DOI: 10.5281/zenodo.5072400
title: Data set from: Rates of Compact Object Coalescences

description: <strong>Data from: Rates of Compact Object Coalescence </strong> <strong>Brief overview: </strong><br> This Zenodo entry contains the data that has been used to make the figures for the living review "Rates of Compact Object Coalescence" by Ilya Mandel & Floor Broekgaarden (2021). To reproduce the figures, download all the <strong>*.csv</strong> files and run the jupyter notebook created to reproduce the results in the publicly available Github directory https://github.com/FloorBroekgaarden/Rates_of_Compact_Object_Coalescence (the exact jupyter notebook can be found here) For any suggestions, questions or inquiry, please email one, or both, of the authors: <strong>Ilya Mandel</strong>: <em>ilya.mandel@monash.edu</em> <strong>Floor Broekgaarden</strong>: <em>floor.broekgaarden@cfa.harvard.edu</em> We very much welcome suggestions for additional/missing literature with rate predictions or measurements. <strong>Extra figures:</strong><br> Extra figures that can be used can be found here: <strong>Vertical figures: https://docs.google.com/presentation/d/1GqJ0k2zpnxBGwIYNeQ0BfsLSU7H2942gspL-PN_iaJY/edit?usp=sharing </strong> <br> The authors are currently working on making an interactive tool for plotting the rates that will be available soon. In the mean time, feel free to send requests for plots/figures to the authors. <strong>Reference</strong><br> If you use this data/code for publication, please cite both the paper: Mandel & Broekgaarden (2021) (https://ui.adsabs.harvard.edu/abs/2021arXiv210714239M/abstract) and the dataset on Zenodo through it's doi (see tabs on the right of this zenodo entry) <br> <br> <strong>Details datafiles: </strong> The PDF <strong>COC_rates_supplementary_material.pdf</strong> attached (and in the Github repository) describes how each of the rates in the data files of this Zenodo entry are retrieved. The other 26 files are .csv files, where each csv file contains the rates from one specific double compact object type: NS-NS, NS-BH or BH-BH, and specific rate group (isolated binary evolution, gravitational wave observations etc.). The files in this entry are: <strong>Data_Mandel_and_Broekgaarden_2021.zip </strong>all the files below conveniently in one zip file so that you only have to do 1 download. <br> <strong>COC_rates_supplementary_material.pdf </strong> # PDF document describing how the rates are retrieved and quoted rom each study<br> <strong>BH-BH_rates_CHE.csv</strong> # BH-BH rates for chemically homogeneous evolution <strong>BH-BH_rates_flybys.csv </strong> # BH-BH rates for formation from wide isolated binaries with dynamical interactions from flybys <strong>BH-BH_rates_globular-clusters.csv</strong> # BH-BH rates for dynamical formation in globular clusters <strong>BH-BH_rates_isolated-binary-evolution.csv</strong> # BH-BH rates for isolated binary evolution <strong>BH-BH_rates_nuclear-clusters.csv</strong> # BH-BH rates for (dynamical )formation in (active) nuclear star clusters <strong>BH-BH_rates_observations-GWs.csv</strong> # BH-BH rates for observations from gravitational waves <strong>BH-BH_rates_population-III.csv</strong> # BH-BH rates for population-III stars <strong>BH-BH_rates_primordial.csv </strong> # BH-BH rates for primordial formation <strong>BH-BH_rates_triples.csv</strong>. # BH-BH rates for formation in (hierarchical) triples <strong>BH-BH_rates_young-stellar-clusters.csv</strong> # BH-BH rates for dynamical formation in young/open star clusters <br> <strong>NS-BH_rates_CHE.csv</strong> # NS-BH rates for chemically homogeneous evolution <strong>NS-BH_rates_flybys.csv </strong> # BH-BH rates for formation from wide isolated binaries with dynamical interactions from flybys <strong>NS-BH_rates_globular-clusters.csv</strong> # NS-BH rates for dynamical formation in globular clusters <strong>NS-BH_rates_isolated-binary-evolution.csv. </strong># NS-BH rates for isolated binary evolution <strong>NS-BH_rates_nuclear-clusters.csv</strong> # NS-BH rates for (dynamical )formation in (active) nuclear star clusters <strong>NS-BH_rates_observations-GWs.csv</strong> # NS-BH rates for observations from gravitational waves <strong>NS-BH_rates_population-III.csv</strong> # NS-BH rates for population-III stars <strong>NS-BH_rates_triples.csv</strong> # NS-BH rates for formation in (hierarchical) triples <strong>NS-BH_rates_young-stellar-clusters.csv</strong> # BH-BH rates for dynamical formation in young/open star clusters<br> <strong>NS-NS_rates_globular-clusters.csv </strong># NS-NS rates for dynamical formation in globular clusters <strong>NS-NS_rates_isolated-binary-evolution.csv </strong> # NS-NS rates for isolated binary evolution <strong>NS-NS_rates_nuclear-clusters.csv </strong># NS-NS rates for (dynamical )formation in (active) nuclear star clusters <strong>NS-NS_rates_observations-GWs.csv</strong> # NS-NS rates for observations from gravitational waves <strong>NS-NS_rates_observations-kilonovae.csv</strong> # NS-NS rates for observations from kilonovae <strong>NS-NS_rates_observations-pulsars.csv</strong> # NS-NS rates for observations from Galactic pulsars <strong>NS-NS_rates_observations-sGRBs.csv </strong># NS-NS rates for observations short gamma-ray bursts <strong>NS-NS_rates_triples.csv </strong># NS-NS rates for formation in (hierarchical) triples <strong>NS-NS_rates_young-stellar-clusters.csv</strong> # NS-NS rates for dynamical formation in young/open star clusters <strong>Each csv file contains the following header: </strong><br> ADS year # year of the paper in the ADS entry<br> ADS month # month of the paper in the ADS entry <br> ADS abstract link # link to the ADS abstract <br> ArXiv link # link to the ArXiv version of the paper <br> First Author # name of the first author<br> label string # label of the study, that corresponds to the label in the figure<br> code (optional) # name of the code used in this study <br> type of limit (for plotting, see jupyter notebook for a dictionary) # integer, that is used to map to a certain limit visualization in the plot (e.g. scatter points vs upper limit). Each entry takes two columns in the csv files. One for the rates (quoted under the header 'rate [Gpc^-3 yr^-1]') and one for "notes" where we sometimes added notes about the rates (such as whether it is an upper or lower limit).
description: Version 7 has fixed a few small typos from version 6, and has the flybys channel in a separate csv file and class version 6 includes the following changes: - Updated GWTC-3 BHBH, NSBH and NSNS rates with latest version population paper - Kinugawa et al. (2020) -&gt; changed to Kinugawa et al. (2021) and updated the rates (we accidentaly quoted the wrong rates from the wrong paper) - Added Nuclear star cluster dynamics, with SMBH from Fragione et al. (2019) for BHBH, NSBH, and NSNS rates - Boekholt et al. (2022) added under AGN rates - added Stegmann (2022) to triple channels - added Olejek (2022) - Added Raveh et al. (2022) - added Zevin et al. (2022) - added Codazzo et al (2022) - added Michaely & Naoz (2022) - added Briel et al. (2022) - added Dorozsmai and Toonen (2022) Version 5 [used for published version of Living Reviews in relativity] has small changes in some of the label names, and has removed the Mandhai 2018 rates since these authors quote SGRB rates and not BNS rates. Version 4 has additional rates from recent papers and is updated to include the GWTC-3 results 11/19/21. This is the version that was used for the re-submitted paper. Version 3 has additional rates that we added after receiving useful feedback from the community (post ArXiv submission) Version 2 has updated and additional rates that we added. Version of the data that was used for the first ArXiv submission.