Constraining modified theories of gravity through the detection of one extremely large mass-ratio inspiral

TL;DR

This paper explores how gravitational waves from extremely large mass-ratio inspirals can be used to test and constrain modified theories of gravity, specifically Chern-Simons theory, with high precision.

Contribution

It demonstrates that XMRIs can effectively constrain the Chern-Simons parameter and recover system parameters with high accuracy using Bayesian methods.

Findings

XMRIs can constrain the Chern-Simons parameter to levels of 10^{-1} to 10^{-6}.

Parameter estimation accuracy reaches 10^{-3} for most intrinsic parameters.

Almost all parameters can be recovered within 1σ confidence interval.

Abstract

Extremely large mass-ratio inspirals (XMRIs), formed by brown dwarfs inspiraling into a massive black hole, emit gravitational waves (GWs) that fall within the detection band of future space-borne detectors such as LISA, TianQin, and Taiji. Their detection will measure the astrophysical properties of the MBH in the center of our galaxy (SgrA$^\ast$) with unprecedented accuracy and provide a unique probe of gravity in the strong field regime. Here, we estimate the benefit of using the GWs from XMRIs to constrain the Chern-Simons theory. Our results show that XMRI signals radiated from the late stages of the evolution are particularly sensitive to differences between Chern-Simons theory and general relativity. For low-eccentricity sources, XMRIs can put bounds on the Chern-Simons parameter $\zeta$ at the level of $10^{-1}$ to an accuracy of $10^{-3}$. For high-eccentricity sources, XMRIs can put bounds on the parameter $\zeta$ at the level of $10^{-1}$ to an accuracy of $10^{-6}$. Furthermore, using the time-frequency MCMC method, we obtain the posterior distribution of XMRIs in the Chern-Simons theory. Our results show that almost all the parameters can be recovered within $1\sigma$ confidence interval. For most of the intrinsic parameters, the estimation accuracy reaches $10^{-3}$. For the brown dwarf mass, the estimation accuracy reaches $10^{-1}$, while for $\zeta$, the estimation accuracy reaches $\Delta\log_{10}\zeta=0.08$ for high eccentricity sources and 1.27 for low eccentricity sources.