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Published January 15, 2017 | Published + Submitted
Journal Article Open

Complete waveform model for compact binaries on eccentric orbits


We present a time domain waveform model that describes the inspiral, merger and ringdown of compact binary systems whose components are nonspinning, and which evolve on orbits with low to moderate eccentricity. The inspiral evolution is described using third-order post-Newtonian equations both for the equations of motion of the binary, and its far-zone radiation field. This latter component also includes instantaneous, tails and tails-of-tails contributions, and a contribution due to nonlinear memory. This framework reduces to the post-Newtonian approximant TaylorT4 at third post-Newtonian order in the zero-eccentricity limit. To improve phase accuracy, we also incorporate higher-order post-Newtonian corrections for the energy flux of quasicircular binaries and gravitational self-force corrections to the binding energy of compact binaries. This enhanced prescription for the inspiral evolution is combined with a fully analytical prescription for the merger-ringdown evolution constructed using a catalog of numerical relativity simulations. We show that this inspiral-merger-ringdown waveform model reproduces the effective-one-body model of Ref. [Y. Pan et al., Phys. Rev. D 89, 061501 (2014).] for quasicircular black hole binaries with mass ratios between 1 to 15 in the zero-eccentricity limit over a wide range of the parameter space under consideration. Using a set of eccentric numerical relativity simulations, not used during calibration, we show that our new eccentric model reproduces the true features of eccentric compact binary coalescence throughout merger. We use this model to show that the gravitational-wave transients GW150914 and GW151226 can be effectively recovered with template banks of quasicircular, spin-aligned waveforms if the eccentricity e_0 of these systems when they enter the a LIGO band at a gravitational-wave frequency of 14 Hz satisfies e^(GW150914)_0 ≤ 0.15 and e^(GW151226) _0 ≤ 0.1. We also find that varying the spin combinations of the quasicircular, spin-aligned template waveforms does not improve the recovery of nonspinning, eccentric signals when e_0 ≥ 0.1. This suggests that these two signal manifolds are predominantly orthogonal.

Additional Information

© 2017 American Physical Society. Received 19 September 2016; published 31 January 2017. We thank Mark Fredricksen, Campus Cluster Administrator at National Center for Supercomputing Applications (NCSA), for his help configuring UIUC's campus cluster to obtain some of the computations presented in this article. B. A. and W. R. gratefully acknowledge a Students Pushing Innovation (SPIN) internship from NCSA. We thank Gabrielle Allen, Haris Markakis and Ed Seidel for fruitful interactions and comments on the article. We thank Andrea Taracchini and Zhoujian Cao for reviewing this manuscript and providing suggestions to improve it. We also thank Sean McWilliams for comments on the IRS model. We gratefully acknowledge support for this research at Canadian Institute for Theoretical Astrophysics (CITA) from Natural Sciences and Engineering Research Council of Canada (NSERC), the Ontario Early Researcher Awards Program, the Canada Research Chairs Program, and the Canadian Institute for Advanced Research; at Caltech from the Sherman Fairchild Foundation and National Science Foundation (NSF) Grants No. PHY-1404569 and No. AST-1333520; at Cornell from the Sherman Fairchild Foundation and NSF Grants No. PHY-1306125 and No. AST-1333129; and at Princeton from NSF Grant No. PHY-1305682 and the Simons Foundation. Calculations were performed at the General Purpose Cluster (GPC) supercomputer at the SciNet HPC Consortium [118]; SciNet is funded by: the Canada Foundation for Innovation (CFI) under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund (ORF)—Research Excellence; and the University of Toronto. Further calculations were performed on the Briarée cluster at Sherbrooke University, managed by Calcul Québec and Compute Canada and with operation funded by the Canada Foundation for Innovation (CFI), Ministére de l'Économie, de l'Innovation et des Exportations du Quebec (MEIE), Réseau de médecine génétique appliquée (RMGA) and the Fonds de recherche du Québec—Nature et Technologies (FRQ-NT); on the Zwicky cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by NSF Grant No. PHY-0960291; on the NSF XSEDE network under Grant No. TG-PHY990007N; on the NSF/NCSA Blue Waters at the University of Illinois with allocation jr6 under NSF PRAC Grant No. ACI-1440083. This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (Grants No. OCI-0725070 and No. ACI-1238993) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. This article has LIGO Document number P1600186.

Attached Files

Submitted - 1609.05933v1.pdf

Published - PhysRevD.95.024038.pdf


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August 19, 2023
August 19, 2023