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Predictions for the hydrogen-free ejecta of pulsational pair-instability supernovae

Renzo, M.; Farmer, R.; Justham, S.; Gotberg, Y.; de Mink,. S. E.; Zapartas, E.; Marchant, P.; Smith, N.

Numerical results of the simulations presented in []

Models are named as MASS_ZX.tar.gz, where MASS is the initial He core mass in solar mass units, and X is the metallicity of the models. H-rich140.tar.gz contains the files for the H-rich model of appendix B.

Each tarball contains the history file, a few MESA profile saved at specific evolutionary phases (before turning on the hydro in MESA at each pulse and at the onset of core-collapse), and the file which contains the properties of the ejecta at the time they first become faster than the escape velocity. These can be used as input in CSM simulations. We also provide the input files to reproduce each model in the corresponding tarball, and template input files at

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Models will be accessible upon publication of the article

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