2024-03-28T13:23:32Z
https://zenodo.org/oai2d
oai:zenodo.org:6226935
2022-12-09T02:26:32Z
user-nrgw-opendata
Gonzalez, Alejandra
Gamba, Rossella
Breschi, Matteo
Zappa, Francesco
Carullo, Gregorio
Bernuzzi, Sebastiano
Nagar, Alessandro
2022-02-22
<pre>We present data release associated to "Numerical-Relativity-Informed Effective-One-Body model for Black-Hole-Neutron-Star Mergers with Higher Modes and Spin Precession" [1]. The BHNS model in this work is implemented and publicly available in <a href="https://bitbucket.org/eob_ihes/teobresums">TEOBResumS</a>.
</pre>
<p>The analysis of both artificial and real GW data was performed with <a href="https://git.tpi.uni-jena.de/mbreschi/bajes">bajes</a> [2].</p>
<p>[1] A. Gonzalez et al., <strong><em>Numerical-Relativity-Informed Effective-One-Body model for Black-Hole-Neutron-Star Mergers with Higher Modes and Spin Precession</em></strong>, <a href="https://arxiv.org/abs/2212.03909">arXiv:2212.03909</a> [gr-qc]<br>
[2] M.Breschi et. al., <strong><em>Bayesian inference of multimessenger astrophysical data: Methods and applications to gravitational waves</em></strong>, Phys. Rev. D 104 (2021) no.4, 042001, doi:10.1103/PhysRevD.104.042001, <a href="https://arxiv.org/abs/2102.00017">arXiv:2102.00017</a> [gr-qc]</p>
https://doi.org/10.5281/zenodo.6226935
oai:zenodo.org:6226935
eng
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://doi.org/10.5281/zenodo.6226934
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eob
bhns
waveform
GW
Numerical-Relativity-Informed Effective-One-Body model for Black-Hole-Neutron-Star Mergers with Higher Modes and Spin Precession
info:eu-repo/semantics/article
oai:zenodo.org:7081337
2022-09-20T14:26:19Z
user-nrgw-opendata
user-eu
Gamba, Rossella
Breschi, Matteo
Carullo, Gregorio
Rettegno, Piero
Albanesi, Simone
Bernuzzi, Sebastiano
Nagar, Alessandro
2022-09-15
<p>Data release associated to "GW190521 as a dynamical capture of two nonspinning black holes" [1].</p>
<p>The posterior samples have been obtained with bajes [2], a pipeline for gravitational wave (GW) and multimessenger astronomy, publicly available <a href="https://github.com/matteobreschi/bajes">here</a>.</p>
<p>The GW model TEOBResumS [3,4] employed for this analysis is publicly available <a href="https://bitbucket.org/eob_ihes/teobresums/src/master/">here</a>.</p>
<p>[1] R.Gamba et. al., <em>GW190521 as a dynamical capture of two nonspinning black holes</em>, <a href="https://arxiv.org/abs/2106.05575">arxiv:2106.05575</a> [gr-qc]<br>
[2] M.Breschi et. al., <em>Bayesian inference of multimessenger astrophysical data: Methods and applications to gravitational waves</em>, Phys. Rev. D 104 (2021) no.4, 042001, doi:10.1103/PhysRevD.104.042001, <a href="https://arxiv.org/abs/2102.00017">arXiv:2102.00017</a> [gr-qc]<br>
[3] A.Nagar et. al., <em>Effective-one-body waveforms from dynamical captures in black hole binaries, </em>Phys. Rev. D 103 (2021) no.6, 064013, doi:10.1103/PhysRevD.103.064013, <a href="https://arxiv.org/abs/2009.12857">arXiv:2009.12857</a> [gr-qc].<br>
[4] R.Gamba et. al., <em>Effective-one-body waveforms for precessing coalescing compact binaries with post-Newtonian twist</em>, Phys. Rev. D 106 (2022) no.2, 024020, doi:10.1103/PhysRevD.106.024020, <a href="https://arxiv.org/abs/2111.03675">arXiv:2111.03675</a> [gr-qc].</p>
<p> </p>
https://doi.org/10.5281/zenodo.7081337
oai:zenodo.org:7081337
Zenodo
https://arxiv.org/abs/arXiv:2106.05575
https://zenodo.org/communities/nrgw-opendata
https://zenodo.org/communities/eu
https://doi.org/10.5281/zenodo.7081336
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GW190521 as a dynamical capture of two nonspinning black holes
info:eu-repo/semantics/article
oai:zenodo.org:4159620
2020-11-02T12:26:56Z
user-nrgw-opendata
user-eu
Nedora, Vsevolod
Bernuzzi, Sebastiano
Radice, David
Daszuta, Boris
Endrizzi, Andrea
Perego, Albino
Prakash, Aviral
Safarzadeh, Mohammadtaher
Schianchi, Federico
Logoteta, Domenico
2020-10-30
<p>We release outflow data extracted at a fixed coordinate sphere with a radius 294km. <br>
Material unbound according to the geodesic criterion is located in the dir <br>
'dynamical_ejecta/'<br>
Material unbound according to the Bernoulli criterion, computed from the <br>
moment the dynamical ejecta saturates is located in the folder `spiral_wave_wind/`<br>
Part of the `spiral_wave_wind` confined to the polar region, above 60~deg <br>
from the binary plane is located in `neutrino_wind/`</p>
<p>See [1] for more details. See also [2] for more details on 'spiral wave wind' <br>
and [3] for more details on dynamical ejecta.</p>
<p>Included data:</p>
<ul>
<li>`Table1.txt`: Table 1 of the paper in a machine-readable format</li>
<li>`[model].tar`: ejecta data for individual simulations. The name reads as following.<br>
"EOS_GravMassesOfStars_NeutrinoScheme_Viscosity(LK)_Resolution".<br>
Simulations without viscosity do not have LK in their name. <br>
Neutrino scheme is consistent in all simulations and is Leackage+M0.<br>
Resolutions available are: LR, SR, and HR that correspond to 246 m, 158 m and 123 m. </li>
<li>EOS tables used for the evolution (Except BLh which is not public)</li>
</ul>
<p>For each model we provide</p>
<ul>
<li>Initial data generated with LORENE</li>
<li>Parameter file</li>
</ul>
<p>Additionally, we provide ejecta properties (for all ejecta types) as:</p>
<ul>
<li>`total_flux.dat`: angle integrated outflow rate and cumulated ejecta mass.<br>
Time is in seconds, masses are in solar masses.</li>
<li>`hist_entropy.dat`: histogram of the ejecta as a function of the entropy (in kb)</li>
<li>`hist_vel_inf.dat`: histogram of the ejecta as a function of the asymptotic velocity (in units of c)</li>
<li>`hist_Y_e.dat`: histogram of the ejecta as a function of the electron fraction Ye.</li>
<li>`ejecta_profile.dat`: time-integrated ejecta profiles as a function of the polar angle.</li>
<li>`hist_vinf_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.</li>
<li>`corr_Y_e_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.</li>
<li>`ejecta.h5`: histograms of the ejecta as a function of Ye, entropy, and expansion timescale tau.</li>
</ul>
<p>For nucleosynthesis yields from pre-computed parametrized trajectories see [4]</p>
<p>[1] V. Nedora, S. Bernuzzi, D. Radice, B. Daszuta, A. Endrizzi, A. Perego, A. Prakash, M. Safarzadeh, F. Schianchi, D. Logoteta <strong><em>Numerical Relativity Simulations of the Neutron Star Merger GW170817: Long-Term Remnant Evolutions, Winds, Remnant Disks, and Nucleosynthesis</em></strong>, <a href="https://arxiv.org/abs/2008.04333">arXiv:2008.04333</a> <br>
[2] V. Nedora, S. Bernuzzi, D. Radice, A. Perego, A. Endrizzi, N. Ortiz, <strong><em>Spiral-wave wind for the blue kilonova</em></strong>, <a href="https://iopscience.iop.org/article/10.3847/2041-8213/ab5794/pdf">Astrophys.J.Lett. 886 (2019)</a>, <a href="https://arxiv.org/abs/1907.04872">arXiv:1907.04872</a> <br>
[3] S. Bernuzzi, M. Breschi, B. Daszuta, A. Endrizzi, D. Logoteta, V. Nedora, A. Perego, F. Schianchi, D. Radice, F. Zappa, I. Bombaci, N. Ortiz, <strong><em>Accretion-induced prompt black hole formation in asymmetric neutron star mergers, dynamical ejecta and kilonova signals</em></strong>, <a href="https://academic.oup.com/mnras/article/497/2/1488/5863958">Mon.Not.Roy.Astron.Soc. 497 (2020)</a>, <a href="https://arxiv.org/abs/2003.06015">arXiv:2003.06015</a> <br>
[4] D. Radice, A. Perego, K. Hotokezaka, S. A. Fromm, S. Bernuzzi, and L. F. Roberts, <strong><em>Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis</em></strong>, <a href="https://iopscience.iop.org/article/10.3847/1538-4357/aaf054">ApJ 869:130 (2018)</a>, <a href="https://arxiv.org/abs/1809.11161">arXiv:1809.11161</a>, <a href="https://zenodo.org/record/3588344#.X5u9ZXX0njs">Released data</a></p>
https://doi.org/10.5281/zenodo.4159620
oai:zenodo.org:4159620
eng
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https://doi.org/10.5281/zenodo.4159619
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Numerical Relativity Simulations of the Neutron Star Merger GW170817: Long-Term Remnant Evolutions, Winds, Remnant Disks, and Nucleosynthesis
info:eu-repo/semantics/article
oai:zenodo.org:46733
2020-01-24T19:24:33Z
user-nrgw-opendata
openaire_data
Radice, David
Bernuzzi, Sebastiano
Ott, Christian D.
