You have already added 0 works in your ORCID record related to the merged Research product.
You have already added 0 works in your ORCID record related to the merged Research product.
The SXS collaboration catalog of binary black hole simulations
Copyright policy )The SXS collaboration catalog of binary black hole simulations
Accurate models of gravitational waves from merging black holes are necessary for detectors to observe as many events as possible while extracting the maximum science. Near the time of merger, the gravitational waves from merging black holes can be computed only using numerical relativity. In this paper, we present a major update of the Simulating eXtreme Spacetimes (SXS) Collaboration catalog of numerical simulations for merging black holes. The catalog contains 2018 distinct configurations (a factor of 11 increase compared to the 2013 SXS catalog), including 1426 spin-precessing configurations, with mass ratios between 1 and 10, and spin magnitudes up to 0.998. The median length of a waveform in the catalog is 39 cycles of the dominant $\ell=m=2$ gravitational-wave mode, with the shortest waveform containing 7.0 cycles and the longest 351.3 cycles. We discuss improvements such as correcting for moving centers of mass and extended coverage of the parameter space. We also present a thorough analysis of numerical errors, finding typical truncation errors corresponding to a waveform mismatch of $\sim 10^{-4}$. The simulations provide remnant masses and spins with uncertainties of 0.03% and 0.1% ($90^{\text{th}}$ percentile), about an order of magnitude better than analytical models for remnant properties. The full catalog is publicly available at https://www.black-holes.org/waveforms .
Comment: 33+18 pages, 13 figures, 4 tables, 2,018 binaries. Catalog metadata in ancillary JSON file. v2: Matches version accepted by CQG. Catalog available at https://www.black-holes.org/waveforms
- University of Salford United Kingdom
- National Aeronautics and Space Administration United States
- The University of Texas at Austin United States
- University of Illinois at Urbana Champaign United States
- University of Tokyo Japan
Microsoft Academic Graph classification: Physics Angular momentum Gravitational wave Parameter space Computational physics Numerical relativity Binary black hole Precession Waveform Order of magnitude
arXiv: Astrophysics::High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology
High Energy Astrophysical Phenomena (astro-ph.HE), Physics and Astronomy (miscellaneous), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, Astrophysics - High Energy Astrophysical Phenomena
High Energy Astrophysical Phenomena (astro-ph.HE), Physics and Astronomy (miscellaneous), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, Astrophysics - High Energy Astrophysical Phenomena
Microsoft Academic Graph classification: Physics Angular momentum Gravitational wave Parameter space Computational physics Numerical relativity Binary black hole Precession Waveform Order of magnitude
arXiv: Astrophysics::High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology
212122
[1] Aasi J et al. (LIGO Scientific) 2015 Class. Quant. Grav. 32 074001 [arXiv:1411.4547]
[2] Acernese F et al. (Virgo) 2015 Class. Quant. Grav. 32 024001 [arXiv:1408.3978]
[3] Abbott B P et al. (LIGO Scientific, Virgo) 2016 Phys. Rev. Lett. 116 061102 [arXiv:1602.03837]
[4] Abbott B P et al. (LIGO Scientific, Virgo) 2016 Phys. Rev. D93 122003 [arXiv:1602.03839]
[5] Abbott B P et al. (LIGO Scientific, Virgo) 2016 Phys. Rev. Lett. 116 131103 [arXiv:1602.03838]
[6] Abbott B P et al. (LIGO Scientific, Virgo) 2016 Phys. Rev. Lett. 116 241102 [arXiv:1602.03840]
[7] Abbott B P et al. (LIGO Scientific, Virgo) 2017 Phys. Rev. Lett. 119 161101 [arXiv:1710.05832]
[8] Abbott B P et al. (LIGO Scientific, Virgo) 2016 Phys. Rev. Lett. 116 241103 [arXiv:1606.04855]
[9] Abbott B P et al. (LIGO Scientific, Virgo) 2017 Phys. Rev. Lett. 118 221101 [Erratum: Phys. Rev. Lett.121,no.12,129901(2018)] [arXiv:1706.01812]
[10] Abbott B P et al. (LIGO Scientific, Virgo) 2017 Astrophys. J. 851 L35 [arXiv:1711.05578]
