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2 results for “Compact object coalescence”
Data set from: Rates of Compact Object Coalescences
<p><strong>Data from: Rates of Compact Object Coalescence </strong></p> <p><strong>Brief overview: </strong><br> This Zenodo entry contains the data that has been used to make the figures for the living review <a href="https://ui.adsabs.harvard.edu/abs/2021arXiv210714239M/abstract">"Rates of Compact Object Coalescence" by Ilya Mandel & Floor Broekgaarden (2021)</a>. 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 <a href="https://github.com/FloorBroekgaarden/Rates_of_Compact_Object_Coalescence">https://github.com/FloorBroekgaarden/Rates_of_Compact_Object_Coalescence</a> (the exact jupyter notebook can be found <a href="https://github.com/FloorBroekgaarden/Rates_of_Compact_Object_Coalescence/tree/main/plottingCode/Make_figures_Mandel_and_Broekgaarden_2021_COC_rates_review.ipynb">here</a>)</p> <p>For any suggestions, questions or inquiry, please email one, or both, of the authors: </p> <ul> <li><strong>Ilya Mandel</strong>: <em>ilya.mandel@monash.edu</em> </li> <li><strong>Floor Broekgaarden</strong>: <em>floor.broekgaarden@cfa.harvard.edu</em></li> </ul> <p>We very much welcome suggestions for additional/missing literature with rate predictions or measurements. </p> <p> </p> <p><strong>Extra figures:</strong><br> Extra figures that can be used can be found here:</p> <p><strong>Vertical figures: <a href="https://docs.google.com/presentation/d/1GqJ0k2zpnxBGwIYNeQ0BfsLSU7H2942gspL-PN_iaJY/edit?usp=sharing">https://docs.google.com/presentation/d/1GqJ0k2zpnxBGwIYNeQ0BfsLSU7H2942gspL-PN_iaJY/edit?usp=sharing</a> </strong></p> <p><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. </p> <p><strong>Reference</strong><br> If you use this data/code for publication, please cite both the paper: <a href="https://ui.adsabs.harvard.edu/abs/2021arXiv210714239M/abstract">Mandel & Broekgaarden (2021)</a> (<a href="https://ui.adsabs.harvard.edu/abs/2021arXiv210714239M/abstract">https://ui.adsabs.harvard.edu/abs/2021arXiv210714239M/abstract</a>) and the dataset on Zenodo through it's doi (see tabs on the right of this zenodo entry) <br> <br> <strong>Details datafiles: </strong></p> <p>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: </p> <p> </p> <ul> <li><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> </li> <li><strong>COC_rates_supplementary_material.pdf </strong> # PDF document describing how the rates are retrieved and quoted rom each study<br> </li> <li><strong>BH-BH_rates_CHE.csv</strong> # BH-BH rates for chemically homogeneous evolution </li> <li><strong>BH-BH_rates_flybys.csv </strong> # BH-BH rates for formation from wide isolated binaries with dynamical interactions from flybys</li> <li><strong>BH-BH_rates_globular-clusters.csv</strong> # BH-BH rates for dynamical formation in globular clusters </li> <li><strong>BH-BH_rates_isolated-binary-evolution.csv</strong> # BH-BH rates for isolated binary evolution </li> <li><strong>BH-BH_rates_nuclear-clusters.csv</strong> # BH-BH rates for (dynamical )formation in (active) nuclear star clusters</li> <li><strong>BH-BH_rates_observations-GWs.csv</strong> # BH-BH rates for observations from gravitational waves</li> <li><strong>BH-BH_rates_population-III.csv</strong> # BH-BH rates for population-III stars </li> <li><strong>BH-BH_rates_primordial.csv </strong> # BH-BH rates for primordial formation</li> <li><strong>BH-BH_rates_triples.csv</strong>. # BH-BH rates for formation in (hierarchical) triples </li> <li><strong>BH-BH_rates_young-stellar-clusters.csv</strong> # BH-BH rates for dynamical formation in young/open star clusters <br> </li> <li><strong>NS-BH_rates_CHE.csv</strong> # NS-BH rates for chemically homogeneous evolution </li> <li><strong>NS-BH_rates_flybys.csv </strong> # BH-BH rates for formation from wide isolated binaries with dynamical interactions from flybys</li> <li><strong>NS-BH_rates_globular-clusters.csv</strong> # NS-BH rates for dynamical formation in globular clusters </li> <li><strong>NS-BH_rates_isolated-binary-evolution.csv. </strong># NS-BH rates for isolated binary evolution </li> <li><strong>NS-BH_rates_nuclear-clusters.csv</strong> # NS-BH rates for (dynamical )formation in (active) nuclear star clusters</li> <li><strong>NS-BH_rates_observations-GWs.csv</strong> # NS-BH