2016-02-29
<p>We distribute complete gravitational-wave signals in the Advanced LIGO band (10 Hz - 8192 Hz) of the inspiral and merger of two neutron stars. These waveforms been constructed by hybridizing numerical-relativity data obtained with the WhiskyTHC code [1] with tidal effective-one-body waveforms [2,3]. More details on the procedure used to generate these waveforms are given in [4]. </p>
<p>The waveforms are distributed as HDF5 files containing the amplitude and phase of the -2 spin-weighted spherical harmonics multipoles of the strain:</p>
<p><span class="math-tex">\(( h_+ - \mathrm{i} h_\times )_{l,m} = \frac{A_{l,m}}{D_{\rm cm}} \exp(-\mathrm{i} \phi_{l,m} )\)</span></p>
<p>where <span class="math-tex">\(D_{\rm cm}\)</span> is the distance in cm from the source.</p>
<p>The data files include a machine readable "/metadata" group with:</p>
<ul>
<li>/metadata/EOS: name of the equation of state</li>
<li>/metadata/M_{A|B}: mass in isolation of star A (or B) in grams</li>
<li>/metadata/R_{A|B}: radius of star A (or B) in cm</li>
<li>/metadata/k2T: tidal coupling constant of the binary (see [3])</li>
<li>/metadata/kl_{A|B}: l=2,3,4 dimensionless Love numbers of star A (or B)</li>
</ul>
<p>We store amplitude and phase for multipoles modes up to l=4 as time series sampled at 16384 Hz.</p>
<p>We make these waveforms freely available in the hope that they will be useful. We kindly ask you to cite [3] and [4] in any publication resulting from the use of these waveforms.</p>
<p>---<br />
[1] http://www.tapir.caltech.edu/~david_e/whiskythc.html<br />
[2] https://eob.ihes.fr/<br />
[3] S. Bernuzzi, A. Nagar, T. Dietrich, T. Damour; Modeling the Dynamics of Tidally Interacting Binary Neutron Stars up to the Merger; Phys.Rev.Lett. 114 (2015) 16, 161103.<br />
[4] D. Radice, S. Bernuzzi, C. D. Ott; The One-Armed Spiral Instability in Neutron Star Mergers and its Detectability in Gravitational Waves; arXiv:1603.05726.</p>
https://doi.org/10.5281/zenodo.46733
oai:zenodo.org:46733
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https://zenodo.org/communities/nrgw-opendata
https://doi.org/
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gravitational waves
neutron stars
The One-Armed Spiral Instability in Neutron Star Mergers and its Detectability in Gravitational Waves
info:eu-repo/semantics/other
oai:zenodo.org:7253784
2023-02-06T14:23:42Z
user-nrgw-opendata
user-eu
Gonzalez, Alejandra
Zappa, Francesco
Breschi, Matteo
Bernuzzi, Sebastiano
Radice, David
Adhikari, Ananya
Camilletti, Alessandro
Chaurasia, Swami Vivekanandji
Doulis, Georgios
Padamata, Surendra
Rashti, Alireza
Ujevic, Maximiliano
Brügmann, Bernd
Cook, William
Dietrich, Tim
Perego, Albino
Poudel, Amit
Tichy, Wolfgang
2022-10-31
<p>We present python notebooks and data release associated to the "Second release of the CoRe database of binary neutron star merger waveforms" [1]. More information on the CoRe DB and collaboration can be found in our <a href="http://www.computational-relativity.org/">website</a> and in the first data release paper [2]. The released simulations are publicly available at <a href="https://core-gitlfs.tpi.uni-jena.de/">https://core-gitlfs.tpi.uni-jena.de/</a>.</p>
<p>The python package <a href="http://git.tpi.uni-jena.de/core/watpy">watpy</a> [1] provides functions and classes to work with the CoRe DB simulations. We also employ <a href="https://git.tpi.uni-jena.de/mbreschi/bajes">bajes</a> [3] for some functions or features.<br>
<br>
[1] A. Gonzalez et al., <em>Second release of the CoRe database of binary neutron star merger waveforms</em>, <a href="https://arxiv.org/abs/2210.16366">arXiv:2210.16366</a> [gr-qc]<br>
[2] T. Dietrich et al., <em>CoRe database of binary neutron star merger waveforms</em>, <a href="https://arxiv.org/abs/1806.01625">arXiv:1806.01625</a>. [gr-qc]<br>
[3] M.Breschi et. al., <em>Bayesian inference of multimessenger astrophysical data: Methods and applications to gravitational waves</em>, Phys. Rev. D 104 (2021) no.4, 042001, doi:10.1103/PhysRevD.104.042001, <a href="https://arxiv.org/abs/2102.00017">arXiv:2102.00017</a> [gr-qc]</p>
https://doi.org/10.5281/zenodo.7253784
oai:zenodo.org:7253784
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://zenodo.org/communities/eu
https://doi.org/10.5281/zenodo.7253783
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Binary neutron stars
Gravitational waves
Numerical Relativity
Second release of the CoRe database of binary neutron star merger waveforms
info:eu-repo/semantics/article
oai:zenodo.org:7915747
2023-05-10T14:26:54Z
user-nrgw-opendata
openaire_data
Chaurasia, Swami Vivekanandji
Markin, Ivan
2023-05-09
<p>This dataset contains the 3D output for NSbh_R2 run at refinement level l=1 and simulation time t=7950 (t=39.16 ms).</p>
<p>Data: Swami Vivekanandji Chaurasia (Stockholm University), Data release packaging: Ivan Markin (University of Potsdam);</p>
<p>Simulations for the project have been performed on the national supercomputer HPE Apollo Hawk at the High Performance Computing (HPC) Center Stuttgart (HLRS) under the grant number GWanalysis/44189, on the GCS Supercomputer SuperMUC NG at the Leibniz Supercomputing Centre (LRZ) [project pn29ba], and on the HPC systems Lise/Emmy of the North German Supercomputing Alliance (HLRN) [project bbp00049] for the final production runs. The particular simulation has been run on HLRN.</p>
https://doi.org/10.5281/zenodo.7915747
oai:zenodo.org:7915747
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://doi.org/10.5281/zenodo.7915746
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NSbh
Ejecta
Numerical Relativity
General-Relativistic Hydrodynamics Simulation of a Neutron Star — Sub-Solar-Mass Black Hole Merger - 3D Ejecta Data
info:eu-repo/semantics/other
oai:zenodo.org:4476842
2021-02-02T00:27:17Z
user-nrgw-opendata
user-eu
Gamba, Rossella
Bernuzzi, Sebastiano
Nagar, Alessandro
2021-02-01
<p>We release the data and the scripts used to produce the figures and tables of [1].<br>
We additionally release a handful of scripts which may be used to reproduce our results (see README.md).</p>
<p>TEOBResumSPA [1] is a frequency-domain effective-one-body multipolar approximant valid from any low frequency to merger based on the TEOBResumS [2] model.<br>
<br>
The software is freely available from <a href="https://bitbucket.org/eob_ihes/teobresums/src/master/">Bitbucket</a>, and can be installed using the standard Python setuptools routine (see documentation). We recommend using TEOBResumS v2.0 .</p>
<p> </p>
<p>[1] R. Gamba et al., Fast, faithful, frequency-domain effective-one-body waveforms for compact binary coalescences, <a href="https://arxiv.org/abs/2012.00027">arXiv:2012.00027</a> [gr-qc]</p>
<p>[2] A. Nagar et al., Time-domain effective-one-body gravitational waveforms for coalescing compact binaries with nonprecessing spins, tides and self-spin effects, Phys.Rev.D 98 (2018) 10, 104052, <a href="https://arxiv.org/abs/1806.01772">arXiv:1806.01772</a> [gr-qc]</p>
https://doi.org/10.5281/zenodo.4476842
oai:zenodo.org:4476842
eng
Zenodo
https://arxiv.org/abs/arXiv:2012.00027
https://zenodo.org/communities/nrgw-opendata
https://zenodo.org/communities/eu
https://doi.org/10.5281/zenodo.4476841
