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Surrogate model of hybridized numerical relativity binary black hole waveforms
Copyright policy )Surrogate model of hybridized numerical relativity binary black hole waveforms
Numerical relativity (NR) simulations provide the most accurate binary black hole gravitational waveforms, but are prohibitively expensive for applications such as parameter estimation. Surrogate models of NR waveforms have been shown to be both fast and accurate. However, NR-based surrogate models are limited by the training waveforms' length, which is typically about 20 orbits before merger. We remedy this by hybridizing the NR waveforms using both post-Newtonian and effective one body waveforms for the early inspiral. We present NRHybSur3dq8, a surrogate model for hybridized nonprecessing numerical relativity waveforms, that is valid for the entire LIGO band (starting at $20~\text{Hz}$) for stellar mass binaries with total masses as low as $2.25\,M_{\odot}$. We include the $\ell \leq 4$ and $(5,5)$ spin-weighted spherical harmonic modes but not the $(4,1)$ or $(4,0)$ modes. This model has been trained against hybridized waveforms based on 104 NR waveforms with mass ratios $q\leq8$, and $|\chi_{1z}|,|\chi_{2z}| \leq 0.8$, where $\chi_{1z}$ ($\chi_{2z}$) is the spin of the heavier (lighter) BH in the direction of orbital angular momentum. The surrogate reproduces the hybrid waveforms accurately, with mismatches $\lesssim 3\times10^{-4}$ over the mass range $2.25M_{\odot} \leq M \leq 300 M_{\odot}$. At high masses ($M\gtrsim40M_{\odot}$), where the merger and ringdown are more prominent, we show roughly two orders of magnitude improvement over existing waveform models. We also show that the surrogate works well even when extrapolated outside its training parameter space range, including at spins as large as 0.998. Finally, we show that this model accurately reproduces the spheroidal-spherical mode mixing present in the NR ringdown signal.
Comment: Matches PRD version. Model publicly available at https://zenodo.org/record/2549618#.XJvMrutKii4. 18 pages, 12 figures
- Max Planck Institute for Heart and Lung Research Germany
- University of Toronto Canada
- Max Planck Society Germany
- University of Illinois at Urbana Champaign United States
- California Institute of Technology United States
Microsoft Academic Graph classification: Physics Angular momentum Spins Spherical harmonics Parameter space Black hole Numerical relativity Binary black hole Mathematical physics Spin-½
FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology
FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology
Microsoft Academic Graph classification: Physics Angular momentum Spins Spherical harmonics Parameter space Black hole Numerical relativity Binary black hole Mathematical physics Spin-½
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[12] Sebastian Khan, Katerina Chatziioannou, Mark Hannam, and Frank Ohme, \Phenomenological model for the gravitational-wave signal from precessing binary black holes with two-spin e ects," (2018), arXiv:1809.10113 [gr-qc]. [OpenAIRE]
[13] Yi Pan, Alessandra Buonanno, Andrea Taracchini, Lawrence E. Kidder, Abdul H. Mrou, Harald P. Pfeiffer, Mark A. Scheel, and Bla Szilgyi, \Inspiral-mergerringdown waveforms of spinning, precessing black-hole binaries in the e ective-one-body formalism," Phys. Rev. D89, 084006 (2014), arXiv:1307.6232 [gr-qc].
[14] Lionel London, Sebastian Khan, Edward FauchonJones, Cecilio Garca, Mark Hannam, Sascha Husa, Xisco Jimnez-Forteza, Chinmay Kalaghatgi, Frank Ohme, and Francesco Pannarale, \First highermultipole model of gravitational waves from spinning and coalescing black-hole binaries," Phys. Rev. Lett. 120, 161102 (2018), arXiv:1708.00404 [gr-qc].
[15] Roberto Cotesta, Alessandra Buonanno, Alejandro Boh, Andrea Taracchini, Ian Hinder, and Serguei Ossokine, \Enriching the Symphony of Gravitational Waves from Binary Black Holes by Tuning Higher Harmonics," Phys. Rev. D98, 084028 (2018), arXiv:1803.10701 [gr-qc].
[16] Sebastian Khan, Sascha Husa, Mark Hannam, Frank Ohme, Michael Prrer, Xisco Jimnez Forteza, and Alejandro Boh, \Frequency-domain gravitational waves from nonprecessing black-hole binaries. II. A phenomenological model for the advanced detector era," Phys. Rev. D93, 044007 (2016), arXiv:1508.07253 [grqc].
