Abstract
We report the results from a haloscope search for axion dark matter in the 3.3-4.2 μeV mass range. This search excludes the axion-photon coupling predicted by one of the benchmark models of "invisible" axion dark matter, the Kim-Shifman-Vainshtein-Zakharov model. This sensitivity is achieved using a large-volume cavity, a superconducting magnet, an ultra low noise Josephson parametric amplifier, and sub-Kelvin temperatures. The validity of our detection procedure is ensured by injecting and detecting blind synthetic axion signals.
Highlights
We report the results from a haloscope search for axion dark matter in the 3.3–4.2 μeV mass range
In the scenario in which the Peccei and Quinn (PQ) symmetry breaks before cosmological inflation, the relic axion abundance is determined only by the initial amplitude (θ0) and mass of the axion field
In the postinflationary scenario, where the PQ symmetry breaks after cosmological inflation, most calculations suggest that the axion mass lies in the Oð1–100Þ μeV range [10,11,12,13,14,15,16,17,18,19,20,21,22]
Summary
We report the results from a haloscope search for axion dark matter in the 3.3–4.2 μeV mass range. This search excludes the axion-photon coupling predicted by one of the benchmark models of “invisible” axion dark matter, the Kim-Shifman-Vainshtein-Zakharov model. This discrepancy is called the strong-CP problem. The existence of a new global axial U(1) symmetry, proposed by Peccei and Quinn (PQ) [3], would solve the strong-CP problem The axion has a coupling to two photons, and the numerical values are represented by two benchmark models, the KimShifman-Vainshtein-Zakharov (KSVZ) [23,24] and DineFischler-Srednicki-Zhitnitsky (DFSZ) [25,26] models
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