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Axion search with a quantum-limited ferromagnetic haloscope

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arxiv 2001.08940 v1 pith:INSCML2M submitted 2020-01-24 hep-ex quant-ph

classification hep-exquant-ph
keywords axionfieldhaloscopeconstantcorrespondingcoupledcouplingferromagnetic
verification ladder T0 review T1 audit T2 compute T3 formal
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abstract

A ferromagnetic axion haloscope searches for Dark Matter in the form of axions by exploiting their interaction with electronic spins. It is composed of an axion-to-electromagnetic field transducer coupled to a sensitive rf detector. The former is a photon-magnon hybrid system, and the latter is based on a quantum-limited Josephson parametric amplifier. The hybrid system consists of ten 2.1 mm diameter YIG spheres coupled to a single microwave cavity mode by means of a static magnetic field. Our setup is the most sensitive rf spin-magnetometer ever realized. The minimum detectable field is $5.5\times10^{-19}\,$T with 9 h integration time, corresponding to a limit on the axion-electron coupling constant $g_{aee}\le1.7\times10^{-11}$ at 95% CL. The scientific run of our haloscope resulted in the best limit on DM-axions to electron coupling constant in a frequency span of about 120 MHz, corresponding to the axion mass range $42.4$-$43.1\,\mu$eV. This is also the first apparatus to perform an axion mass scanning by changing the static magnetic field.

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Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Probing the axion-electron coupling at cavity experiments

    hep-ph 2025-07 conditional novelty 6.0 of 10

    Cavity walls radiate microwave photons when axion dark matter generates a chiral magnetic current at the conductor surface, turning existing haloscope data into a bound on the axion-electron coupling g_ae ≲ 10^-5.

  2. Searching for Axion Dark Matter Near Relaxing Magnetars

    hep-ph 2025-05 conditional novelty 6.0 of 10

    Resonant axion-to-photon conversion near magnetars could be observable with ALMA and SKA, but the predicted line strength and frequency depend heavily on which plasma model is correct.

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