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Gravitational-Waves
Fast, faithful, frequency-domain effective-one-body waveforms for compact binary coalescences
info:eu-repo/semantics/article
oai:zenodo.org:4700060
2021-04-19T12:27:23Z
user-nrgw-opendata
user-eu
Nedora, Vsevolod
Radice, David
Bernuzzi, Sebastiano
Perego, Albino
Daszuta, Boris
Endrizzi, Andrea
Prakash, Aviral
Schianchi, Federico
2021-04-19
<p>Dynamical ejecta synchrotron emission as a possible contributor to the rebrightening of GRB170817A</p>
<p>Nedora, Vsevolod; Radice, David; Bernuzzi, Sebastiano; Perego, Albino; Daszuta, Boris; Endrizzi, Andrea; Prakash, Aviral; Schianchi, Federico.</p>
<p>We release light curves of the synchrotron emission of dynamical ejecta from a set of <br>
numerical relativity simulations (see [1] for details). </p>
<p>The data files are named according to model EOS, mass ratio, the inclusion of the <br>
subgrid turbulence and resolution. <br>
For instance, the `DD2_q182_LK_SR.dat` file contains light curves for the model <br>
with DD2 EOS, mass ratio q=1.82, with subgrid turbulence and computed at standard <br>
resolution. </p>
<p>Each file contains three columns: time [s], flux at 1keV and at 3GGz [erg].</p>
<p>Additionally, "Table 1" from [1] is included in the machine-readable format. Table contains <br>
- `model`: name of the model as described above,<br>
- `Lambda`: reduced tidal deformability,<br>
- `EOS`: equation of state,<br>
- `q`: model mass ratio defined as M1/M2, where M1 is the more massive star, so q is always larger than 1,<br>
- `Mej`: the total mass of the fast ejecta [Msun],<br>
- `Yeej`: electron fraction,<br>
- `vej`: velocity [c],<br>
- `theta_rms`: root mean square of the half opening angle around the binary plane [deg],</p>
<p>For more information on the light curve calculation and the related discussion see [1].<br>
The numerical relativity simulations used here are discussed in [1,2,3].</p>
<p>[1] V. Nedora, D. Radice, S. Bernuzzi, A. Perego B. Daszuta, A. Endrizzi, A. Prakash and F. Schianchi, Dynamical ejecta synchrotron emission as a possible contributor to the rebrightening of GRB170817A, <a href="https://arxiv.org/abs/2104.04537">arXiv:2104.04537</a><br>
[2] V. Nedora, S. Bernuzzi, D. Radice, B. Daszuta, A. Endrizzi, A. Perego, A. Prakash, M. Safarzadeh, F. Schianchi, D. Logoteta, Numerical Relativity Simulations of the Neutron Star Merger GW170817: Long-Term Remnant Evolutions, Winds, Remnant Disks, and Nucleosynthesis, <a href="https://iopscience.iop.org/article/10.3847/1538-4357/abc9be/pdf">APJ (906) 2</a>, <a href="https://arxiv.org/abs/2008.04333">arXiv:2008.04333</a> <br>
[3] S. Bernuzzi, M. Breschi, B. Daszuta, A. Endrizzi, D. Logoteta, V. Nedora, A. Perego, F. Schianchi, D. Radice, F. Zappa, I. Bombaci, N. Ortiz, Accretion-induced prompt black hole formation in asymmetric neutron star mergers, dynamical ejecta and kilonova signals, <a href="https://academic.oup.com/mnras/article/497/2/1488/5863958">Mon.Not.Roy.Astron.Soc. 497 (2020)</a>, <a href="https://arxiv.org/abs/2003.06015">arXiv:2003.06015</a> </p>
https://doi.org/10.5281/zenodo.4700060
oai:zenodo.org:4700060
Zenodo
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https://doi.org/10.5281/zenodo.4700059
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Dynamical ejecta synchrotron emission as a possible contributor to the rebrightening of GRB170817A
info:eu-repo/semantics/article
oai:zenodo.org:10477452
2024-01-10T08:28:34Z
user-nrgw-opendata
openaire_data
Breschi, Matteo
Gamba, Rossella
Godzieba, Daniel
Bernuzzi, Sebastiano
Perego, Albino
Radice, David
Bernuzzi, Sebastiano
Godzieba, Daniel
2024-01-10
<p>We release the set of about 10M equations of state (EOS) used in the paper </p>
<p><a title="Bayesian inference of multimessenger astrophysical data: Joint and coherent inference of gravitational waves and kilonovae" href="https://arxiv.org/abs/2401.03750" target="_blank" rel="noopener">Bayesian inference of multimessenger astrophysical data: Joint and coherent inference of gravitational waves and kilonovae</a> Breschi et al.</p>
<p>The EOS set is generated with a Markov Chain Monte Carlo approach by fixing the crust EOS and assuming i) general relativity; ii) causality at higher densities. Hence, it is agnostic on nuclear physics and not affected by nuclear physics uncertainties. The set includes EOS with and without first order phase transition. Please see</p>
<p><a title="On the maximum mass of neutron stars and GW190814" href="https://iopscience.iop.org/article/10.3847/1538-4357/abd4dd/meta" target="_blank" rel="noopener">On the maximum mass of neutron stars and GW190814</a> Godzieba et al. (also <a title="arxiv link" href="https://arxiv.org/abs/2007.10999" target="_blank" rel="noopener">arxiv link</a>)</p>
<p>The EOS are four-pieces piecewise polytropes. There are 4 adiabatic indices and three transition densities where the adiabatic index changes. The first index is for the crust EOS and is fixed for all EOSs. <br> <br>The columns of the original txt files are arranged as follows: <br> <br> column 1: G0 (crust adiabatic index) \<br> column 2: G1 |__________ four adiabatic indices<br> column 3: G2 |<br> column 4: G3 / <br> column 5: log(rho0) \ <br> column 6: log(rho1) |------- log of the three transition densities <br> column 7: log(rho2) / <br> column 8: central density of M = 1.4 Msun neutron star <br> column 9: radius of M = 1.4 Msun neutron star <br> column 10: lambda_2 of M = 1.4 Msun neutron star <br> column 11: central density of maximum mass neutron star <br> column 12: radius of maximum mass neutron star <br> column 13: mass of maximum mass neutron star <br> column 14: maximum sound speed squared divided by the speed of light <br> squared (max(c_s^2)/c^2) of the maximum mass neutron star <br> <br>Each of these columns a dataset of the HDF5.</p>
<p>Please cite the two references above if you use the dataset.</p>
https://doi.org/10.5281/zenodo.10477452
oai:zenodo.org:10477452
Zenodo
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https://doi.org/10.5281/zenodo.10477451
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Bayesian inference of multimessenger astrophysical data: Joint and coherent inference of gravitational waves and kilonovae, (2024-01-10)
equation of state
neutron star
Bayesian inference of multimessenger astrophysical data: Joint and coherent inference of gravitational waves and kilonovae
info:eu-repo/semantics/other
oai:zenodo.org:3355374
2020-01-20T17:07:59Z
user-nrgw-opendata
user-eu
Bernuzzi, Sebastiano
Harms, Enno
Lukes-Gerakopoulos , Georgios
2019-07-30
<p>We release data about the gravitational-wave fluxes radiated by a spinnig test-body in circular orbit around Schwarzschild.</p>
<p> * Computations were performed with two codes that solve the Teukolsky equation: a 2+1 time-domain (TD) and a frequency domain (FD) code.<br>
* Multipolar flux data are released up to $\ell=m=7$ and for different orbital radii (frequencies)<br>
* Different values of the body spin are considered in the interval $-1<\sigma<1$</p>
<p>Details and references can be found at https://arxiv.org/abs/1907.12233</p>
<p>Units c=G=1</p>
<p> </p>
See also https://zenodo.org/record/61308#.XUA2yvyxXOE for similar data.
