throughthe single-state approximation is too high and that rates based on Gamow-Tellerstrengths estimated in shell-model and QRPA calculations are more accurate. TheQRPA calculations tested in this manner were used for estimating the electroncapture rates for 78 isotopes near $N=50$ and above $Z=28$. The impact of usingthese new electron-capture rates in simulations of supernovae instead of therates based on the single-state approximation is investigated, indicating asignificant reduction in the deleptonization that affects multi-messengersignals, such as the emission of neutrinos and gravitational waves.

physical review. c

Constraints for stellar electron-capture rates on $^{86}$Kr via the  $^{86}$Kr($t$,$^{3}$He$+\gamma$)$^{86}$Br reaction and the implications for  core-collapse supernovae