Progenitors of Type IIb Supernovae: I. Evolutionary Pathways and Rates

Mesa templates and data associated with Sravan et al. (2018). MESA version 9575.

Each tar.xz contains one set of simulations, with files marked as binaries_* and singles_* corresponding to binary star, and single star simulations. Files ending in *high_Z.tar.xz and *low_Z.tar.xz correspond to the high and low metallicity simulations in the paper. for binary runs, the three digits indicate the mass transfer efficiency with 001, 010, 050 and 100 corresponding to efficiencies of 0.01, 0.10, 0.50 and 1.00.

Within the files, simulation results are contained in individual folders, that also include all necessary MESA files to recreate the simulation. For single star simulations, the folder name indicates the value of log10(M_ZAMS/Msun), so for example, the folder named "1.6000" represents a star with ZAMS mass of 39.81 Msun. For binary systems, data is arranged such that, for example, the folder "1.400/0.825_3.000" represents a binary system with a primary mass at ZAMS of log10(M_1,ZAMS/Msun)=1.4, mass ratio q=M_2,ZAMS/M_1,ZAMS=0.825 and initial orbital period log P_i/days=3.

All MESA output files have been post-processed to reduce their size. within each folder, the files named "last_prof*.data.s" contain the structure of the models at the end of a simulation. Files "LOGS/history.data.s", "LOGS1/history.data.s" and "LOGS2/history.data.s" contain information that can be represented by a single number at each timestep, such as the age, luminosity and effective temperature of the star. "LOGS/history.data.s" is used in single star simulations, while "LOGS1/history.data.s" and "LOGS2/history.data.s" correspond to each star in a binary run.