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Vector Coherent Oscillation Dark Matter
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We construct a model of hidden massive vector boson dark matter as a homogeneous coherent oscillation in the entire universe without any dangerous instability. We make use of a particular form of the vector boson coupling to a scalar field through the gauge kinetic function. This scenario may be distinguished from other dark matter models through the observation of statistical anisotropy in the dark matter isocurvature perturbation.
Forward citations
Cited by 6 Pith papers
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Generating Moving Field Initial Conditions with Spatially Varying Boost
A 'spatially varying boost' algorithm assigns arbitrary, position-dependent bulk velocities to field initial data by composing local Lorentz boosts, demonstrated on solitons, Proca fields, and spin-1 wave dark matter.
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Spin-1 Ultralight Dark Matter under Cosmological Scrutiny: Mass Constraints from CMB and Distance Probes
Cosmological data place a lower bound near 10⁻²⁴ eV on spin-1 ultralight dark matter and predict a CMB anisotropy signature that may be detectable when the vector field is a minor dark-matter component.
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Dark Photon Dark Matter from Quantum Fluctuations during Starobinsky Inflation
Dark photons produced by quantum fluctuations during Starobinsky inflation must have a mass of 5.6–7.4 µeV to be all the dark matter.
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Light Dark Matter Detection with Sub-eV Transition-Edge Sensors
Optical transition-edge sensors with sub-eV thresholds are projected to probe unexplored light dark matter parameter space with nanogram-month exposures.
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Black-hole hair from vector dark matter accretion
A Schwarzschild black hole accreting from a bath of vector dark matter develops a nontrivial Proca field profile, with density amplified by up to 10^7 near the horizon and mass accretion rates reaching tens of solar m...
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Misalignment production of isotropized vector dark matter?
Kinetic-coupling misalignment of an isotropized multi-vector condensate cannot produce dark matter: non-Gaussianity and isocurvature constraints exclude the viable parameter space in both weak- and strong-mixing regimes.
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