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7 results for “Gravitational Wave Background”
KDE Representations of the Gravitational Wave Background Free Spectra Present in the NANOGrav 15-Year Dataset
<p><i><strong>OVERVIEW</strong></i></p><p><i><strong>----------------</strong></i></p><p>This is a downloadable file of probability densities from KDEs (Kernel Density Estimator) of free spectrum analyses of the NANOGrav 15yr Dataset (DOI <a href="https://doi.org/10.5281/zenodo.7967584">10.5281/zenodo.7967584</a>) that can be used with the <a href="https://github.com/astrolamb/ceffyl">Ceffyl</a> and <a href="https://github.com/andrea-mitridate/PTArcade">PTArcade</a> packages. Please see the GitHub page for Ceffyl/PTArcade installation details and usage information.<br><br>Details on how this data product was produced can be found in <a href="https://journals.aps.org/prd/abstract/10.1103/PhysRevD.108.103019"><i>Lamb, Taylor & van Haasteren 2023 (DOI 10.1103/PhysRevD.108.103019).</i></a></p><p><i><strong>DIRECTORY AND FILE STRUCTURE</strong></i></p><p><i><strong>----------------------------------------------------</strong></i></p><p>Each directory contains a file with log-pdfs representing their corresponding free spectra (`density.npy`), the frequencies at which they were analysed (`freqs.npy`), the grid-points at which each log-pdf was computed (`log10rhogrid.npy`), frequency labels (`log10rholabels.txt`), analysis label (`pulsar_list.txt`), an array of bandwidths computed using the Sheather-Jones method (see Lamb et al. 2023; 'bandwidths.npy'), and a file with some metadata about the data (`log.txt`).</p><p>./30f_fs{cp}_ceffyl </p><ul><li>A representation of a 30 frequency CURN free spectrum.</li></ul><p>./30f_fs{hd}_ceffyl</p><ul><li>A representation of a 30 frequency HD-correlated free spectrum</li></ul><p>./30f_fs{hd+mp+dp}_ceffyl_hd-only</p><ul><li>A representation of an analysis that simultaneously modeled a HD-correlated free spectrum, a MP-correlated free spectrum, and a DP-correlated free spectrum. Only the HD component is represented here.</li></ul><p>./30f_fs{hd+mp+dp+cp}_ceffyl_hd-only</p><ul><li>A representation of an analysis that simultaneously modeled a HD-correlated free spectrum, a MP-correlated free spectrum, a DP-correlated free spectrum, and a CURN free spectrum. Only the HD component is represented here.</li></ul><p>./README</p><ul><li>this is a readme</li></ul><p><i><strong>SOFTWARE</strong></i></p><p><i><strong>------------------</strong></i></p><p>This data should ideally be used with the latest versions of:</p><ul><li><i><strong>ceffyl</strong></i> (https://github.com/astrolamb/ceffyl)</li><li><i><strong>PTArcade </strong></i>(https://github.com/andrea-mitridate/PTArcade)</li></ul><p><i><strong>PLANNED REVISIONS</strong></i></p><p><i><strong>---------------------------------</strong></i></p><p>None</p><p><i><strong>CHANGE LOG</strong></i></p><p><i><strong>----------------------</strong></i></p><p>10/12/2023 - updated KDE representations</p><p>A bug was found that produced a poor reflection at the lower prior boundary. Hence, data was being represented well at the lower prior boundary. This has now been corrected.</p>
Comparing recent PTA results on the nanohertz stochastic gravitational wave background - full noise and GWB parameter comparison plots
<p>A full collection of plots comparing the noise properties of individual pulsars and gravitational wave background parameters discussed in the companion paper <em>Comparing recent PTA results on the nanohertz stochastic gravitational wave background</em> (IPTA 2024).</p> <p><code>Section4_GWB_comparison.zip</code> supplements and expands section 4.1, "Comparing the published GWB measurements," of IPTA (2024). It contains parameter difference distributions for GWB model parameters. There are four different models included. The HD correlated powerlaw (PL) model make up the basis for Figure 2. Additionally, there are three comparisons not included in IPTA (2024). First, comparisons the common uncorrelated red noise (CURN) PL model are included. Finally, comparisons of two free spectral (FS) models (HD and CURN) are included. These comparisons fit the HD and CURN FS posteriors using the <code>ceffyl</code> software package, and then compare the parameters of the resulting powerlaw fits.