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Surrogate model of hybridized numerical relativity binary black hole waveforms

Varma, V., Field, S., Scheel, M. A., Blackman, J., Kidder, L. E., & Pfeiffer, H. (2019). Surrogate model of hybridized numerical relativity binary black hole waveforms. Physical Review D, 99(6): 064045. doi:10.1103/PhysRevD.99.064045.

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Genre: Journal Article

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1812.07865.pdf (Preprint), 2MB
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Creators:
Varma, Vijay, Author
Field, Scott, Author
Scheel, Mark A., Author
Blackman, Jonathan, Author
Kidder, Lawrence E., Author
Pfeiffer, Harald1, Author
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290

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Free keywords: General Relativity and Quantum Cosmology, gr-qc
Abstract: 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-ringdown is 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.

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Dates: 2018-12-192019
Publication Status: Published in print
Pages: 17 pages, 12 figures
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Rev. Method: -
Identifiers: arXiv: 1812.07865
URI: http://arxiv.org/abs/1812.07865
DOI: 10.1103/PhysRevD.99.064045
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Title: Physical Review D
Source Genre: Journal
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Pages: - Volume / Issue: 99 (6) Sequence Number: 064045 Start / End Page: - Identifier: -