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Energetics and phasing of nonprecessing spinning coalescing black hole binaries

Nagar, Alessandro and Damour, Thibault and Reisswig, Christian and Pollney, Denis (2016) Energetics and phasing of nonprecessing spinning coalescing black hole binaries. Physical Review D, 93 (4). Art. No. 044046. ISSN 2470-0010.

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We present an improved numerical relativity (NR) calibration of the new effective-one-body (EOB) model for coalescing nonprecessing spinning black hole binaries recently introduced by Damour and Nagar [Phys. Rev. D 90, 044018 (2014)]. We do so by comparing the EOB predictions to both the phasing and the energetics provided by two independent sets of NR data covering mass ratios 1 ≤ q ≤ 9.989 and dimensionless spin range −0.95 ≤ χ ≤ +0.994. One set of data is a subset of the Simulating eXtreme Spacetimes (SXS) catalog of public waveforms; the other set consists of new simulations obtained with the Llama code plus Cauchy characteristic evolution. We present the first systematic computation of the gauge-invariant relation between the binding energy and the total angular momentum, E_b (j), for a large sample of, spin-aligned, SXS and Llama data. The dynamics of the EOB model presented here involves only two free functional parameters, one [a^c_6 (ν)] entering the nonspinning sector, as a 5PN effective correction to the interaction potential, and one [c_3 (a_1, a_2, ν)] in the spinning sector, as an effective next-to-next-to-next-to-leading order correction to the spin-orbit coupling. These parameters are determined [together with a third functional parameter Δt_(NQC) (χ) entering the waveform] by comparing the EOB phasing with the SXS phasing, the consistency of the energetics being checked afterwards. The quality of the analytical model for gravitational wave data analysis purposes is assessed by computing the EOB/NR faithfulness. Over the NR data sample and when varying the total mass between 20 and 200 M⊙ the EOB/NR unfaithfulness (integrated over the NR frequency range) is found to vary between 99.493% and 99.984% with a median value of 99.944%.

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Additional Information:© 2016 American Physical Society. Received 28 June 2015; published 17 February 2016. We thank Andrea Taracchini, Alessandra Buonanno and the other authors of Ref. [11] for sharing with us the NR and EOB Eb(j) curves for χ=−0.95 and χ=+0.98; Michael Puerrer for useful comments on the first version of the manuscript; Sascha Husa for assistance in computing low eccentricity initial data; and Simone Balmelli for help with generating the data of Fig. 20. We finally thank Michael Boyle for having computed for us the data of Fig. 23 so as to approximately remove the drift of the center of mass. C. R. acknowledges support by NASA through Einstein Postdoctoral Fellowship Grant No. PF2-130099 awarded by the Chandra X-ray center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. NAS8-03060. Computations were performed using resources of the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center and NSF XSEDE (allocation TG-MCA02N014 and TG-PHY100033). Additional computations were performed on the Caltech computer cluster “Zwicky” (NSF MRI award No. PHY-0960291).
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NASA Einstein Postdoctoral FellowshipPF2-130099
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:65403
Deposited By: Tony Diaz
Deposited On:16 Mar 2016 23:00
Last Modified:16 Mar 2016 23:00

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