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Researchers have developed an improved Bayesian statistical method to search for ultralight dark matter particles using precision measurements of pulsar timing. The study establishes new constraints on both scalar and vector dark matter in mass ranges between 10^-23 eV and 10^-21 eV by analyzing how these hypothetical particles would affect the orbits of pulsars in binary systems. Their approach avoids artificial overestimation of sensitivity by properly accounting for uncertain orbital parameters, yielding results comparable to current laboratory and space-based experiments.
Why it matters
This work opens a new experimental window to detect dark matter candidates that are too light to be found by traditional particle physics experiments. If ultralight bosonic dark matter exists, pulsar timing arrays could provide independent confirmation alongside other detection methods, helping solve one of physics' most fundamental mysteries about the nature of dark matter.
Understand the Science
arXiv:2604.26092v2 Announce Type: replace
Abstract: If dark matter consists of ultralight bosons, on galactic scales it can be effectively described as a coherent classical field experiencing oscillations. Such a field could perturb the dynamics of celestial bodies via a direct coupling to ordinary matter, introducing signatures detectable through high-precision pulsar timing analysis. In this work, we extend a two-step Bayesian inference framework, originally developed for linearly coupled scalar ultralight dark matter (ULDM), to probe a quadratic scalar coupling and spin-1 vector dark matter. By explicitly marginalising over nuisance orbital parameters, our approach provides robust sensitivity limits that avoid the artificial overestimation often associated with direct fitting techniques. For quadratic scalar ULDM, we establish new constraints on the coupling $beta$ for masses between $2 times 10^{-22}$ eV and $2 times 10^{-21}$ eV inaccessible to other experiments, while identifying mass regimes where the sensitivity is dominated by the orbital phase $Psi’$ or the projected semi-major axis $x$. For vector ULDM, we characterize resonant signatures present even in circular orbits and obtain bounds on the coupling $g$ within the $10^{-23}$ eV to $10^{-18}$ eV range, yielding results within the same orders of magnitude as current laboratory and space-based experiments.
Source: Sensitivity of binary pulsar timing to spin-0 and spin-1 ultralight dark matter