Detecting dark photon dark matter with Gaia-like astrometry observations

Abstract

A class of dark photon dark matter models with ultralight masses would lead to oscillation of a test body through a coupling with baryons or B − L charge. This periodical oscillation of an observer results in swing of a star's apparent position due to the effect of aberration of light, which could be probed with high-precision astrometry observations of stars in the Milky Way. We propose to use the observations of stellar positions of a number of stars by Gaia to search for this kind of dark photon dark matter. We show that this astrometry method is able to give promising sensitivities to search for the dark photon dark matter in the mass range of 10 −23 ∼ 10 −21 eV.

High-precision search for dark photon dark matter with the Parkes Pulsar Timing Array

“…Furthermore, the dark matter background can cause displacements on terrestrial/celestial objects, leading to observable effects [25]. For example, depending on the mass of dark photon particles which determines the dark matter oscillation frequency, such motion can be probed using high-precision astrometry [26], spectroscopic [27], timing observations [28,29], as well as gravitational-wave detectors [30][31][32].…”

“…where m is the mass of the test body, an characterizes the coupling strength of the new gauge interaction that is normalized to the electromagnetic coupling constant e. The dark charge q equals the baryon number for the U(1) B interaction or baryon-minus-lepton number for the U(1) B−L interaction. Such an acceleration allows the detection of the DPDM in several ways, e.g., using high-precision astrometry [26] or gravitational-wave detectors [30].…”

Mass formulae and staticity condition for dark matter charged black holes

“…By virtue of the direct calculation it can be envisaged that for all asymptotically flat perturbations, as well as, for N μ ,Ã 0 ,B 0 fulfilling the auxiliary conditions r → ∞, one reaches the conclusion that variation δH is equal to the right-hand side of the relation given by the equation (15).…”

“…The studies of gamma rays emission in dwarf galaxies, oscillation of the fine structure constant, exploration of the possible low-energy mass dark sector [11][12][13], studies of dark photon production in the former observations of supera e-mails: marek.rogatko@poczta.umcs.lublin.pl; rogat@kft.umcs. lublin.pl (corresponding author) nova 1987A event [14], Gaia-like astrometry observations [15], as well as, studies of dynamics of galaxy clusters collisions [16], are expected to deliver new way of elaborating the old problem. Recently SENSEI device [17] is dedicated for the direct-detection of dark matter in eV to GeV energy range.…”

Dissecting axion and dark photon with a network of vector sensors

“…On the other hand, there are types of experiments sensitive to vector-like signals, including effective magnetic fields leading to the spin precession [33,34,35,36,37,38,39,40,41,42] that can capture axion-fermion coupling or dipole couplings with the dark photon [43], effective electric currents from kinetic mixing dark photon in a shielded room [19], and forces brought from U (1) B−L /U (1) B dark photon [44,45,46,47]. Taking the axion-fermion coupling as an example, in the non-relativistic limit of the fermion, one has the vector-like coupling between the spatial derivative of the axion and the spin operator of the fermion g a ∂ µ a ψγ µ γ 5 ψ → g a ∇a • σ,…”