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  Parameter Estimation Method that Directly Compares Gravitational Wave Observations to Numerical Relativity

Lange, J., O'Shaughnessy, R., Boyle, M., Bustillo, J. C., Campanelli, M., Chu, T., et al. (2017). Parameter Estimation Method that Directly Compares Gravitational Wave Observations to Numerical Relativity. Physical Review D, 96: 104041. doi:10.1103/PhysRevD.96.104041.

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 Urheber:
Lange, Jacob, Autor
O'Shaughnessy, Richard, Autor
Boyle, Michael, Autor
Bustillo, Juan Calderón, Autor
Campanelli, Manuela, Autor
Chu, Tony, Autor
Clark, James A., Autor
Demos, Nicholas, Autor
Fong, Heather, Autor
Healy, James, Autor
Hemberger, Daniel, Autor
Hinder, Ian1, Autor           
Jani, Karan, Autor
Khamesra, Bhavesh, Autor
Kidder, Lawrence E., Autor
Kumar, Prayush, Autor
Laguna, Pablo, Autor
Lousto, Carlos O., Autor
Lovelace, Geoffrey, Autor
Ossokine, Serguei1, Autor
Pfeiffer, Harald1, AutorScheel, Mark A., AutorShoemaker, Deirdre, AutorSzilagyi, Bela, AutorTeukolsky, Saul, AutorZlochower, Yosef, Autor mehr..
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290              

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Schlagwörter: General Relativity and Quantum Cosmology, gr-qc
 Zusammenfassung: We present and assess a Bayesian method to interpret gravitational wave signals from binary black holes. Our method directly compares gravitational wave data to numerical relativity simulations. This procedure bypasses approximations used in semi-analytical models for compact binary coalescence. In this work, we use only the full posterior parameter distribution for generic nonprecessing binaries, drawing inferences away from the set of NR simulations used, via interpolation of a single scalar quantity (the marginalized log-likelihood, $\ln {\cal L}$) evaluated by comparing data to nonprecessing binary black hole simulations. We also compare the data to generic simulations, and discuss the effectiveness of this procedure for generic sources. We specifically assess the impact of higher order modes, repeating our interpretation with both $l\le2$ as well as $l\le3$ harmonic modes. Using the $l\le3$ higher modes, we gain more information from the signal and can better constrain the parameters of the gravitational wave signal. We assess and quantify several sources of systematic error that our procedure could introduce, including simulation resolution and duration; most are negligible. We show through examples that our method can recover the parameters for equal mass, zero spin; GW150914-like; and unequal mass, precessing spin sources. Our study of this new parameter estimation method demonstrates we can quantify and understand the systematic and statistical error. This method allows us to use higher order modes from numerical relativity simulations to better constrain the black hole binary parameters.

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 Datum: 2017-05-272017
 Publikationsstatus: Erschienen
 Seiten: 30 pages, 22 figures; submitted to PRD
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Titel: Physical Review D
  Andere : Phys. Rev. D.
Genre der Quelle: Zeitschrift
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Ort, Verlag, Ausgabe: Lancaster, Pa. : American Physical Society
Seiten: - Band / Heft: 96 Artikelnummer: 104041 Start- / Endseite: - Identifikator: ISSN: 0556-2821
CoNE: https://pure.mpg.de/cone/journals/resource/111088197762258