https://doi.org/10.5281/zenodo.3355374
oai:zenodo.org:3355374
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://zenodo.org/communities/eu
https://doi.org/10.5281/zenodo.3355373
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Gravitational-wave fluxes of a spinning test-body orbiting around Schwarzschild black hole
info:eu-repo/semantics/preprint
oai:zenodo.org:7090935
2023-12-20T17:08:21Z
user-nrgw-opendata
openaire_data
Mitra, Ayan
Shukirgaliyev, Bekdaulet
Abylkairov, Sultan
Abdikamalov, Ernazar
2022-09-18
<p>The gravitational wave strain from сore-collapse supernova simulations used in our analysis. The file contains 402 signals labeled as <em>s00A0O00</em> or s00A0O00.0, where:</p>
<p><em>s00</em> -- corresponds to (zero-age) progenitor mass, e.g. s27 means 27 solar mass</p>
<p><em>A0</em> -- corresponds for a degree of differential rotation</p>
<p><em>O00 </em>or <em>O00.0 </em>-- corresponds to central angular velocity, e.g. O07 or O07.5 means that our model has a central angular velocity of 7 or 7.5 rad/s, respectively</p>
<p>Our waveforms are represented as a quadrupole wave amplitude. One can get a strain <em>h</em> multiplied by the distance <em>D </em>(= 10 kpc) by the following formula: <em>hD</em> = <strong><em>our_data</em></strong>/3.66 cm; see Eq (20) of Dimmelmeier et al 2008 [<a href="https://journals.aps.org/prd/abstract/10.1103/PhysRevD.78.064056">link</a>] for more information. All waveforms are represented in the time range from -15 to 20 ms with a 0.001 ms step size. The time of zero corresponds to the time of bounce. See [<a href="https://arxiv.org/abs/2209.14542">https://arxiv.org/abs/2209.14542</a>] for more information.</p>
https://doi.org/10.5281/zenodo.7090935
oai:zenodo.org:7090935
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://doi.org/10.5281/zenodo.7090934
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Exploring Supernova Gravitational Waves with Machine Learning
info:eu-repo/semantics/other
oai:zenodo.org:3235675
2020-01-24T19:25:50Z
user-nrgw-opendata
openaire_data
user-eu
David Radice
Albino Perego
Kenta Hotokezaka
Steven A. Fromm
Sebastiano Bernuzzi
Luke F. Roberts
2019-05-30
<p>We release dynamical ejecta data from binary neutron star merger simulations. The outflows are extracted at a fixed coordinate sphere with radius 300 G/c^2 Msun (= 443 km). Only material unbound according to the geodesic criterion is considered to be part of the dynamical ejecta. See [1] for more details.</p>
<p>Included data:</p>
<ul>
<li>`Table2.txt`: Table 2 of the paper in machine readable format</li>
<li>`tabulated_nucsyn.h5`: nucleosynthesis yields from pre-computed parametrized trajectories. The first three indices of each dataset are Ye, entropy, and expansion timescale tau. For example `Y_final[iYe, ientr, itau, iiso]` gives the final abundance of isotope `iiso` with `A[iiso]` and `Z[iiso]` for a trajectory with initial Ye = `Ye[iYe]`, initial entropy `s[ientr]`, and expansion timescale `tau[itau]`.</li>
<li>`tabulated_rho.h5`: gives the density scale corresponding to the Ye, entropy, and expansion timescale in `tabulated_nucsyn.h5`.</li>
<li>`[model].tar`: ejecta data for individual simulations. The naming convention is the same as in the paper.</li>
</ul>
<p>For each model we provide:</p>
<ul>
<li>`outflow.txt`: angle integrated outflow rate and cumulated ejecta mass. Data are given in units with Msun = G = c = 1 (eg, the conversion factor for time to seconds is 4.9258e-6).</li>
<li>`hist_entropy.dat`: histogram of the ejecta as a function of the entropy (in kb)</li>
<li>`hist_vinf.dat`: histogram of the ejecta as a function of the asymptotic velocity (in units of c)</li>
<li>`hist_ye.dat`: histogram of the ejecta as a function of the electron fraction Ye.</li>
<li>`profile.txt`: time integrated ejecta profiles as a function of the polar angle.</li>
<li>`hist_vinf_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.</li>
<li>`hist_ye_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.</li>
<li>`hist_ye_entropy_tau.h5`: histograms of the ejecta as a function of Ye, entropy, and expansion timescale tau.</li>
</ul>
<p>Additionally we distribute:</p>
<ul>
<li>Initial data generated with LORENE and associated EOS tables.</li>
<li>EOS tables used for the evolution</li>
<li>Parameter file used for each simulation</li>
</ul>
<p>For the multidimensional histograms the indices are ordered as specified in the file name, ie the file `hist_ye_theta.h5` tabulates the ejecta mass as a function of Ye (first index) and polar angle theta (second index).</p>
<p><br>
[1] D. Radice, A. Perego, K. Hotokezaka, S. A. Fromm, S. Bernuzzi, and L. F. Roberts, <em>Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis</em>, <a href="https://dx.doi.org/10.3847/1538-4357/aaf054">ApJ 869:130 (2018)</a>, <a href="https://arxiv.org/abs/1809.11161">arXiv:1809.11161</a></p>
https://doi.org/10.5281/zenodo.3235675
oai:zenodo.org:3235675
Zenodo
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https://doi.org/10.5281/zenodo.3235674
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Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis
info:eu-repo/semantics/other
oai:zenodo.org:4476594
2021-01-30T00:27:04Z
user-nrgw-opendata
user-eu
Matteo Breschi
Rossella Gamba
Sebastiano Bernuzzi
2021-01-29
<p>We release the posterior samples (and the related configuration files for reproducibility) coming from the analyses of gravitational-wave (GW) triggers presented in GWTC-1 [1] estimated with TEOBResumS model [2] using the Bajes pipeline [3].</p>
