Gravitational wave inference on a numerical-relativity simulation of a black hole merger beyond general relativity. (arXiv:2208.02805v1 [gr-qc])

<a href="http://arxiv.org/find/gr-qc/1/au:+Okounkova_M/0/1/0/all/0/1">Maria Okounkova</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Isi_M/0/1/0/all/0/1">Maximiliano Isi</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Chatziioannou_K/0/1/0/all/0/1">Katerina Chatziioannou</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Farr_W/0/1/0/all/0/1">Will M. Farr</a>

We apply common gravitational wave inference procedures on binary black hole

merger waveforms from a theory of gravity beyond general relativity. We

consider dynamical Chern-Simons gravity, a modified theory of gravity with

origins in string theory and loop quantum gravity. This theory introduces an

additional parameter $ell$, corresponding to the length-scale below which

quantum gravity effects become important. We simulate data based on numerical

relativity waveforms produced under this theory that differ from the

predictions of general relativity in the strongly nonlinear merger regime. We

consider a system with parameters similar to GW150914 with different values of

$ell$ and signal-to-noise ratios. We perform two analyses of the simulated

data. The first is a template-based analysis that uses waveforms derived under

general relativity and allows us to identify degeneracies between waveforms

predicted by the two theories of gravity. The second is a

morphology-independent analysis based on BayesWave that does not assume that

the signal is consistent with general relativity. Under the BayesWave analysis,

the simulated signals can be faithfully reconstructed. However, waveform models

derived under general relativity are unable to fully mimic the simulated

modified-gravity signals and such a deviation would be identifiable with

existing inference tools. Depending on the magnitude of the deviation $ell$,

we find that the templated analysis can under perform the

morphology-independent analysis in fully recovering simulated beyond-GR

waveforms even for achievable signal-to-noise ratios $gtrsim 20{-}30$.

We apply common gravitational wave inference procedures on binary black hole

merger waveforms from a theory of gravity beyond general relativity. We

consider dynamical Chern-Simons gravity, a modified theory of gravity with

origins in string theory and loop quantum gravity. This theory introduces an

additional parameter $ell$, corresponding to the length-scale below which

quantum gravity effects become important. We simulate data based on numerical

relativity waveforms produced under this theory that differ from the

predictions of general relativity in the strongly nonlinear merger regime. We

consider a system with parameters similar to GW150914 with different values of

$ell$ and signal-to-noise ratios. We perform two analyses of the simulated

data. The first is a template-based analysis that uses waveforms derived under

general relativity and allows us to identify degeneracies between waveforms

predicted by the two theories of gravity. The second is a

morphology-independent analysis based on BayesWave that does not assume that

the signal is consistent with general relativity. Under the BayesWave analysis,

the simulated signals can be faithfully reconstructed. However, waveform models

derived under general relativity are unable to fully mimic the simulated

modified-gravity signals and such a deviation would be identifiable with

existing inference tools. Depending on the magnitude of the deviation $ell$,

we find that the templated analysis can under perform the

morphology-independent analysis in fully recovering simulated beyond-GR

waveforms even for achievable signal-to-noise ratios $gtrsim 20{-}30$.

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