Abstract
This paper explores the accuracy with which gravitational waves emitted in the coalescence of compact binaries need to be computed so that the inference of binary parameters from gravitational wave events will not be affected by systematic biases.
Highlights
Observations of gravitational waves (GWs) from coalescing compact object binaries have revolutionized our knowledge about the universe and provided access to astrophysics previously outside our grasp [1]
This is the expected behavior for a multimodal Gaussian which the posterior distribution is expected to follow in the high SNR limit, the 90% credible regions for some marginal 2D posteriors shown in the other panels are clearly not Gaussian
We provide a comparison between results obtained from two different waveform models, the agreement between these models and the source PN-numerical relativity (NR) waveforms and discuss the importance of limitations of the models in interpreting the parameter estimation results
Summary
Observations of gravitational waves (GWs) from coalescing compact object binaries have revolutionized our knowledge about the universe and provided access to astrophysics previously outside our grasp [1]. The currently available model waveforms, which approximates the solutions to the twobody problem in general relativity (GR), have been shown to be sufficiently accurate to not cause any systematic biases in the recovered parameters (masses, spins, location in the universe, etc.) for BBHs observed so far [19]. These “golden binaries,” stellar-mass BBHs like GW150914
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