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  Eccentric binary black hole inspiral-merger-ringdown gravitational waveform model from numerical relativity and post-Newtonian theory

Hinder, I., Kidder, L. E., & Pfeiffer, H. (2018). Eccentric binary black hole inspiral-merger-ringdown gravitational waveform model from numerical relativity and post-Newtonian theory. Physical Review D, 98: 044015. doi:10.1103/PhysRevD.98.044015.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0000-6390-D Version Permalink: http://hdl.handle.net/21.11116/0000-0002-ED2D-2
Genre: Journal Article

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Hinder, Ian1, Author              
Kidder, Lawrence E., Author
Pfeiffer, Harald1, Author              
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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: We present a prescription for computing gravitational waveforms for the inspiral, merger and ringdown of non-spinning eccentric binary black hole systems. The inspiral waveform is computed using the post-Newtonian expansion and the merger waveform is computed by interpolating a small number of quasi-circular NR waveforms. The use of circular merger waveforms is possible because eccentric binaries circularize in the last few cycles before the merger, which we demonstrate up to mass ratio $q = m_1/m_2 = 3$. The complete model is calibrated to 23 numerical relativity (NR) simulations starting ~20 cycles before the merger with eccentricities $e_\text{ref} \le 0.08$ and mass ratios $q \le 3$, where $e_\text{ref}$ is the eccentricity ~7 cycles before the merger. The NR waveforms are long enough that they start above 30 Hz (10 Hz) for BBH systems with total mass $M \ge 80 M_\odot$ ($230 M_\odot$). We find that, for the sensitivity of advanced LIGO at the time of its first observing run, the eccentric model has a faithfulness with NR of over 97% for systems with total mass $M \ge 85 M_\odot$ across the parameter space ($e_\text{ref} \le 0.08, q \le 3$). For systems with total mass $M \ge 70 M_\odot$, the faithfulness is over 97% for $e_\text{ref} \lesssim 0.05$ and $q \le 3$. The NR waveforms and the Mathematica code for the model are publicly available.

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 Dates: 2017-09-062018
 Publication Status: Published in print
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 Rev. Method: -
 Identifiers: arXiv: 1709.02007
URI: http://arxiv.org/abs/1709.02007
DOI: 10.1103/PhysRevD.98.044015
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Title: Physical Review D
  Other : Phys. Rev. D.
Source Genre: Journal
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Publ. Info: Lancaster, Pa. : American Physical Society
Pages: - Volume / Issue: 98 Sequence Number: 044015 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: /journals/resource/111088197762258