Population synthesis data for the mass distribution of stripped stars

Here we provide the results of our population synthesis model runs used in The Mass Distribution of Stars Stripped in Binaries: The Effect of Metallicity (Hovis-Afflerbach et al. 2025).

The .zip file contains four folders, for the four metallicities modeled in this study. These are Z=0.014, similar to solar metallicity, Z=0.006, similar to the metallicity of the LMC, Z=0.002, similar to the metallicity of the SMC and many galaxies at Cosmic Noon, and Z=0.002, very low metallicity.

Each folder contains 100 files, one for each model run. Each file contains a header including the assumptions made in running the model, and a table with the data. The table has one row for each stripped star present when the run concludes (after 1 Gyr, when the population is in equilibrium), and the following columns:

Evolution: the evolutionary pathway to the creation of this stripped star. This can be either strip_RLOF_MS (stable mass transfer during the Main Sequence), strip_RLOF_HG (stable mass transfer during the Hertzsprung gap), or strip_CEE_HG (common envelope evolution during the Hertzsprung gap).

M1init: the initial mass of the primary star, in units of solar masses.

M2init: the initial mass of the secondary star, in units of solar masses.

star_mass_1: the final stripped star mass of the primary star, in units of solar masses.

Python files to create the figures in the paper from this data, along with instructions for doing so, can be found at https://github.com/berylha/stripped-star-distribution.