</p> <p><code>Section5_Noise_comparison.zip</code> supplements section 5, "Comparing Pulsar Noice Properties," of IPTA (2024). It contains plots for 27 pulsars timed by more than one PTA collaboration, including the plots for PSR J1012+5307, which are presented in Figure 7. The plots include noise parameter posteriors, time domain GP realizations, TOA residuals, and TOA radio frequency.</p>
Dataset from "More accurate gravitational wave backgrounds from cosmic strings"
<p>This file contains data tables representing gravitational wave backgrounds (GWBs) produced by Nambu-Goto cosmic strings evolved under numerical gravitational backreaction. The GWBs were produced using the methodology of "More accurate gravitational wave backgrounds from cosmic strings" [to appear], by the same authors as this dataset.</p> <p>The file is organized in three columns:</p> <ol> <li>The base-10 logarithm of the string coupling to gravity, G\mu. The range is from -8 to -22 in steps of -0.1.</li> <li>The frequency in Hz, f. The range is from 10^(-12) Hz to 10^5 Hz in multiplicative steps of 10^(0.01).</li> <li>The critical energy density fraction in gravitational waves scaled by the dimensionless Hubble constant squared, \Omega_{gw} h^2.</li> </ol>
Mass-redshift dependency of Supermassive Black Hole Binaries for the Gravitational Wave Background
<p>These show the posterior distributions as supplementary material for arXiv:2305.18293 and doi:10.1093/mnras/stae1219</p> <p>The corner plots for the complete 20 parameters with amplitudes hc = 0.5e-15, 1e-15, 2e-15, 3e-15, and 4e-15 for both circular and eccentric population of SMBHBs are presented in the 'free_parameters' folder.</p> <p>The corner plots for the 16 parameters with amplitudes hc = 0.5e-15, 2e-15, and 4e-15 for both circular and eccentric population of SMBHBs using the fitted BH-bulge mass parameters from the simulations can be found in the 'simulation_parameters' folder.</p> <p>The posterior distributions are shown as black contours, while the prior distributions are denoted by light green lines. The top right inlay figure shows the median and central 2sigma range of the recovered characteristic spectrum, where the 5 points denote the frequency bins of 1/(25years), 2/(25years), 3/(25years), 4/(25years) and 5/(25years), which are used as the input data for the Bayesian analysis. To guide the eye the analytic sensitivity curve from the IPTA DR2 is also plotted.</p>
Data Release: "A New Probe of Gravitational Parity Violation Through (Non-)Observation of the Stochastic Gravitational-Wave Background"
<p>This dataset contains the results presented in "<strong>A New Probe of Gravitational Parity Violation Through (Non-)Observation of the Stochastic Gravitational-Wave Background</strong>" (<a href="https://arxiv.org/abs/2312.12532">arXiv:2312.12532</a>).</p> <p>The code used to generate this data can be found in the repository <a href="https://github.com/tcallister/stochastic-birefringence/">https://github.com/tcallister/stochastic-birefringence/</a>. This repository includes <a href="https://github.com/tcallister/stochastic-birefringence/tree/main/data">jupyter notebooks</a> that can be used to open, explore, and plot the files contained in this data set. Additional information about reproducing and/or using this dataset can be found in <a href="https://tcallister.github.io/stochastic-birefringence/">our associated documentation</a>.</p> <p>Further notes:</p> <ul> <li>The file <em>o1o2o3_mass_c_iid_mag_iid_tilt_powerlaw_redshift_result.json</em>, used for figure generation, was published by the LIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration in support of the paper "<a href="https://arxiv.org/abs/2111.03634">The population of merging compact binaries inferred using gravitational waves through GWTC-3</a>" (see <a href="../record/5655785">https://zenodo.org/record/5655785</a>).</li> <li>The file <em>matlab_orfs.dat</em> is created via running the script <a href="https://github.com/tcallister/stochastic-birefringence/blob/main/input/generate_matlab_orfs.m">generate_matlab_orfs.m</a>, which requires a local installation of LIGO matapps tools to rerun.</li> </ul>