[17] Alejandro Bohe, Lijing Shao, Andrea Taracchini, Alessandra Buonanno, Stanislav Babak, Ian W. Harry, Ian Hinder, Serguei Ossokine, Michael Purrer, Vivien Raymond, Tony Chu, Heather Fong, Prayush Kumar, Harald P. Pfei er, Michael Boyle, Daniel A. Hemberger, Lawrence E. Kidder, Geo rey Lovelace, Mark A. Scheel, and Bela Szilagyi, \Improved e ective-one-body model of spinning, nonprecessing binary black holes for the era of gravitational-wave astrophysics with advanced detectors," Phys. Rev. D 95, 044028 (2017), arXiv:1611.03703 [gr-qc].
[18] Mark Hannam, Patricia Schmidt, Alejandro Bohe, Leila Haegel, Sascha Husa, et al., \A simple model of complete precessing black-hole-binary gravitational waveforms," Phys. Rev. Lett. 113, 151101 (2014), arXiv:1308.3271 [gr-qc].
[19] Andrea Taracchini et al., \E ective-one-body model for black-hole binaries with generic mass ratios and spins," Phys. Rev. D89, 061502 (2014), arXiv:1311.2544 [grqc].
[20] Yi Pan, Alessandra Buonanno, Michael Boyle, Luisa T. Buchman, Lawrence E. Kidder, Harald P. Pfei er, and Mark A. Scheel, \Inspiral-merger-ringdown multipolar waveforms of nonspinning black-hole binaries using the e ective-one-body formalism," Phys. Rev. D84, 124052 (2011), arXiv:1106.1021 [gr-qc].
[21] Ajit Kumar Mehta, Chandra Kant Mishra, Vijay Varma, and Parameswaran Ajith, \Accurate inspiralmerger-ringdown gravitational waveforms for nonspinning black-hole binaries including the e ect of subdominant modes," Phys. Rev. D96, 124010 (2017), arXiv:1708.03501 [gr-qc].
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Citations provided by BIP!Popularity provided by BIP!- National Science Foundation (NSF)
- 1238993
- Directorate for Computer & Information Science & Engineering | Division of Advanced Cyberinfrastructure
- 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
- National Science Foundation (NSF)
- 1713694
- Directorate for Computer & Information Science & Engineering | Division of Advanced Cyberinfrastructure
- Max Planck Institute for Heart and Lung Research Germany
- University of Toronto Canada
- Max Planck Society Germany
- University of Illinois at Urbana Champaign United States
- California Institute of Technology United States
- Max Planck Institute for Gravitational Physics Germany
- University of Massachusetts System United States
- Max Planck Institute for Plasma Physics - Greifswald Germany
- Max Planck Institute for Extraterrestrial Physics Germany
- Canadian Institute for Theoretical Astrophysics Canada
- Canadian Inst. for Theoretical Astrophysics (CITA) University of Toronto Canada
- Max Planck Institute for Plasma Physics Germany
- Max Planck Institute for Nuclear Physics Germany
- Max Planck Institute for Physics Germany
- University of Massachusetts Dartmouth United States
- Cornell University United States
- Max Planck Institute for Chemical Physics of Solids Germany
- University of Toronto Canada
Numerical relativity (NR) simulations provide the most accurate binary black hole gravitational waveforms, but are prohibitively expensive for applications such as parameter estimation. Surrogate models of NR waveforms have been shown to be both fast and accurate. However, NR-based surrogate models are limited by the training waveforms' length, which is typically about 20 orbits before merger. We remedy this by hybridizing the NR waveforms using both post-Newtonian and effective one body waveforms for the early inspiral. We present NRHybSur3dq8, a surrogate model for hybridized nonprecessing numerical relativity waveforms, that is valid for the entire LIGO band (starting at $20~\text{Hz}$) for stellar mass binaries with total masses as low as $2.25\,M_{\odot}$. We include the $\ell \leq 4$ and $(5,5)$ spin-weighted spherical harmonic modes but not the $(4,1)$ or $(4,0)$ modes. This model has been trained against hybridized waveforms based on 104 NR waveforms with mass ratios $q\leq8$, and $|\chi_{1z}|,|\chi_{2z}| \leq 0.8$, where $\chi_{1z}$ ($\chi_{2z}$) is the spin of the heavier (lighter) BH in the direction of orbital angular momentum. The surrogate reproduces the hybrid waveforms accurately, with mismatches $\lesssim 3\times10^{-4}$ over the mass range $2.25M_{\odot} \leq M \leq 300 M_{\odot}$. At high masses ($M\gtrsim40M_{\odot}$), where the merger and ringdown are more prominent, we show roughly two orders of magnitude improvement over existing waveform models. We also show that the surrogate works well even when extrapolated outside its training parameter space range, including at spins as large as 0.998. Finally, we show that this model accurately reproduces the spheroidal-spherical mode mixing present in the NR ringdown signal.
Comment: Matches PRD version. Model publicly available at https://zenodo.org/record/2549618#.XJvMrutKii4. 18 pages, 12 figures