Probing ultralight dark matter with future ground-based gravitational-wave detectors

TL;DR

This paper investigates how future ground-based gravitational-wave detectors can detect or constrain ultralight bosonic dark matter by analyzing the gravitational waves emitted from black hole superradiance, especially considering higher modes.

Contribution

It extends previous research by analyzing higher modes in the gravitational wave background and evaluating the detection prospects with upcoming ground-based detectors.

Findings

Higher modes dominate the gravitational wave background for bosons with masses above 10^{-12} eV.

Future detectors could detect or constrain bosons in the mass range 7×10^{-14} to 2×10^{-11} eV.

Significant improvement over current LIGO and Virgo constraints is possible.

Abstract

Ultralight bosons are possible fundamental building blocks of nature, and promising dark matter candidates. They can trigger superradiant instabilities of spinning black holes (BHs) and form long-lived "bosonic clouds" that slowly dissipate energy through the emission of gravitational waves (GWs). Previous studies constrained ultralight bosons by searching for the stochastic gravitational wave background (SGWB) emitted by these sources in LIGO data, focusing on the most unstable dipolar and quadrupolar modes. Here we focus on scalar bosons and extend previous works by: (i) studying in detail the impact of higher modes in the SGWB; (ii) exploring the potential of future proposed ground-based GW detectors, such as the Neutron Star Extreme Matter Observatory, the Einstein Telescope and Cosmic Explorer, to detect this SGWB. We find that higher modes largely dominate the SGWB for bosons with masses $\gtrsim 10^{-12}$ eV, which is particularly relevant for future GW detectors. By estimating the signal-to-noise ratio of this SGWB, due to both stellar-origin BHs and from a hypothetical population of primordial BHs, we find that future ground-based GW detectors could observe or constrain bosons in the mass range $\sim [7\times 10^{-14}, 2\times 10^{-11}]$ eV and significantly improve on current and future constraints imposed by LIGO and Virgo observations.