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

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. We focus on scalar bosons and extend previous work 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 $\ensuremath{\gtrsim}{10}^{\ensuremath{-}12}\text{ }\text{ }\mathrm{eV}$, which will be particularly relevant for future GW detectors. By estimating the signal-to-noise ratio of this SGWB, both due to 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 $\ensuremath{\sim}[7\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}14},2\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}11}]\text{ }\text{ }\mathrm{eV}$ and significantly improve on the current and future constraints imposed by LIGO and Virgo observations.