Measurement of the central Galactic black hole by extremely large mass-ratio inspirals

TL;DR

This paper demonstrates that gravitational wave signals from extremely large mass-ratio inspirals can precisely measure the mass, spin, and deviation parameters of the Galactic Center black hole, enhancing our understanding of its properties.

Contribution

The study introduces simulations of X-MRI gravitational waves using a specific metric, showing high-precision parameter estimation with current models and potential improvements with more observations.

Findings

Mass, spin, and deviation parameters can be measured with high accuracy (~10^{-5} - 10^{-6}) from a single X-MRI event.

Parameter measurement accuracy improves with additional X-MRI observations.

Simulations use an axisymmetric Konoplya-Rezzolla-Zhidenko metric to model gravitational wave signals.

Abstract

In the Galaxy, extremely large mass-ratio inspirals(X-MRIs) composed of brown dwarfs and the massive black hole at the Galactic Center are expected to be promising gravitational wave sources for space-borne detectors. In this work, we simulate the gravitational wave signals from twenty X-MRI systems by an axisymmetric Konoplya-Rezzolla-Zhidenko metric with varied parameters. We find that the mass, spin, and deviation parameters of the Kerr black hole could be determined accurately ( $\sim 10^{-5} - 10^{-6}$ ) with only one X-MRI event with a high signal-to-noise ratio. The measurement of the above parameters could be improved with more X-MRI observations.