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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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Datensatz-Permalink: http://hdl.handle.net/11858/00-001M-0000-002E-9B65-1 Versions-Permalink: http://hdl.handle.net/21.11116/0000-0000-B003-5
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American Physical Society
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 Urheber:
Huerta, E. A., Autor
Moore, C. J., Autor
Kumar, Prayush, Autor
George, Daniel, Autor
Chua, Alvin J. K., Autor
Haas, Roland, Autor
Wessel, Erik, Autor
Johnson, Daniel, Autor
Glennon, Derek, Autor
Rebei, Adam, Autor
Holgado, A. Miguel, Autor
Gair, Jonathan R., Autor
Pfeiffer, Harald1, Autor              
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290              

Inhalt

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Schlagwörter: 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
 Zusammenfassung: 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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 Datum: 2017-11-162018
 Publikationsstatus: Im Druck publiziert
 Seiten: 17 pages, 9 figures, 1 Appendix. Submitted to Phys. Rev. D
 Ort, Verlag, Ausgabe: -
 Inhaltsverzeichnis: -
 Art der Begutachtung: -
 Identifikatoren: arXiv: 1711.06276
URI: http://arxiv.org/abs/1711.06276
DOI: 10.1103/PhysRevD.97.024031
 Art des Abschluß: -

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Titel: Physical Review D
  Andere : Phys. Rev. D.
Genre der Quelle: Zeitschrift
 Urheber:
Affiliations:
Ort, Verlag, Ausgabe: Lancaster, Pa. : American Physical Society
Seiten: - Band / Heft: 97 Artikelnummer: 024031 Start- / Endseite: - Identifikator: ISSN: 0556-2821
CoNE: /journals/resource/111088197762258