TY - JOUR
T1 - Compact binary coalescences
T2 - constraints on waveforms
AU - Ashtekar, Abhay
AU - De Lorenzo, Tommaso
AU - Khera, Neev
N1 - Funding Information:
We would like to thank K. G. Arun, A. Gupta, and B. Sathyaprakash for comments on the manuscript; Bala Iyer and Luc Blanchet for extensive correspondence on the PN methods; Alessandra Buonanno for discussions on EOB, and Larry Kidder, on NR; and Badri Krishnan for several detailed discussions on waveforms in general and Phenom models in particular. We are also indebted to participants of the APS meeting in Denver, IGC@25 conference at Penn State, GR22/Amaldi13 conference in Valencia, and the Discussion meeting on Future of Gravitational Waves at ICTS, Bangalore for questions and suggestions. This work was supported in part by the NSF Grant PHY-1806356, Grant UN2017-92945 from the Urania Stott Fund of Pittsburgh Foundation and the Eberly research funds of Penn State.
Funding Information:
We would like to thank K. G. Arun, A. Gupta, and B. Sathyaprakash for comments on the manuscript; Bala Iyer and Luc Blanchet for extensive correspondence on the PN methods; Alessandra Buonanno for discussions on EOB, and Larry Kidder, on NR; and Badri Krishnan for several detailed discussions on waveforms in general and Phenom models in particular. We are also indebted to participants of the APS meeting in Denver, IGC@25 conference at Penn State, GR22/Amaldi13 conference in Valencia, and the Discussion meeting on Future of Gravitational Waves at ICTS, Bangalore for questions and suggestions. This work was supported in part by the NSF Grant PHY-1806356, Grant UN2017-92945 from the Urania Stott Fund of Pittsburgh Foundation and the Eberly research funds of Penn State.
Publisher Copyright:
© 2020, Springer Science+Business Media, LLC, part of Springer Nature.
PY - 2020/11/1
Y1 - 2020/11/1
N2 - Gravitational waveforms for compact binary coalescences (CBCs) have been invaluable for detections by the LIGO-Virgo collaboration. They are obtained by a combination of semi-analytical models and numerical simulations. So far systematic errors arising from these procedures appear to be less than statistical ones. However, the significantly enhanced sensitivity of the new detectors that will become operational in the near future will require waveforms to be much more accurate. This task would be facilitated if one has a variety of cross-checks to evaluate accuracy, particularly in the regions of parameter space where numerical simulations are sparse. Currently errors are estimated by comparing the candidate waveforms with the numerical relativity (NR) ones, which are taken to be exact. The goal of this paper is to propose a qualitatively different tool. We show that full non-linear general relativity (GR) imposes an infinite number of sharp constraints on the CBC waveforms. These can provide clear-cut measures to evaluate the accuracy of candidate waveforms against exact GR, help find systematic errors, and also provide external checks on NR simulations themselves.
AB - Gravitational waveforms for compact binary coalescences (CBCs) have been invaluable for detections by the LIGO-Virgo collaboration. They are obtained by a combination of semi-analytical models and numerical simulations. So far systematic errors arising from these procedures appear to be less than statistical ones. However, the significantly enhanced sensitivity of the new detectors that will become operational in the near future will require waveforms to be much more accurate. This task would be facilitated if one has a variety of cross-checks to evaluate accuracy, particularly in the regions of parameter space where numerical simulations are sparse. Currently errors are estimated by comparing the candidate waveforms with the numerical relativity (NR) ones, which are taken to be exact. The goal of this paper is to propose a qualitatively different tool. We show that full non-linear general relativity (GR) imposes an infinite number of sharp constraints on the CBC waveforms. These can provide clear-cut measures to evaluate the accuracy of candidate waveforms against exact GR, help find systematic errors, and also provide external checks on NR simulations themselves.
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U2 - 10.1007/s10714-020-02764-1
DO - 10.1007/s10714-020-02764-1
M3 - Article
AN - SCOPUS:85095595766
SN - 0001-7701
VL - 52
JO - General Relativity and Gravitation
JF - General Relativity and Gravitation
IS - 11
M1 - 107
ER -