Data release: "The metallicity dependence and evolutionary times of merging binary black holes: Combined constraints from individual gravitational-wave detections and the stochastic background"
<p>This data release contains the data to reproduce the results of "<strong>The metallicity dependence and evolutionary times of merging binary black holes: Combined constraints from individual gravitational-wave detections and the stochastic background</strong>" (<a href="https://arxiv.org/abs/2310.17625">arXiv:2310.17625</a>, published version <a href="https://iopscience.iop.org/article/10.3847/1538-4357/ad3d5c">here</a>).</p> <p>The code that was used to generate this data can be found on <a href="https://github.com/kevinturbang/bbh_gwb_time_delay_inference">this GitHub repository</a>. Jupyter notebooks to reproduce the figures of the paper are also included, and can be found <a href="https://github.com/kevinturbang/bbh_gwb_time_delay_inference/tree/main/figures">here</a>.</p>
KDE Representations of the Gravitational Wave Background Free Spectra Present in the NANOGrav 12.5-Year Dataset
<p><em><strong>OVERVIEW</strong></em></p> <p><em><strong>----------------</strong></em></p> <p>This is a downloadable file of probability densities from KDEs (Kernel Density Estimator) of the CRN free spectrum analysis of the <a href="https://nanograv.org/science/data/125-year-pulsar-timing-array-data-release">NANOGrav 12.5yr Dataset</a> that can be used with the <a href="https://github.com/astrolamb/ceffyl">Ceffyl</a> and <a href="https://github.com/andrea-mitridate/PTArcade">PTArcade</a> packages. Please see the GitHub page for Ceffyl/PTArcade installation details and usage information.<br><br>Details on how this data product was produced can be found in <a href="https://journals.aps.org/prd/abstract/10.1103/PhysRevD.108.103019"><em>Lamb, Taylor & van Haasteren 2023 (DOI 10.1103/PhysRevD.108.103019).</em></a></p> <p><em><strong>DIRECTORY AND FILE STRUCTURE</strong></em></p> <p><em><strong>----------------------------------------------------</strong></em></p> <p>The directory `ng12p5_ceffyl` contains a file with log-pdfs representing their corresponding free spectra (`density.npy`), the frequencies at which they were analysed (`freqs.npy`), the grid-points at which each log-pdf was computed (`log10rhogrid.npy`), frequency labels (`log10rholabels.txt`), analysis label (`pulsar_list.txt`), an array of bandwidths computed using the Sheather-Jones method (see Lamb et al. 2023; 'bandwidths.npy'), and a file with some metadata about the data (`log.txt`).</p> <p>Note: there are two copies of `ng12p5_ceffyl` in here by accident! Both are correct versions.</p> <p>The free spectrum was ran with a 30 frequency common uncorrelated free spectrum model (CRN FS) and a 30 frequency intrinsic red noise. <a href="https://nanograv.org/science/data/125-year-stochastic-gravitational-wave-background-search">The free spectrum can be found here</a>.</p> <p><em><strong>SOFTWARE</strong></em></p> <p><em><strong>------------------</strong></em></p> <p>This data should ideally be used with the latest versions of:</p> <ul> <li><em><strong>ceffyl</strong></em> (https://github.com/astrolamb/ceffyl)</li> <li><em><strong>PTArcade </strong></em>(https://github.com/andrea-mitridate/PTArcade)</li> </ul> <p><em><strong>PLANNED REVISIONS</strong></em></p> <p><em><strong>---------------------------------</strong></em></p> <p>None</p> <p><em><strong>CHANGE LOG</strong></em></p> <p><em><strong>----------------------</strong></em></p> <p>16/01/2024 - updated KDE representations</p> <p>A bug was found that produced a poor reflection at the lower prior boundary. Hence, data was being represented well at the lower prior boundary. This has now been corrected.</p>
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