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  Accurate effective-one-body waveforms of inspiralling and coalescing black-hole binaries

Damour, T., Nagar, A., Hannam, M., Husa, S., & Brügmann, B. (2008). Accurate effective-one-body waveforms of inspiralling and coalescing black-hole binaries. Physical Review D, 78(4): 044039. doi:10.1103/PhysRevD.78.044039.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0013-13BE-A Version Permalink: http://hdl.handle.net/11858/00-001M-0000-0013-13C2-D
Genre: Journal Article

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 Creators:
Damour, Thibault1, 2, Author
Nagar, Alessandro1, 2, 3, Author
Hannam, Mark4, 5, Author
Husa, Sascha6, Author              
Brügmann, Bernd4, Author
Affiliations:
1External Organizations, Institut des Hautes Etudes Scientifiques, 91440 Bures-sur-Yvette, France , ou_persistent22              
2External Organizations, ICRANet, 65122 Pescara, Italy , ou_persistent22              
3External Organizations, INFN, sez. di Torino, Via P. Giuria 1, Torino, Italy , ou_persistent22              
4External Organizations, Theoretical Physics Institute, University of Jena, 07743, Jena, Germany , ou_persistent22              
5External Organizations, Physics Department, University College Cork, Cork, Ireland , ou_persistent22              
6Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, Golm, DE, ou_24013              

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 Abstract: The effective-one-body (EOB) formalism contains several flexibility parameters, notably a5, vpole, and [overline a]RR. We show here how to jointly constrain the values of these parameters by simultaneously best-fitting the EOB waveform to two, independent, numerical relativity (NR) simulations of inspiralling and/or coalescing binary black-hole systems: published Caltech-Cornell inspiral data (considered for gravitational wave frequencies Momega<=0.1) on one side, and newly computed coalescence data on the other side. The resulting, approximately unique, “best-fit” EOB waveform is then shown to exhibit excellent agreement with NR coalescence data for several mass ratios. The dephasing between this best-fit EOB waveform and published Caltech-Cornell inspiral data is found to vary between -0.0014 and +0.0008 radians over a time span of ~2464M up to gravitational wave frequency Momega=0.1, and between +0.0013 and -0.0185 over a time span of 96M after Momega=0.1 up to Momega=0.1565. The dephasings between EOB and the new coalescence data are found to be smaller than: (i) ±0.025 radians over a time span of 730M (11 cycles) up to merger, in the equal-mass case, and (ii) ±0.05 radians over a time span of about 950M (17 cycles) up to merger in the 2:1 mass-ratio case. These new results corroborate the aptitude of the EOB formalism to provide accurate representations of general relativistic waveforms, which are needed by currently operating gravitational wave detectors.

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 Dates: 2008-08-18
 Publication Status: Published online
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Title: Physical Review D
Source Genre: Journal
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Pages: - Volume / Issue: 78 (4) Sequence Number: 044039 Start / End Page: - Identifier: ISSN: 1089-4918