<p>Bajes [baɪɛs] is a Python package developed at Friedrich-Schiller-Universtaet Jena that aims to provide a simple, complete and reliableimplementation capable to robustly perform Bayesian inference on arbitrary sets of data, with specific functionalities for multimessenger astrophysics.</p>
<p>The Bajes software can be downloaded from <a href="https://github.com/matteobreschi/bajes">Github</a> and installed using the standard Python setuptools routine (see documentation).</p>
<p>The presented data contain .zip repositories for every analyzed GW events. Each repository stores the following objects:</p>
<ul>
<li>config.ini : the configuration file employed to execute the job;</li>
<li>posterior.dat : ASCII file containing the posterior samples (sorted by increasing likelihood), with the following columns:
<ul>
<li>m_chirp : chirp mass, detector-frame [solar masses]</li>
<li>m_ratio : mass ratio [greater or equal to 1]</li>
<li>m_chirp_source : chirp mass, source-frame [solar masses]</li>
<li>m_1_source : primary mass component, source-frame [solar masses]</li>
<li>m_2_source : secondary mass component, source-frame [solar masses]</li>
<li>s_1_z : primary (dimensionless) spin z-component (aligned to orbital angular momentum)</li>
<li>s_2_z : secondary (dimensionless) spin z-component (aligned to orbital angular momentum)</li>
<li>chi_eff : effective spin parameter </li>
<li>lum_distance : luminosity distance [Mpc]</li>
<li>inclination : inclination angle [rad]</li>
<li>right_ascension : right ascension angle [rad]</li>
<li>declination : declination angle [rad]</li>
<li>Two additional columns are included for GW170817 with the tidal deformabilities, lambda_1 and lambda_2</li>
</ul>
</li>
</ul>
<p>[1] LIGO Scientific and Virgo Collaboration, <em>GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs</em>, <strong>Phys.Rev.X 9 (2019) 3, 031040</strong>, <a href="https://arxiv.org/abs/1811.12907">arXiv:1811.12907</a> [astro-ph.HE]</p>
<p>[2] A. Nagar et al., <em>Time-domain effective-one-body gravitational waveforms for coalescing compact binaries with nonprecessing spins, tides and self-spin effects</em>, <strong>Phys.Rev.D 98 (2018) 10, 104052</strong>, <a href="https://arxiv.org/abs/1806.01772">arXiv:1806.01772</a> [gr-qc]</p>
<p>[3] M. Breschi et al., <em>Bajes: Bayesian inference of multimessenger astrophysical data, methods and application to gravitational-waves</em>, related paper (2021)</p>
https://doi.org/10.5281/zenodo.4476594
oai:zenodo.org:4476594
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Zenodo
https://zenodo.org/communities/nrgw-opendata
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https://doi.org/10.5281/zenodo.4476593
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Gravitational-waves
Bayesian inference
Bajes: Bayesian inference of multimessenger astrophysical data, methods and application to gravitational-waves
info:eu-repo/semantics/article
oai:zenodo.org:57844
2020-01-24T19:25:04Z
user-nrgw-opendata
openaire_data
Bernuzzi, Sebastiano
Radice, David
Ott, Christian D.
Roberts, Luke F.
Mösta, Philipp
Galeazzi, Filippo
2016-07-12
<p>We release neutron star merger waveforms computed using fully general relativistic simulations of equal and unequal-mass binaries drawn from the galactic population. The simulations employ finite-temperature microphysical equations of state (LS220, DD2, and SFHo) and neutrino cooling. Please, see</p>
<p>http://arxiv.org/abs/1512.06397</p>
<p>for details.</p>
<p> </p>
<p>Each tarball refers to a simulation and contains</p>
<ul>
<li>Curvature multipolar waveform <span class="math-tex">\(\psi^{(4)}_{\ell m}\)</span></li>
<li>Metric multipolar waveform <span class="math-tex">\(h_{\ell m}\)</span></li>
<li>Radiated energy and angular momentum</li>
</ul>
<p>Files:</p>
<ul>
<li><em>waveforms/Psi4_l?_m?_r200.txt </em>
<ul>
<li>Columns: <span class="math-tex">\(t,\ \Re{(\psi^{(4)}_{\ell m})},\ \Im{(\psi^{(4)}_{\ell m})} \)</span></li>
</ul>
</li>
<li><em>waveforms/Rh_l?_m?_r200.txt</em>
<ul>
<li>Columns: <span class="math-tex">\(u/M,\ \Re{(h_{\ell m})}/M,\ \Im{(h_{\ell m})}/M,\ \Re{(\dot{h}_{\ell m})},\ \Im{(\dot{h}_{\ell m}}),\ M\omega_{\ell m},\ A_{\ell m}/M,\ \phi_{\ell m},\ t \)</span></li>
</ul>
</li>
<li><em>waveforms/Ej_r200.txt</em>
<ul>
<li>Columns: <span class="math-tex">\(E_b,\ j,\ E_\text{rad},\ J_\text{rad},\ t \)</span></li>
</ul>
</li>
</ul>
<p>where</p>
<ul>
<li><span class="math-tex">\(t\)</span> simulation time</li>
<li><span class="math-tex">\(u\)</span> retarded time</li>
<li><span class="math-tex">\(M\)</span> binary mass</li>
<li><span class="math-tex">\(\omega_{\ell m}\)</span> wave frequency</li>
<li><span class="math-tex">\(A_{\ell m}\)</span> wave amplitude</li>
<li><span class="math-tex">\(\phi_{\ell m}\)</span> wave phase</li>
<li><span class="math-tex">\(E_\text{GW}\)</span> radiated energy</li>
<li><span class="math-tex">\(J_\text{GW}\)</span> radiated angular momentum</li>
<li><span class="math-tex">\(E_b\)</span> binary energy</li>
<li><span class="math-tex">\(j\)</span> binary specific angular momentum</li>
</ul>
<p>Please refer to the paper and references therein for the definition of the different quantities.</p>
<p>Units <span class="math-tex">\(c=G=M_\text{Sun}=1\)</span></p>
https://doi.org/10.5281/zenodo.57844
oai:zenodo.org:57844
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://doi.org/
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Binary neutron stars
Gravitational waves
Numerical relativity
How loud are neutron star mergers?
