New Limits on Axionic Dark Matter from the Magnetar PSR J1745-2900

TL;DR

This study uses radio spectra from the Galactic Center magnetar PSR J1745-2900 to set new constraints on axionic dark matter, excluding certain axion models within specific mass and coupling ranges.

Contribution

It provides the first limits on axionic dark matter from magnetar observations, extending the mass and coupling parameter space beyond previous terrestrial experiments.

Findings

Excluded axion models with specific coupling strengths over multiple mass ranges.

Set stronger limits assuming a maximal dark matter cusp near Sgr A*.

No significant spectral features detected in the 4.1-165.6 μeV range.

Abstract

Axions are a promising dark matter candidate that were motivated to solve the strong CP problem and that may also address the cosmological matter-antimatter asymmetry. Axion-photon conversion is possible in the presence of the strong magnetic fields, and the photon so produced will have energy equal to the axion mass. Here we report new limits on axionic dark matter obtained from radio spectra of the Galactic Center magnetar PSR J1745-2900. The magnetar has a magnetic field of $1.6\times10^{14}$ G that interacts with a dark matter density $2\times10^5$ to $2\times10^9$ times greater than the local dark matter encountered by terrestrial haloscopes, depending on the Galactic dark matter profile. No significant spectral features are detected across 62% of the axion mass range 4.1-165.6 $\mu$eV (1-40 GHz). The interpretation of flux limits into limits on the two-photon coupling strength $g_{a\gamma\gamma}$ depends on the magnetospheric conversion model and on the dark matter density at the Galactic Center. For a standard dark matter profile, we exclude axion models with $g_{a\gamma\gamma}> $ 6-34 $\times 10^{-12}$ GeV$^{-1}$ with 95% confidence over the mass ranges 4.2-8.4, 8.9-10.0, 12.3-16.4, 18.6-26.9, 33.0-62.1, 70.1-74.3, 78.1-80.7, 105.5-109.6, 111.6-115.2, 126.0-159.3, and 162.5-165.6 $\mu$eV. For the maximal dark matter cusp allowed by stellar orbits near Sgr A*, these limits reduce to $g_{a\gamma\gamma} > $ 6-34 $ \times10^{-14}$ GeV$^{-1}$, which exclude some theoretical models for masses $> 33$ $\mu$eV. Limits may be improved by modeling stimulated axion conversion, by ray-tracing conversion pathways in the magnetar magnetosphere, and by obtaining deeper broad-band observations of the magnetar.