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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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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-002D-8CB3-C Version Permalink: http://hdl.handle.net/21.11116/0000-0002-F663-9
Genre: Journal Article

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 Creators:
Lange, Jacob, Author
O'Shaughnessy, Richard, Author
Boyle, Michael, Author
Bustillo, Juan Calderón, Author
Campanelli, Manuela, Author
Chu, Tony, Author
Clark, James A., Author
Demos, Nicholas, Author
Fong, Heather, Author
Healy, James, Author
Hemberger, Daniel, Author
Hinder, Ian1, Author              
Jani, Karan, Author
Khamesra, Bhavesh, Author
Kidder, Lawrence E., Author
Kumar, Prayush, Author
Laguna, Pablo, Author
Lousto, Carlos O., Author
Lovelace, Geoffrey, Author
Ossokine, Serguei1, Author
Pfeiffer, Harald1, AuthorScheel, Mark A., AuthorShoemaker, Deirdre, AuthorSzilagyi, Bela, AuthorTeukolsky, Saul, AuthorZlochower, Yosef, Author more..
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: 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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 Dates: 2017-05-272017
 Publication Status: Published in print
 Pages: 30 pages, 22 figures; submitted to PRD
 Publishing info: -
 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 1705.09833
URI: http://arxiv.org/abs/1705.09833
DOI: 10.1103/PhysRevD.96.104041
 Degree: -

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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: 96 Sequence Number: 104041 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: /journals/resource/111088197762258