info:eu-repo/semantics/other
oai:zenodo.org:5138447
2021-08-03T16:53:38Z
user-nrgw-opendata
openaire_data
Godzieba, Daniel A
Radice, David
Bernuzzi, Sebastiano
2021-07-26
<p>The MATLAB workspace file eos_data_set.mat contains the parameters and physical properties of 1,966,225 phenomenological neutron star (NS) equations of state (EOS).</p>
https://doi.org/10.5281/zenodo.5138447
oai:zenodo.org:5138447
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://doi.org/10.5281/zenodo.3954899
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Phenomenological EOS Data Set
info:eu-repo/semantics/other
oai:zenodo.org:3979635
2021-08-03T16:53:38Z
user-nrgw-opendata
openaire_data
Godzieba, Daniel A
Radice, David
Bernuzzi, Sebastiano
2020-07-21
<p>The MATLAB workspace file eos_data_set.mat contains the parameters and physical properties of 1,966,225 phenomenological neutron star (NS) equations of state (EOS).</p>
https://doi.org/10.5281/zenodo.3979635
oai:zenodo.org:3979635
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://doi.org/10.5281/zenodo.3954899
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Phenomenological EOS Data Set
info:eu-repo/semantics/other
oai:zenodo.org:5139957
2021-08-03T16:53:38Z
user-nrgw-opendata
openaire_data
Godzieba, Daniel A
Radice, David
Bernuzzi, Sebastiano
2021-07-26
<p>The MATLAB workspace file eos_data_set.mat contains the parameters and physical properties of 1,966,225 phenomenological neutron star (NS) equations of state (EOS).</p>
https://doi.org/10.5281/zenodo.5139957
oai:zenodo.org:5139957
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://doi.org/10.5281/zenodo.3954899
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Phenomenological EOS Data Set
info:eu-repo/semantics/other
oai:zenodo.org:201145
2020-01-24T19:24:38Z
user-nrgw-opendata
openaire_data
Richers, Sherwood
Ott, Christian David
Abdikamalov, Ernazar
O'Connor, Evan
Sullivan, Chris
2016-12-15
<p>Gravitational waveforms from 1824 fiducial and detailed electron capture simulations, sampled at 65535 Hz. The file is in HDF5 format, using the flags {dtype="f4",compression="gzip",shuffle=True,fletcher32=True}. Each group is contained in the "waveforms" top-level group and is named with the "A" and "omega_0" values from Equation 5 and the EOS. In each sub-group is a dataset containing timestamps in seconds (t=0 is core bounce) and a dataset containing the strain multiplied by the distance in centimeters. The values of A in kilometers, omega_0 in radians/s, and the EOS are stored as attributes of each group.</p>
<p>In addition, the Ye(rho) profiles are stored in the "yeofrho" top-level group. Each sub-group is labeled by the EOS used to generate the profile.</p>
<p>Finally, select reduced data is stored in the "reduced_data" top-level group. The following quantities are each stored as a 1824-element array, where elements of the same index from different datasets correspond to the same 2D simulation.</p>
<p>A(km) -- differential rotation parameter in Equation 5<br>
D*bounce_amplitude_1(cm) -- The minimum of the first (negative) GW strain peak, multiplied by distance.<br>
D*bounce_amplitude_2(cm) -- The maximum of the second (positive) GW strain peak, multiplied by distance.<br>
EOS -- the equation of state used in the simulation<br>
MbarICgrav(Msun) -- gravitational mass of the inner core, averaged over time after core bounce<br>
Mgrav1_IC_b(Msun) -- gravitational mass of the inner core at bounce<br>
Mrest_IC_b(Msun) -- rest mass of the inner core at bounce<br>
SNR(aLIGOfrom10kpc) -- signal to noise ratio of the GW signal, assuming a distance of 10kpc and aLIGO sensitivity<br>
T_c_b(MeV) -- central temperature at bounce<br>
Ye_c_b -- central electron fraction at bounce<br>
alpha_c_b -- central lapse at bounce<br>
beta1_IC_b -- ratio of rotational kinetic to gravitational potential energy of the inner core at bounce<br>
fpeak(Hz) -- frequency of the post-bounce GW oscillations<br>
j_IC_b() -- angular momentum of the inner core at bounce<br>
omega_0(rad|s) -- initial (pre-collapse) rotation rate used in Equation 5<br>
omega_max(rad|s) -- maximum rotation rate achieved outside of 5km<br>
rPNSequator_b(km) -- radius of the rho=10^11 g/ccm contour along the equator at bounce<br>
rPNSpole_b(km) -- radius of the rho=10^11 g/ccm contour along the pole at bounce<br>
r_omega_max(km) -- radius where omega_max occurs<br>
rho_c_b(g|ccm) -- central density at bounce (not time averaged)<br>
rhobar_c_postbounce(g|ccm) -- central density time averaged after bounce<br>
s_c_b(kB|baryon) -- central entropy at bounce<br>
t_postbounce_end(s) -- time of the end of the postbounce signal (t=0 is core bounce)<br>
tbounce(s) -- time of core bounce (t=0 is the beginning of the simulation)<br>
</p>
https://doi.org/10.5281/zenodo.201145
oai:zenodo.org:201145
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gravitational wave
core-collapse supernova
Equation of State Effects on Gravitational Waves from Rotating Core Collapse
info:eu-repo/semantics/other
oai:zenodo.org:5637361
2021-11-10T13:49:18Z
user-nrgw-opendata
openaire_data
Johnson-McDaniel, Nathan K.
Ghosh, Abhirup
Ghonge, Sudarshan
Saleem, Muhammed
Krishnendu, N. V.
Clark, James A.
2021-11-09
<p>This data release accompanies the paper Johnson-McDaniel et al., Investigating the relation between gravitational wave tests of general relativity, arXiv:2109.06988.</p>
<p>It provides the frame files containing the simulated observations of GR and non-GR signals (with no noise) analyzed in that paper. Specifically, these are simulated observations of binary black hole coalescences like GW150914 and GW170608.</p>
<p>Each directory inside one of the tarballs corresponds to a given simulated observation and contains three frame files, one for each observatory (LIGO Hanford, LIGO Livingston, and Virgo). The GR cases contain simulated observations generated using the IHES EOB and IMRPhenomD models, while the non-GR cases contain the modified EOB, TIGER, FTA, and modified dispersion relation (MDR) simulated observations, as described in the paper. Specifically, the TIGER and FTA cases modify the 2PN coefficient, while the MDR cases are for a massive graviton. For the GW150914-like simulated observations, there are two selections (one large, one smaller) of the non-GR parameter for each non-GR case.</p>
<p>The frame files in the GW150914-like (GW170808-like) cases contain 8 (16) seconds of data, starting from a GPS time of 1126259456 (1180922480). In both cases, the peak of the waveform (the "trigger time") is placed 2 seconds from the end of the data segment, so at GPS times of 1126259462 and 1180922494 for the GW150914-like and GW170608-like cases, respectively.</p>
<p>Any publication that uses these data should cite the aforementioned paper that describes them (arXiv:2109.06988), as well as this Zenodo release, doi:10.5281/zenodo.5637361.</p>
<p>Contents:</p>
<p>GW150914_like_GR.tgz:<br>
- GW150914_like_IHES_EOB_GR<br>
- GW150914_like_IMRPhenomD_GR</p>
<p>GW150914_like_nonGR_larger.tgz:<br>
- GW150914_like_IHES_EOB_modGR_a2_400<br>
- GW150914_like_IMRPhenomD_TIGER_dchi4_m13<br>
- GW150914_like_IMRPhenomD_FTA_dchi4_m13<br>
- GW150914_like_IMRPhenomD_MDR_alpha0_A_5em44</p>
<p>GW150914_like_nonGR_smaller.tgz:<br>
- GW150914_like_IHES_EOB_modGR_a2_40<br>
- GW150914_like_IMRPhenomD_TIGER_dchi4_m2<br>
- GW150914_like_IMRPhenomD_FTA_dchi4_m2<br>
- GW150914_like_IMRPhenomD_MDR_alpha0_A_1em44</p>
<p>GW170608_like_GR.tgz:<br>
- GW170608_like_IHES_EOB_GR<br>
- GW170608_like_IMRPhenomD_GR</p>
<p>GW170608_like_nonGR.tgz:<br>
- GW170608_like_IHES_EOB_modGR_a2_40<br>
- GW170608_like_IMRPhenomD_TIGER_dchi4_m2<br>
- GW170608_like_IMRPhenomD_FTA_dchi4_m2<br>
- GW170608_like_IMRPhenomD_MDR_alpha0_A_1em43</p>
https://doi.org/10.5281/zenodo.5637361
oai:zenodo.org:5637361
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Zenodo
https://arxiv.org/abs/arXiv:2109.06988
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https://doi.org/10.5281/zenodo.5637360
