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Universal features of gravitational waves emitted by superkick binary black hole systems

Ma, Sizheng and Giesler, Matthew and Varma, Vijay and Scheel, Mark A. and Chen, Yanbei (2021) Universal features of gravitational waves emitted by superkick binary black hole systems. Physical Review D, 104 (8). Art. No. 084003. ISSN 2470-0010. doi:10.1103/physrevd.104.084003.

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We use numerical relativity to study the merger and ringdown stages of “superkick” binary black hole systems (those with equal mass and antiparallel spins). We find a universal way to describe the mass and current quadrupole gravitational waves emitted by these systems during the merger and ringdown stage: (i) The time evolutions of these waves are insensitive to the progenitor’s parameters (spins) after being normalized by their own peak values. (ii) The peak values, which encode all the spin information of the progenitor, can be consistently fitted to formulas inspired by post-Newtonian theory. We find that the universal evolution of the mass quadrupole wave can be accurately modeled by the so-called Backwards One-Body (BOB) model. However, the BOB model, in its present form, leads to a lower waveform match and a significant parameter-estimation bias for the current quadrupole wave. We also decompose the ringdown signal into seven overtones, and study the dependence of mode amplitudes on the progenitor’s parameters. Such dependence is found to be insensitive to the overtone index (up to a scaling factor). Finally, we use the Fisher matrix technique to investigate how the ringdown waveform can be at least as important for parameter estimation as the inspiral stage. Assuming the Cosmic Explorer, we find the contribution of ringdown portion dominates as the total mass exceeds ∼250 M_⊙. For massive binary black hole (BBH) systems, the accuracy of parameter measurement is improved by incorporating the information of ringdown—the ringdown sector gives rise to a different parameter correlation from inspiral stage; hence, the overall parameter correlation is reduced in full signal.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Ma, Sizheng0000-0002-4645-453X
Giesler, Matthew0000-0003-2300-893X
Varma, Vijay0000-0002-9994-1761
Scheel, Mark A.0000-0001-6656-9134
Chen, Yanbei0000-0002-9730-9463
Additional Information:© 2021 American Physical Society. (Received 10 July 2021; accepted 9 August 2021; published 1 October 2021) We want to thank Serguei Ossokine, Alvin Chua, Gregorio Carullo, and Sean McWilliams for useful discussions. S. M. and Y. C. are supported by the Simons Foundation (Grant No. 568762), the Brinson Foundation, and the National Science Foundation (Grants No. PHY–2011968, No. PHY–2011961, and No. PHY–1836809). V. V. is generously supported by a Klarman Fellowship at Cornell, the Sherman Fairchild Foundation, and NSF Grants No. PHY–170212 and No. PHY–1708213 at Caltech. The computations presented here were conducted on the Caltech High Performance Cluster, partially supported by a grant from the Gordon and Betty Moore Foundation.
Group:TAPIR, Astronomy Department
Funding AgencyGrant Number
Simons Foundation568762
Brinson FoundationUNSPECIFIED
Cornell UniversityUNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
Gordon and Betty Moore FoundationUNSPECIFIED
Issue or Number:8
Record Number:CaltechAUTHORS:20211014-212144527
Persistent URL:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:111455
Deposited By: George Porter
Deposited On:18 Oct 2021 18:11
Last Modified:28 Apr 2023 20:37

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