Limits on dark matter, ultralight scalars, and cosmic neutrinos with gyroscope spin and precision clocks

TL;DR

This paper uses gyroscope and clock measurements in space and on Earth to set new limits on dark matter density, cosmic neutrino overdensity, and scalar couplings, advancing tests of gravity and dark matter models at solar system scales.

Contribution

It introduces a novel approach combining gyroscope spin deviations and precision clock data to constrain dark matter, neutrino overdensity, and scalar interactions in the solar system.

Findings

Dark matter overdensity limit at Neptune's orbit: η ≲ 4.45×10^3

Cosmic neutrino overdensity bound: ξ ≲ 5.34×10^{10}

Scalar coupling constraint: g ≲ 7.09×10^{-24} for m_φ ≲ 1.32×10^{-18} eV

Abstract

Dark matter (DM) within the solar system induces deviations in the geodetic drift of gyroscope spin due to its gravitational interaction. Assuming a constant DM density as a minimal scenario, we constrain DM overdensity within the Gravity Probe B (GP-B) orbit and project limits for Earth's and Neptune's orbits around the Sun. The presence of electrons in gravitating sources and test objects introduces a scalar-mediated Yukawa potential, which can be probed using terrestrial and space--based precision clocks. We derive projected DM overdensity $(\eta)$ limits from Sagnac time measurements using onboard satellite clocks, highlighting their dependence on the source mass and orbital radius. The strongest limit, $\eta\lesssim 4.45\times 10^3$, is achieved at Neptune's orbit ($\sim 30~\mathrm{AU}$), exceeding existing constraints. Correspondingly, the cosmic neutrino overdensity is bounded as $\xi\lesssim 5.34\times 10^{10}$, surpassing results from KATRIN and cosmic ray studies. The best limit on electrophilic scalar coupling is $g\lesssim 7.09\times 10^{-24}$ for scalar mass $m_\varphi\lesssim 1.32\times 10^{-18}~\mathrm{eV}$ competitive with existing fifth-force bounds. These precision measurements offer a robust framework for testing gravity at solar system scales and probing DM in scenarios inaccessible to direct detection experiments.