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  Hierarchical data-driven approach to fitting numerical relativity data for nonprecessing binary black holes with an application to final spin and radiated energy

Jiménez-Forteza, X., Keitel, D., Husa, S., Hannam, M., Khan, S., & Pürrer, M. (2017). Hierarchical data-driven approach to fitting numerical relativity data for nonprecessing binary black holes with an application to final spin and radiated energy. Physical Review D, 95: 064024. doi:10.1103/PhysRevD.95.064024.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-002D-21AB-C Version Permalink: http://hdl.handle.net/11858/00-001M-0000-002E-07E5-B
Genre: Journal Article

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1611.00332.pdf (Preprint), 7MB
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 Creators:
Jiménez-Forteza, Xisco, Author
Keitel, David, Author
Husa, Sascha, Author
Hannam, Mark, Author
Khan, Sebastian1, Author              
Pürrer, Michael2, Author              
Affiliations:
1Binary Merger Observations and Numerical Relativity, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, escidoc:2461691              
2Astrophysical 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, High Energy Astrophysical Phenomena, astro-ph.HE
 Abstract: Numerical relativity is an essential tool in studying the coalescence of binary black holes (BBHs). It is still computationally prohibitive to cover the BBH parameter space exhaustively, making phenomenological fitting formulas for BBH waveforms and final-state properties important for practical applications. We describe a general hierarchical bottom-up fitting methodology to design and calibrate fits to numerical relativity simulations for the three-dimensional parameter space of quasicircular nonprecessing merging BBHs, spanned by mass ratio and by the individual spin components orthogonal to the orbital plane. Particular attention is paid to incorporating the extreme-mass-ratio limit and to the subdominant unequal-spin effects. As an illustration of the method, we provide two applications, to the final spin and final mass (or equivalently: radiated energy) of the remnant black hole. Fitting to 427 numerical relativity simulations, we obtain results broadly consistent with previously published fits, but improving in overall accuracy and particularly in the approach to extremal limits and for unequal-spin configurations. We also discuss the importance of data quality studies when combining simulations from diverse sources, how detailed error budgets will be necessary for further improvements of these already highly accurate fits, and how this first detailed study of unequal-spin effects helps in choosing the most informative parameters for future numerical relativity runs.

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 Dates: 2016-11-012017-03-272017
 Publication Status: Published in print
 Pages: 23 pages, 31 figures, 15 tables; data and example implementations as supplementary material. Updated to match PRD version
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 Rev. Method: -
 Identifiers: arXiv: 1611.00332
DOI: 10.1103/PhysRevD.95.064024
URI: http://arxiv.org/abs/1611.00332
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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: 95 Sequence Number: 064024 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: http://pubman.mpdl.mpg.de/cone/journals/resource/111088197762258