rates for observations from gravitational waves</li> <li><strong>NS-BH_rates_population-III.csv</strong> # NS-BH rates for population-III stars </li> <li><strong>NS-BH_rates_triples.csv</strong> # NS-BH rates for formation in (hierarchical) triples </li> <li><strong>NS-BH_rates_young-stellar-clusters.csv</strong> # BH-BH rates for dynamical formation in young/open star clusters<br> </li> <li><strong>NS-NS_rates_globular-clusters.csv </strong># NS-NS rates for dynamical formation in globular clusters </li> <li><strong>NS-NS_rates_isolated-binary-evolution.csv </strong> # NS-NS rates for isolated binary evolution </li> <li><strong>NS-NS_rates_nuclear-clusters.csv </strong># NS-NS rates for (dynamical )formation in (active) nuclear star clusters</li> <li><strong>NS-NS_rates_observations-GWs.csv</strong> # NS-NS rates for observations from gravitational waves</li> <li><strong>NS-NS_rates_observations-kilonovae.csv</strong> # NS-NS rates for observations from kilonovae</li> <li><strong>NS-NS_rates_observations-pulsars.csv</strong> # NS-NS rates for observations from Galactic pulsars</li> <li><strong>NS-NS_rates_observations-sGRBs.csv </strong># NS-NS rates for observations short gamma-ray bursts</li> <li><strong>NS-NS_rates_triples.csv </strong># NS-NS rates for formation in (hierarchical) triples </li> <li><strong>NS-NS_rates_young-stellar-clusters.csv</strong> # NS-NS rates for dynamical formation in young/open star clusters </li> </ul> <p> </p> <p><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). </p> <p>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). </p> <p> </p>
Observation of Gravitational Waves from the Coalescence of a 2.5-4.5 Msun Compact Object and a Neutron Star --- Data Release
<p>This data release contains the analysis results and data behind the figures of the GW230529 discovery paper (<a href="https://urldefense.com/v3/__https://dcc.ligo.org/LIGO-P2300352/public/__;!!Dq0X2DkFhyF93HkjWTBQKhk!W4i4x3JfGgemcFsnnEYP5qxiknddvrG1LWpTLjs_JGK907kTrEBkS8o6i5T6RUFMX0v04jCPhtTq9K2SLcv_4g$" target="_blank" rel="nofollow noreferrer noopener">https://dcc.ligo.org/LIGO-P2300352/public/</a>). Strain data for this event (the L1:GDS-CALIB_STRAIN_CLEAN_AR channel) can be downloaded on GWOSC (<a href="https://doi.org/10.7935/6k89-7q62" target="_blank" rel="noopener">https://doi.org/10.7935/6k89-7q62</a>).</p> <p>The PESummary metafile containing the parameter estimation posterior samples for all analyses performed in the paper (<strong>posterior_samples.h5</strong>) and skymap fits file (<strong>skymap_combined_PHM_high_spin.fits</strong>) for the preferred parameter estimation analysis (high-spin, combined samples using binary black hole waveforms) can be downloaded directly as individual files.</p> <p>The other analysis results are grouped by type: rates, populations, searches, and tidal. The <strong>figure_scripts.tar.gz</strong> file contains all the paper figures in jpeg format along with a Jupyter notebook to reproduce them and additional required helper scripts. Example code for working with the individual result files is given in the <strong>PaperPlots.ipynb</strong> notebook included in this tar file.</p> <p>In brief, the <strong>rates.tar.gz</strong> file contains two files that each include a subset of the rates probability distributions shown in Fig. 3 of the paper. The <strong>populations.tar.gz</strong> file contains all the data behind Figs. 4-8, with subdirectories for each of the three population analyses considered in the paper: Binned Gaussian Process, NSBH-pop, and Power-Law + Dip + Break. In addition to the data behind the figures, the Power-Law + Dip + Break subdirectory additionally includes two *result.json files for the hyper-parameter posterior samples. These files have the same format as the corresponding NSBH-pop *result.json files and can be manipulated in the same way, as shown in the figures notebook.</p> <p>The <strong>searches.tar.gz</strong> file contains the data behind Figs. 9-11 for each of the three search pipelines whose results are included in the paper. Finally, the <strong>tidal.tar.gz</strong> file contains the four probability distributions plotted in Fig. 14. All other figures are produced only using the posterior_samples.h5 file.</p>
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