The role of collision speed, cloud density, and turbulence in the formation of young massive clusters via cloud-cloud collisions

This repository contains the essential unprocessed data to recreate the results in this paper (10.1093/mnras/staa2857; Liow and Dobbs 2020), which contains the following directories:

initial_conditions

• This directory contains the initial condition dumpfiles. There are 24 main models in this paper. They are named XY_abc, where 'X' is either 'B', 'C', or 'D', representing low, standard, and high initial cloud density respectively; 'Y' is either '1' or '2', representing low and high turbulence; 'abc' is a three-digit number representing the collision Mach number.
• Additional models in appendices have prefixes attached to the filenames. The prefixes are either 'R' (resolution test models; Appendix A), 'T' (random turbulent seeds models; Appendix B), or 'M' (massive clouds models; Appendix D). The value after 'R' shows the number of SPH particles used, a.k.a. resolution.
• The dumpfiles were produced using PHANTOM v1.3.0 (Price et al. 2018; https://phantomsph.bitbucket.io/) in binary format and can be visualised using SPLASH v2.8.0 (Price 2007; https://splash-viz.readthedocs.io/en/latest/intro.html) with code units 100,000 MSun and 10 pc. 

ten_percents 

• This directory contains the dumpfiles at t_10%, the time when 10% of the gas mass is converted to sink mass. Most analysis in the paper was done at this snapshot. They can be visualised using SPLASH similar to the initial condition dumpfiles.

ev_files

• This directory contains ASCII files that track the global properties (energies, total linear/angular momentum, etc) throughout the simulation. The suffixes '_0?' right before '.ev', not relevant to the analysis, show the number of times the simulations were continued. 

all_turbulent_fields

• This directory contains turbulent fields used in most models ('turb001' and 'turb002') and in the random turbulent seed models (otherwise), written in binary format. See 'README' for the random seeds used, and 'velfield.f' for the code to generate the turbulent fields.

Not included in this repository are the intermediate dumpfiles and the sink particle data, but the data shown in this repository is sufficient to reproduce the time and snapshots in the paper. Post-processed data (e.g. global star formation rates, sink particle information at t_10% and other specific snapshots) and results are not included here to preserve data authenticity.

Readers are welcome to contact the authors for the post-processed data and more information.