Supplementary data for the article Fichtner et al., 2024, A&A, 690, A72

Supplementary data for the paper:
Fichtner Y. A., Mackey J., Grassitelli L., Romano-Díaz E., Porciani C., 2024, A&A, 690, A72, Connecting stellar and galactic scales: Energetic feedback from stellar wind bubbles to supernova remnants, DOI: https://doi.org/10.1051/0004-6361/202449638 

Paper abstract:
Context. Energy and momentum feedback from stars is a key element of models for galaxy formation and interstellar medium dynamics, but resolving the relevant length scales to directly include this feedback remain out of reach of current-generation simulations.
Aims. We aim to constrain the energy feedback by winds, photoionisation and supernovae (SNe) from massive stars.
Methods. We measure the thermal and kinetic energy imparted to the interstellar medium on various length scales, calculated from high-resolution 1D radiation-hydrodynamics simulations. Our grid of simulations covers a broad range of densities, metallicities, and state-of-the-art evolutionary models of single and binary stars.
Results. A single star or binary system can carve a cavity of tens-of-pc size into the surrounding medium. During the pre-SN phase, post-main-sequence stellar winds and photoionisation dominate. While SN explosions dominate the total energy budget, the pre-SN feedback is of great importance by reducing the circumstellar gas density and delaying the onset of radiative losses in the SN remnant. Contrary to expectations, the metallicity dependence of the stellar wind has little effect on the cumulative energy imparted by feedback to the ISM; the only requirement is the existence of a sufficient level of pre-SN radiative and mechanical feedback. The ambient medium density determines how much and when feedback energy reaches to distance >= 10 − 20 pc and affects the division between kinetic and thermal feedback.
Conclusions. Our results can be used as a sub-grid model for feedback in large-scale simulations of galaxies. The results reinforce that the uncertain mapping of stellar evolution sequences to SN explosion energy is very important to determining the overall feedback energy from a stellar population.

General description of the data release:
The data release contains tables with the cumulative flows of kinetic energy, thermal energy, mass and metal mass as a function of time for every simulation presented in the corresponding paper. The cumulative flows are calculated at three different distances from the stellar source (5, 10 and 20 pc). Exemplary parameter files of the simulations and readme files are also included.
The tables could be used in a sub-grid model of stellar feedback to determine the amount of feedback ejecta (mass, metals, thermal and kinetic energy) that can be injected, taking into account the circumstellar medium. It is possible to do so as a function of time, ambient metallicity and ambient density. The data release includes simulations of different stellar models of single and binary stars, making it possible to choose between different stellar populations.
It is also possible to use the data for a comparison to other work.