Grouped star formation: converting sink particles to stars in hydrodynamical simulations

<p>This repository contains the essential raw data and codes to recreate the plots&nbsp;in this paper (10.1093/mnras/stab3617; <a href="https://ui.adsabs.harvard.edu/abs/2022MNRAS.510.2657L/abstract">Liow et al. 2022</a>), which contains the following directories and codes:</p> <p><strong>B12/</strong></p> <ul> <li>This directory contains the initial condition (or the snapshot right before star formation) and the snapshot at 0.19&nbsp;Myr for all the sub-parsec-scale isolated cluster models (see Sections 2.3.1 and 3.1). The only exception is the B12/B12/ subdirectory, which contains the sink particles at 0.19 Myr from the original simulation (Bate 2012).&nbsp;</li> <li>The gas, sink and star files were produced using AMUSE v2021.6.0 (Portegies Zwart et al. 2021; <a href="https://zenodo.org/record/4946130">https://zenodo.org/record/4946130</a>), while the random state and setting files were created using Ekster v1.01 (Rieder and Liow 2021; <a href="https://zenodo.org/record/5520944">https://zenodo.org/record/5520944</a>). See Ekster for more information on how to run the code.</li> </ul> <p><strong>L20/&nbsp;</strong></p> <ul> <li>This directory contains the initial condition (or the snapshot right before star formation) and the snapshot at 1.75&nbsp;Myr for all the parsec-scale cloud-cloud collision models (see Sections 2.3.2&nbsp;and 3.2). The only exception is the L20/L20/ subdirectory, which contains the sink particles at 1.75&nbsp;Myr from the original simulation (Liow and Dobbs 2020).&nbsp;</li> </ul> <p><strong>J+/</strong></p> <ul> <li>This directory contains the stars at 5 Myr, and stars and sinks at 20 Myr for all the parsec-scale isolated cluster models (see Sections 2.3.3&nbsp;and 3.3). The only exception is the J+/J+/ subdirectory, which contains the sink particles at 5 Myr and at 20 Myr from the original simulation (Jaffa et al. 2022).</li> </ul> <p><strong>R+/</strong></p> <ul> <li>This directory contains the stars at 1.80 Myr and at 2.40 Myr for the kilo-parsec-scale spiral arm model (see Sections 2.3.4 and 3.4).</li> </ul> <p><strong>L20_Extra/</strong></p> <ul> <li>This directory contains the initial condition (or the snapshot right before star formation) and the snapshot at 1.75&nbsp;Myr for all the additional parsec-scale cloud-cloud collision models to study the effect of changing random seeds on cluster properties (see Section 4.1).</li> </ul> <p><strong>B12_VG/</strong></p> <ul> <li>This directory contains the initial condition (or the snapshot right before star formation) and the snapshot at 0.19&nbsp;Myr for all the additional sub-parsec-scale isolated cluster models to study the effect of varying upper star mass limits (see Section 4.2).</li> </ul> <p><strong>L20_VG/</strong></p> <ul> <li>This directory contains the initial condition (or the snapshot right before star formation) and the snapshot at 1.75 Myr for all the additional parsec-scale cloud-cloud collision models&nbsp;to&nbsp;study the effect of varying upper star mass limits (see Section 4.2).</li> </ul> <p><strong>misc/</strong></p> <ul> <li>This directory contains the miscellaneous files to produce some of the plots in the paper.&nbsp;</li> </ul> <p><strong>load_data.py</strong></p> <ul> <li>This python code loads the necessary sink and star files for the code &#39;plot.py&#39;.&nbsp;</li> </ul> <p><strong>plot.py</strong></p> <ul> <li>This python code recreates the plots in the paper. See individual functions for more information.</li> </ul> <p>Please contact the authors&nbsp;for&nbsp;more information.</p>