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gravitational waves
binary black holes
deviations from general relativity
Investigating the relation between gravitational wave tests of general relativity
info:eu-repo/semantics/other
oai:zenodo.org:7916719
2023-05-10T14:26:55Z
user-nrgw-opendata
openaire_data
Chaurasia, Swami Vivekanandji
Ujevic, Maximiliano
Abac, Adrian
Markin, Ivan
2023-05-09
<p>This dataset contains the gravitational waveform for NSbh simulation. See the README.txt file for details.</p>
<p>Simulations: Swami Vivekanandji Chaurasia (Stockholm University);</p>
<p>Postprocessing: Maximiliano Ujevic (Universidade Federal do ABC) and Adrian Abac (Max Planck Institute for Gravitational Physics);</p>
<p>Data release packaging: Ivan Markin (University of Potsdam);</p>
<p>Simulations for the project have been performed on the national supercomputer HPE Apollo Hawk at the High Performance Computing (HPC) Center Stuttgart (HLRS) under the grant number GWanalysis/44189, on the GCS Supercomputer SuperMUC NG at the Leibniz Supercomputing Centre (LRZ) [project pn29ba], and on the HPC systems Lise/Emmy of the North German Supercomputing Alliance (HLRN) [project bbp00049] for the final production runs. The particular simulation has been run on HLRN.</p>
https://doi.org/10.5281/zenodo.7916719
oai:zenodo.org:7916719
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https://doi.org/10.5281/zenodo.7916718
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General-Relativistic Hydrodynamics Simulation of a Neutron Star — Sub-Solar-Mass Black Hole Merger - Gravitational Waveform
info:eu-repo/semantics/other
oai:zenodo.org:5481812
2021-09-08T05:37:49Z
user-nrgw-opendata
openaire_data
Sotani, Hajime
Takiwaki, Tomoya
2021-09-07
<p>The data of the gravitational wavefroms of core-collapse supernovae, which are used in Sotani and Takiwaki (2020), Monthly Notices of the Royal Astronomical Society, Volume 498, Issue 3, pp.3503-3512.</p>
<p>Data Format:</p>
<p>The data are in ASCII format and the two columns are1:time time since bounce in sec</p>
<p>2:hplus plus polarization of the GW amplitude. We assume the source distance of 10 kpc.</p>
<p>The data are sampled at ~10 kHz, but, the sampling is not uniform in time. Therefore resampling might be necessary.</p>
https://doi.org/10.5281/zenodo.5481812
oai:zenodo.org:5481812
Zenodo
https://doi.org/10.1093/mnras/staa2597
https://arxiv.org/abs/arXiv:2008.00419
https://ui.adsabs.harvard.edu/#abs/2020MNRAS.498.3503S
https://zenodo.org/communities/nrgw-opendata
https://doi.org/10.5281/zenodo.5481811
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
Monthly Notices of the Royal Astronomical Society, 498(3), pp.3503-3512, (2021-09-07)
Core-Collapse Supernovae
gravitational wave
Avoided crossing in gravitational wave spectra from protoneutron star
info:eu-repo/semantics/other
oai:zenodo.org:5779691
2023-02-06T16:46:23Z
user-nrgw-opendata
user-eu
Cusinato, Marco
Guercilena, Federico Maria
Perego, Albino
Logoteta, Domenico
Radice, David
Bernuzzi, Sebastiano
Ansoldi, Stefano
2021-11-25
<p>Data relative to the paper "Neutrino emission from binary neutron star mergers: characterizing light curves and mean energies" by Cusinato et al. 2021 . </p>
<table summary="Additional metadata">
<tbody>
<tr>
<td><a href="https://arxiv.org/abs/2111.13005">arXiv:2111.13005</a> [astro-ph.HE]</td>
</tr>
</tbody>
</table>
<p>This data release includes all neutrino-related quantities for the BNS models presented in the paper, plus additional metadata. The data is stored in a single HDF5 file and documented in the accompanying README file.</p>
<p> </p>
<p> </p>
https://doi.org/10.5281/zenodo.5779691
oai:zenodo.org:5779691
eng
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://zenodo.org/communities/eu
https://doi.org/10.5281/zenodo.5779690
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
neutrinos
binary neutron stars
Neutrino emission from binary neutron star mergers: characterizing light curves and mean energies
info:eu-repo/semantics/article
oai:zenodo.org:5555498
2021-10-09T01:48:41Z
user-nrgw-opendata
openaire_data
Sotani, Hajime
Takiwaki, Tomoya
Togashi, Hajime
2021-10-08
<p>The data of the gravitational wavefroms of core-collapse supernovae, which are used in Sotani, Takiwaki and Togashi (2021), PRD in press</p>
<p>Data Format:</p>
<p>The data are in ASCII format and the two columns are1:time time since bounce in sec</p>
<p>2:hplus plus polarization of the GW amplitude. We assume the source distance of 10 kpc.</p>
<p>The data are sampled at ~10 kHz, but, the sampling is not uniform in time. Therefore resampling might be necessary.</p>
https://doi.org/10.5281/zenodo.5555498
oai:zenodo.org:5555498
Zenodo
https://arxiv.org/abs/arXiv:2110.03131
https://zenodo.org/communities/nrgw-opendata
https://doi.org/10.5281/zenodo.5555497
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
Core-Collapse Supernovae
gravitational wave
Universal relation for supernova gravitational waves
info:eu-repo/semantics/other
oai:zenodo.org:5489428
2021-10-07T02:28:59Z
user-nrgw-opendata
openaire_data
Takiwaki, Tomoya
Kotake, Kei
Foglizzo, Thierry
2021-09-08
<p>The data of the gravitational wavefroms of core-collapse supernovae, which are used in Takiwaki, Kotake, and Foglizzo, (2021), Monthly Notices of the Royal Astronomical Society, Volume 508, Issue 1, pp.966-985</p>
https://doi.org/10.5281/zenodo.5489428
oai:zenodo.org:5489428
Zenodo
https://arxiv.org/abs/arXiv:2107.02933
https://doi.org/10.1093/mnras/stab2607
https://zenodo.org/communities/nrgw-opendata
https://doi.org/10.5281/zenodo.5489427
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
Core-Collapse Supernovae
gravitational wave
Insights into non-axisymmetric instabilities in three-dimensional rotating supernova models with neutrino and gravitational-wave signatures
info:eu-repo/semantics/other
oai:zenodo.org:3588344
2020-01-24T19:25:44Z
user-nrgw-opendata
openaire_data
user-eu
David Radice
Albino Perego
Kenta Hotokezaka
Steven A. Fromm
Sebastiano Bernuzzi
Luke F. Roberts
2019-05-30
<p>We release dynamical ejecta data from binary neutron star merger simulations. The outflows are extracted at a fixed coordinate sphere with radius 300 G/c^2 Msun (= 443 km). Only material unbound according to the geodesic criterion is considered to be part of the dynamical ejecta. See [1] for more details.</p>
<p>Included data:</p>
<ul>
<li>`Table2.txt`: Table 2 of the paper in machine readable format</li>
<li>`tabulated_nucsyn.h5`: nucleosynthesis yields from pre-computed parametrized trajectories. The first three indices of each dataset are Ye, entropy, and expansion timescale tau. For example `Y_final[iYe, ientr, itau, iiso]` gives the final abundance of isotope `iiso` with `A[iiso]` and `Z[iiso]` for a trajectory with initial Ye = `Ye[iYe]`, initial entropy `s[ientr]`, and expansion timescale `tau[itau]`.</li>
<li>`tabulated_rho.h5`: gives the density at T = 6 GK corresponding to the Ye, entropy, and expansion timescale used in `tabulated_nucsyn.h5`.</li>
<li>`[model].tar`: ejecta data for individual simulations. The naming convention is the same as in the paper.</li>
</ul>
<p>For each model we provide:</p>
<ul>
<li>`outflow.txt`: angle integrated outflow rate and cumulated ejecta mass. Data are given in units with Msun = G = c = 1 (eg, the conversion factor for time to seconds is 4.9258e-6).</li>
<li>`hist_entropy.dat`: histogram of the ejecta as a function of the entropy (in kb)</li>
<li>`hist_vinf.dat`: histogram of the ejecta as a function of the asymptotic velocity (in units of c)</li>
<li>`hist_ye.dat`: histogram of the ejecta as a function of the electron fraction Ye.</li>
<li>`profile.txt`: time integrated ejecta profiles as a function of the polar angle.</li>
<li>`hist_vinf_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.</li>
<li>`hist_ye_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.</li>
<li>`hist_ye_entropy_tau.h5`: histograms of the ejecta as a function of Ye, entropy, and expansion timescale tau.</li>
