Testing general relativity with gravitational waves: a reality check

TL;DR

This paper introduces a simple formula to evaluate the detectability of deviations from General Relativity in gravitational wave signals, aiding tests of gravity theories with current detectors.

Contribution

It provides a universal, easy-to-apply formula for estimating the signal-to-noise ratio needed to detect non-GR corrections in gravitational wave data.

Findings

Second-generation detectors can detect deviations of 1-10% from GR

The formula applies to various tests, including alternative theories and phenomenological models

It simplifies the assessment of gravitational wave tests for gravity theories

Abstract

The observations of gravitational-wave signals from astrophysical sources such as binary inspirals will be used to test General Relativity for self consistency and against alternative theories of gravity. I describe a simple formula that can be used to characterize the prospects of such tests, by estimating the matched-filtering signal-to-noise ratio required to detect non-General-Relativistic corrections of a given magnitude. The formula is valid for sufficiently strong signals; it requires the computation of a single number, the fitting factor between the General-Relativistic and corrected waveform families; and it can be applied to all tests that embed General Relativity in a larger theory, including tests of individual theories such as Brans-Dicke gravity, as well as the phenomenological schemes that introduce corrections and extra terms in the post-Newtonian phasing expressions of inspiral waveforms. The formula suggests that the volume-limited gravitational-wave searches performed with second-generation ground-based detectors would detect alternative-gravity corrections to General-Relativistic waveforms no smaller than 1-10% (corresponding to fitting factors of 0.9 to 0.99).