citations This is an alternative to the "Influence" indicator, which also reflects the overall/total impact of an article in the research community at large, based on the underlying citation network (diachronically).191 popularity This indicator reflects the "current" impact/attention (the "hype") of an article in the research community at large, based on the underlying citation network.Top 0.1% influence This indicator reflects the overall/total impact of an article in the research community at large, based on the underlying citation network (diachronically).Top 10% impulse This indicator reflects the initial momentum of an article directly after its publication, based on the underlying citation network.Top 0.1% citations This is an alternative to the "Influence" indicator, which also reflects the overall/total impact of an article in the research community at large, based on the underlying citation network (diachronically).191 popularity This indicator reflects the "current" impact/attention (the "hype") of an article in the research community at large, based on the underlying citation network.Top 0.1% influence This indicator reflects the overall/total impact of an article in the research community at large, based on the underlying citation network (diachronically).Top 10% impulse This indicator reflects the initial momentum of an article directly after its publication, based on the underlying citation network.Top 0.1%
Citations provided by BIP!Popularity provided by BIP!- Natural Sciences and Engineering Research Council of Canada (NSERC)
- Netherlands Organisation for Scientific Research (NWO) (NWO)
- 680-47-460
- National Science Foundation (NSF)
- 0725070
- Directorate for Computer & Information Science & Engineering | Division of Advanced Cyberinfrastructure
- National Science Foundation (NSF)
- 1806665
- Directorate for Mathematical & Physical Sciences | Division of Physics
- University of Salford United Kingdom
- National Aeronautics and Space Administration United States
- The University of Texas at Austin United States
- University of Illinois at Urbana Champaign United States
- University of Tokyo Japan
- University of Toronto Canada
- Max Planck Society Germany
- California Institute of Technology United States
- Cornell University United States
- University of Massachusetts System United States
- University of Manchester United Kingdom
- University of Mississippi United States
- Jet Propulsion Lab United States
- Canadian Institute for Theoretical Astrophysics Canada
- Department of Physics and Astronomy Northwestern University United States
- California Institute of Technology, Jet Propulsion Laboratory United States
- University of Massachusetts Dartmouth United States
- Massachusetts Institute of Technology United States
- University of Birmingham United Kingdom
- Department of Physics and Astronomy University of Rochester United States
- Department of Physics and Astronomy University of California, Irvine United States
- Jet Propulsion Laboratory, California Institute of Technology, NASA, Pasadena, CA United States
- Jet Propulsion Laboratory (JPL) California Institute of Technology United States
- California State University, Fullerton United States
- Canadian Inst. for Theoretical Astrophysics (CITA) University of Toronto Canada
- University of Manchester, UK United Kingdom
- University of Toronto Canada
Accurate models of gravitational waves from merging black holes are necessary for detectors to observe as many events as possible while extracting the maximum science. Near the time of merger, the gravitational waves from merging black holes can be computed only using numerical relativity. In this paper, we present a major update of the Simulating eXtreme Spacetimes (SXS) Collaboration catalog of numerical simulations for merging black holes. The catalog contains 2018 distinct configurations (a factor of 11 increase compared to the 2013 SXS catalog), including 1426 spin-precessing configurations, with mass ratios between 1 and 10, and spin magnitudes up to 0.998. The median length of a waveform in the catalog is 39 cycles of the dominant $\ell=m=2$ gravitational-wave mode, with the shortest waveform containing 7.0 cycles and the longest 351.3 cycles. We discuss improvements such as correcting for moving centers of mass and extended coverage of the parameter space. We also present a thorough analysis of numerical errors, finding typical truncation errors corresponding to a waveform mismatch of $\sim 10^{-4}$. The simulations provide remnant masses and spins with uncertainties of 0.03% and 0.1% ($90^{\text{th}}$ percentile), about an order of magnitude better than analytical models for remnant properties. The full catalog is publicly available at https://www.black-holes.org/waveforms .
Comment: 33+18 pages, 13 figures, 4 tables, 2,018 binaries. Catalog metadata in ancillary JSON file. v2: Matches version accepted by CQG. Catalog available at https://www.black-holes.org/waveforms