LIGO Document P1500144-v3
- A frequentist asymptotic expansion method for error estimation is employed for a network of gravitational wave detectors to assess the amount of information that can be extracted from gravitational wave observations. Mathematically we derive lower bounds in the errors that any parameter estimator will have in the absence of prior knowledge to distinguish between the post-Einsteinian (ppE) description of coalescing binary systems and that of general relativity. When such errors are smaller than the parameter value, there is possibility to detect these violations from GR. A parameter space with inclusion of dominant dephasing ppE parameters \( (\beta, b) \) is used for a study of first- and second-order (co)variance expansions, focusing on the inspiral stage of a nonspinning binary system of zero eccentricity detectible through Advanced LIGO and Advanced Virgo. Our procedure is an improvement of the Cramer-Rao Lower Bound. When Bayesian errors are lower than our bound it means that they depend critically on the priors. The analysis indicates the possibility of constraining deviations from GR in inspiral SNR (\( \rho \sim 15-17 \)) regimes that are achievable in upcoming scientific runs (GW150914 had an inspiral SNR \( \sim 12 \)). The errors on \( \beta \) also increase errors of other parameters such as the chirp mass \( \mathcal{M} \) and symmetric mass ratio \( \eta \). Application is done to existing alternative theories of gravity, which include modified dispersion relation of the waveform, non-spinning models of quadratic modified gravity, and dipole gravitational radiation (i.e., Brans-Dicke type) modifications
- Update version accepted to PRD.
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