Detecting ultralight axion dark matter wind with laser interferometers

Abstract

The ultralight axion with mass around $10^{-22}$ eV is known as a candidate of dark matter. A peculiar feature of the ultralight axion is oscillating pressure in time, which produces oscillation of gravitational potentials. Since the solar system moves through the dark matter halo at the velocity of about $v \sim 300 \, \text{km} / \text{s} = 10^{-3}$, there exists axion wind, which looks like scalar gravitational waves for us. Hence, there is a chance to detect ultralight axion dark matter with a wide mass range by using laser interferometer detectors. We calculate the detector signal induced by the oscillating pressure of the ultralight axion field, which would be detected by future laser interferometer experiments. We also argue that the detector signal can be enhanced due to the resonance in modified gravity theory explaining the dark energy.Comment: 4 pages, 1 figure, published versio

Stimulated emission of dark matter axion from condensed matter excitations

“…15 Recently, new detection methods of ultralight axion-like particles corresponding to BEC dark matters are proposed. See [28,47,48] for example.…”

Dark matter signals on a laser interferometer

“…The last two factors in Eq. (20) means the ratio between the surface area of two bottom faces and the total surface area of the mirror. Our possible upper limit on the cross section as a function of the WIMP mass along with those by other experiments are shown in Fig.…”

“…We propose a search method for WIMP signals using laser interferometric gravitational wave detectors. Possible dark matter signals on laser interferometers have been investigated in several works [19][20][21]. However, calculations of the signals caused by direct interaction between a WIMP and nucleons in the mirror of interferometers have not been considered in the literature yet.…”

Detectability of ultralight scalar field dark matter with gravitational-wave detectors

“…Since the frequency of the motion is f φ m φ /2π and the frequency dispersion is tiny, ∆f φ ∼ f φ v 2 DM , detectors' signals are nearly monochromatic. It is worth mentioning that using the GW detectors to probe the ultralight scalar field dark matter was also investigated in [29]. In this reference, not the effects caused by the scalar force but the effects of metric perturbations sourced by the scalar field were considered, and it was found arXiv:1811.05003v1 [hep-ph] 9 Nov 2018 that such effects are far from the detectable level even with the future experiments.…”