DOI: 10.5281/zenodo.5178776
title: BHNS simulations from: Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Mergers

description: The data for all <strong>BHNS </strong>simulations shown in<em><strong> "Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Mergers". </strong>Broekgaarden et al. (2021, submitted, preprint: https://arxiv.org/abs/2112.05763)</em> <strong>Contents: </strong> <strong>18 zip files that each contain an hdf5 file with the raw data for one of the simulations from Table 1 in the paper. The only exception is the fiducial.zip file and the unstableCaseBB.zip file, which contain both the fiducial (model A) and 'optimistic CE' (model K) data file and the "unstable case BB" (model E) and "unstable case BB + optimistic CE" (model F) files.</strong><br> <strong>These zip files are: </strong> <em>fiducial.zip, </em> the Fiducial model (A) and Optimistic CE model (K) <em>massTransferEfficiencyFixed_0_25.zip, </em>the \(\beta\) = 0.25 model (B) <em>massTransferEfficiencyFixed_0_5.zip</em>, the \(\beta\) = 0.5 model (C) <em>massTransferEfficiencyFixed_0_75.zip,</em> the \(\beta\) = 0.75 model (D) <em>unstableCaseBB.zip, </em>the unstable case BB mass transfer model (E) and unstable case BB & optimistic CE model (F) <em>alpha0_1 zip</em>, the \(\alpha = 0.1\) model (G) <em>alpha0_5.zip</em>, the \(\alpha = 0.5\) model (H) <em>alpha2_0.zip</em>, the \(\alpha = 2.0\) model (I) <em>alpha10_0.zip</em>, the \(\alpha = 10.0\) model (J) <em>rapid.zip</em>, the rapid SN model (L) <em>maxNSmass2_0.zip, </em>the max \(m_{\rm{NS}} = 2\, \rm{M}_{\odot}\) model (M) <em>maxNSmass3_0.zip, </em>the max \(m_{\rm{NS}} = 3\, \rm{M}_{\odot}\) model (N) <em>noPISN.zip</em>, the no PISN model (O) <em>ccSNkick_100km_s.zip, </em>the \(\sigma_{\rm{cc}}\)= 100 km/s model (P) <em>ccSNkick_30km_s.zip, </em>the \(\sigma_{\rm{cc}}\)= 30 km/s model (Q) <em>noBHkick.zip, </em>the no BH SN kick model (R) <em>wolf_rayet_multiplier_0_1.zip, </em>the model with Wolf-Rayet wind factor \(f_{\rm{WR}} = 0.1\) (S) <em>wolf_rayet_multiplier_5.zip, </em>the model with Wolf-Rayet wind factor \(f_{\rm{WR}} = 5\) (T)<br> <br> 2 more zip files containing csv files with the summarized rates to create Figures 1, 2 and 3, which do not require downloading the entire dataset, but instead use these csv files with the summarized rates: <strong>csvFilesForFigure1_DCOpaper.zip </strong># contains the files to recreate figure 1 with the merger rates per metallicity for BH-BH, BH-NS and NS-NS: formationRatesTotalAndPerChannel_BHBH_.csv formationRatesTotalAndPerChannel_BHNS_.csv formationRatesTotalAndPerChannel_NSNS_.csv <strong>csvFilesForFigure2_and_3_DCOpaper.zip </strong># contains the files to recreate figure 2 with the merger rates for intrinsic and GW detection weighted, containing the csv files with names: rates_MSSFR_Models_BHBH_AllDCOsimulation.csv rates_MSSFR_Models_NSNS_AllDCOsimulation.csv rates_MSSFR_Models_BHNS_AllDCOsimulation.csv Details of how to use the data (a readme), as well as scripts to reproduce all results, plots, and figures from the paper are given in the accompanying Github repository https://github.com/FloorBroekgaarden/Double-Compact-Object-Mergers If you use this data, please cite Broekgaarden et al. (2021): see https://ui.adsabs.harvard.edu/abs/2021arXiv211205763B/abstract