</ul>
<p>Additionally we distribute:</p>
<ul>
<li>Initial data generated with LORENE and associated EOS tables.</li>
<li>EOS tables used for the evolution</li>
<li>Parameter file used for each simulation</li>
</ul>
<p>For the multidimensional histograms the indices are ordered as specified in the file name, ie the file `hist_ye_theta.h5` tabulates the ejecta mass as a function of Ye (first index) and polar angle theta (second index).</p>
<p><br>
[1] D. Radice, A. Perego, K. Hotokezaka, S. A. Fromm, S. Bernuzzi, and L. F. Roberts, <em>Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis</em>, <a href="https://dx.doi.org/10.3847/1538-4357/aaf054">ApJ 869:130 (2018)</a>, <a href="https://arxiv.org/abs/1809.11161">arXiv:1809.11161</a></p>
https://doi.org/10.5281/zenodo.3588344
oai:zenodo.org:3588344
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://zenodo.org/communities/eu
https://doi.org/10.5281/zenodo.3235674
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis
info:eu-repo/semantics/other
oai:zenodo.org:4283517
2020-11-22T00:27:18Z
user-nrgw-opendata
user-eu
Nedora, Vsevolod
Schianchi, Federico
Bernuzzi, Sebastiano
Radice, David
Daszuta, Boris
Endrizzi, Andrea
Perego, Albino
Prakash, Aviral
Zappa, Francesco
2020-11-21
<p>We release compiled numerical relativity data of neutron star mergers taken from<br>
several previous studies done by different groups with <br>
different physics setups (see [1] for details).</p>
<p>The data file, 'summary_table.csv' contains the following columns:</p>
<p>- `model`: name or a number of the model as referred to in the source,<br>
- `bibkey`: citation reference, according to <a href="https://inspirehep.net/">inspirehep</a> convention,<br>
- `dataset`: name of the dataset, as used in [1] study,<br>
- `EOS`: equation of state,<br>
- `nus`: short abbreviation of neutrino transport scheme, 'M1' stands for the M1 scheme, 'leak' stands for leakage scheme only, 'leakM0' stands for the leakage plus M0 scheme, 'leakM1' stands for leakage and M1 scheme and 'none' stands for no neutrinos in simulations,<br>
- `arxiv`: link to the source paper on arXiv <a href="https://arxiv.org/">arXiv</a> ;</p>
<p>on the binary parameters:</p>
<p>- `q`: model mass ratio defined as M1/M2, where M1 is the more massive star, so q is always larger than 1,<br>
- `M1`, `M2`: gravitational masses of stars [Msum],<br>
- `Mb1`, `Mb2`: baryonic masses of the stars [Msun],<br>
- `C1`, `C2`: stars' compactness,<br>
- `Lambda`: reduced tidal parameter;</p>
<p>on the properties of the dynamical ejecta and disk:</p>
<p>- `Mej`: total mass [Msun],<br>
- `vej`: velocity [c],<br>
- `Yeej`: electron fraction,<br>
- `theta_rms`: root mean square of the half opening angle around the binary plane [deg],<br>
- `Mdisk`: disk mass [Msun].</p>
<p>For more information on the data compilation and statistical analysis see [1]. <br>
The properties of the dynamical ejecta of the models of `M0RefSet` are discussed in [2,3] that <br>
was publicly released on <a href="https://zenodo.org/record/4159620#.X7khP3X0njt">Zenodo</a> .</p>
<p>[1] V. Nedora, F. Schianchi, S. Bernuzzi, D. Radice, B. Daszuta, A. Endrizzi, A. Perego, A. Prakash, F. Zappa, <strong><em>Mapping dynamical ejecta and disk masses from numerical relativity simulations of neutron star mergers</em></strong>, arXiv:2008.xxxxx <br>
[2] V. Nedora, S. Bernuzzi, D. Radice, B. Daszuta, A. Endrizzi, A. Perego, A. Prakash, M. Safarzadeh, F. Schianchi, D. Logoteta, <strong>Numerical Relativity Simulations of the Neutron Star Merger GW170817: Long-Term Remnant Evolutions, Winds, Remnant Disks, and Nucleosynthesis</strong>, <a href="https://arxiv.org/abs/2008.04333">arXiv:2008.04333 </a><br>
[3] S. Bernuzzi, M. Breschi, B. Daszuta, A. Endrizzi, D. Logoteta, V. Nedora, A. Perego, F. Schianchi, D. Radice, F. Zappa, I. Bombaci, N. Ortiz, <strong>Accretion-induced prompt black hole formation in asymmetric neutron star mergers, dynamical ejecta and kilonova signals</strong>, <a href="https://academic.oup.com/mnras/article/497/2/1488/5863958">Mon.Not.Roy.Astron.Soc. 497 (2020)</a>, <a href="https://arxiv.org/abs/2003.06015">arXiv:2003.06015 </a></p>
https://doi.org/10.5281/zenodo.4283517
oai:zenodo.org:4283517
eng
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://zenodo.org/communities/eu
https://doi.org/10.5281/zenodo.4283516
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
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Mapping dynamical ejecta and disk masses from numerical relativity simulations of neutron star mergers
info:eu-repo/semantics/article
oai:zenodo.org:61308
2020-01-24T19:24:37Z
user-nrgw-opendata
openaire_data
Harms, Enno
Lukes-Gerakopoulos , Georgios
Bernuzzi, Sebastiano
Nagar, Alessandro
2016-09-01
<p>We release gravitational wave fluxes at null-infinity from a spinning test-body in circular equatorial orbits around a Schwarzschild black hole. Four different prescriptions are used for the dynamics: the Mathisson-Papapetrou formalism under the Tulczyjew (TUL) spin-supplementary-condition (SSC), the Pirani (PIR) SSC and the Ohashi-Kyrian-Semerak (OKS) SSC, and the spinning particle limit of the effective-one-body Hamiltonian (HAM) of [Phys.~Rev.~D.90,~044018(2014)]. For more details see xxxx .</p>
<p>The multipolar fluxes are given for l=2,3 m=1,2,3 at the Boyer-Lindquist radii</p>
<p> r = 4 5 6 7 8 10 12 15 20 30 ,</p>
<p>in cases they were not computed the data contains a "42". Note that the fluxes in these data files are assumed to contain both the +m and -m contributions, since they are identical for equatorial orbits and aligned spins. <br />
Additionally, the data files contain the key numbers describing the circular dynamics (see paper).</p>
<p>Units <span class="math-tex"><em>c</em>=<em>G</em>=1.</span></p>
https://doi.org/10.5281/zenodo.61308
oai:zenodo.org:61308
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://doi.org/
info:eu-repo/semantics/openAccess
Creative Commons Zero v1.0 Universal
https://creativecommons.org/publicdomain/zero/1.0/legalcode
gravitational waves
spinning bodies
binary black holes
Teukolsky equation
Spinning test-body orbiting around Schwarzschild black hole: circular dynamics and gravitational-wave fluxes
info:eu-repo/semantics/other
oai:zenodo.org:5140275
2021-08-03T16:53:38Z
user-nrgw-opendata
openaire_data
Godzieba, Daniel A
Radice, David
Bernuzzi, Sebastiano
2021-07-27
<p>The MATLAB workspace file eos_data_set.mat contains the parameters and physical properties of 1,966,225 phenomenological neutron star (NS) equations of state (EOS).</p>
https://doi.org/10.5281/zenodo.5140275
oai:zenodo.org:5140275
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://doi.org/10.5281/zenodo.3954899
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
Phenomenological EOS Data Set
info:eu-repo/semantics/other
oai:zenodo.org:3954900
2021-08-03T16:53:38Z
user-nrgw-opendata
openaire_data
Godzieba, Daniel A
Radice, David
Bernuzzi, Sebastiano
2020-07-21
<p>The MATLAB workspace file eos_data_set.mat contains the parameters and physical properties of 1,966,225 phenomenological neutron star (NS) equations of state (EOS).</p>
https://doi.org/10.5281/zenodo.3954900
oai:zenodo.org:3954900
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://doi.org/10.5281/zenodo.3954899
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
Phenomenological EOS Data Set
info:eu-repo/semantics/other
oai:zenodo.org:5156158
2021-08-04T13:48:22Z
user-nrgw-opendata
openaire_data
Godzieba, Daniel A
Radice, David
Bernuzzi, Sebastiano
2021-08-03
<p>The MATLAB workspace file eos_data_set.mat contains the parameters and physical properties of 1,966,225 phenomenological neutron star (NS) equations of state (EOS).</p>
https://doi.org/10.5281/zenodo.5156158
oai:zenodo.org:5156158
Zenodo
https://zenodo.org/communities/nrgw-opendata
https://doi.org/10.5281/zenodo.3954899
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
Phenomenological EOS Data Set
info:eu-repo/semantics/other