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  Eccentric, nonspinning, inspiral, Gaussian-process merger approximant for the detection and characterization of eccentric binary black hole mergers

Huerta, E. A., Moore, C. J., Kumar, P., George, D., Chua, A. J. K., Haas, R., et al. (2018). Eccentric, nonspinning, inspiral, Gaussian-process merger approximant for the detection and characterization of eccentric binary black hole mergers. Physical Review D, 97: 024031. doi:10.1103/PhysRevD.97.024031.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-002E-9B65-1 Version Permalink: http://hdl.handle.net/21.11116/0000-0000-B003-5
Genre: Journal Article

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 Creators:
Huerta, E. A., Author
Moore, C. J., Author
Kumar, Prayush, Author
George, Daniel, Author
Chua, Alvin J. K., Author
Haas, Roland, Author
Wessel, Erik, Author
Johnson, Daniel, Author
Glennon, Derek, Author
Rebei, Adam, Author
Holgado, A. Miguel, Author
Gair, Jonathan R., Author
Pfeiffer, Harald1, Author              
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, escidoc:1933290              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc,Astrophysics, Cosmology and Extragalactic Astrophysics, astro-ph.CO, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,Computer Science, Computational Engineering, Finance, and Science, cs.CE
 Abstract: We present $\texttt{ENIGMA}$, a time domain, inspiral-merger-ringdown waveform model that describes non-spinning binary black holes systems that evolve on moderately eccentric orbits. The inspiral evolution is described using a consistent combination of post-Newtonian theory, self-force and black hole perturbation theory. Assuming moderately eccentric binaries that circularize prior to coalescence, we smoothly match the eccentric inspiral with a stand-alone, quasi-circular merger, which is constructed using machine learning algorithms that are trained with quasi-circular numerical relativity waveforms. We show that $\texttt{ENIGMA}$ reproduces with excellent accuracy the dynamics of quasi-circular compact binaries. We validate $\texttt{ENIGMA}$ using a set of $\texttt{Einstein Toolkit}$ eccentric numerical relativity waveforms, which describe eccentric binary black hole mergers with mass-ratios between $1 \leq q \leq 5.5$, and eccentricities $e_0 \lesssim 0.2$ ten orbits before merger. We use this model to explore in detail the physics that can be extracted with moderately eccentric, non-spinning binary black hole mergers. In particular, we use $\texttt{ENIGMA}$ to show that the gravitational wave transients GW150914, GW151226, GW170104 and GW170814 can be effectively recovered with spinning, quasi-circular templates if the eccentricity of these events at a gravitational wave frequency of 10Hz satisfies $e_0\leq \{0.175,\, 0.125,\,0.175,\,0.175\}$, respectively. We show that if these systems have eccentricities $e_0\sim 0.1$ at a gravitational wave frequency of 10Hz, they can be misclassified as quasi-circular binaries due to parameter space degeneracies between eccentricity and spin corrections.

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 Dates: 2017-11-162018
 Publication Status: Published in print
 Pages: 17 pages, 9 figures, 1 Appendix. Submitted to Phys. Rev. D
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 Rev. Method: -
 Identifiers: arXiv: 1711.06276
URI: http://arxiv.org/abs/1711.06276
DOI: 10.1103/PhysRevD.97.024031
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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: 97 Sequence Number: 024031 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: http://pubman.mpdl.mpg.de/cone/journals/resource/111088197762258