Axion Search Experiment in Kyoto

Tada, M.; Kishimoto, Y.; Shibata, Masayuki; Kominato, K.; Ooishi, C.; Yamada, Shigeru; Funahashi, H.; Yamamoto, K.; Masaike, A.; Matsuki, S.

doi:10.1142/9789812776754_0013

Cited by 3 publications

(6 citation statements)

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“…(2. 19) with (2.20) we find that up to some geometrical factors QV cavity is replaced by A dish /m γ ∼ A dish λ. Having lost the ∼ Q ∼ 10 6 enhancement due to the resonance we can attempt to compensate for this by using a large area of the dish antenna.…”

Section: Dish Antenna Search For Hidden Photonsmentioning

confidence: 69%

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Searching for WISPy cold dark matter with a dish antenna

Horns

Jaeckel

Lindner

et al. 2013

J. Cosmol. Astropart. Phys.

235

257

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The cold dark matter of the Universe may be comprised of very light and very weakly interacting particles, so-called WISPs. Two prominent examples are hidden photons and axion-like particles. In this note we propose a new technique to sensitively search for this type of dark matter with dish antennas. The technique is broadband and allows to explore a whole range of masses in a single measurement. arXiv:1212.2970v1 [hep-ph] 12 Dec 2012 1 Other proposals use optical cavities [20]. Finally, an alternative technique relying on the QCD axion coupling to neutrons has recently been proposed in [21].2 In some models the mass of an axion required to be most of the dark matter can be determined up to uncertainties in the instantonic QCD potential. However, if the dominant fraction of axion dark matter arises after inflation from the misalignment mechanism, the dark matter density is proportional to the (square of) the misalignment angle which is determined by chance and can easily vary by an order of magnitude without fine-tuning. This leads to uncertainties of a similar size in the axion mass.

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Section: Dish Antenna Search For Hidden Photonsmentioning

confidence: 69%

“…Haloscopes [10] such as ADMX [17,18] (or CARRACK II [19]) on the other hand are direct dark matter searches exploiting microwave cavities 1 . They achieve enormous sensitivity by enhancing the conversion of WISPy dark matter into photons in a resonant cavity.…”

Section: Introductionmentioning

confidence: 99%

Searching for WISPy cold dark matter with a dish antenna

Horns

Jaeckel

Lindner

et al. 2013

J. Cosmol. Astropart. Phys.

235

257

View full text Add to dashboard Cite

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“…(Color in online edition) Schematic diagram of the prototype experimental system to search for cosmic axions with Rydberg atoms in cooled resonant cavities: (1) conversion cavity; (2) detection cavity; (3) cancellation coil; (4) main superconducting magnet coil; (5) thermal atomic beam oven; (6) ion source and neutralization system; (7) neutralizer with resonant charge-exchange reaction; (8) bending and focusing electrodes; (9) accelerating electrodes; (10) ion source of surface ionization type; (11) tuning rod; (12) dilution refrigerator system; (13) laser beam; (14) field-ionization system; (15) ionization electrodes. From Tada et al, 2001. ͉e͘ are individually detected.…”

Section: B the Carrack1 Detectormentioning

confidence: 99%

“…In addition, the rod for the conversion cavity is moved via Kevlar strings. The Kevlar string has very low heat conductivity, enough tensile strength to drive a rod of weight ϳ100 g, and low extensibility (Tada et al, 2001).…”

Section: Frequency Tuningmentioning

confidence: 99%

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Microwave cavity searches for dark-matter axions

et al. 2003

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Recent determinations of cosmological parameters point to a flat Universe, whose total energy density is composed of about two-thirds vacuum energy and one-third matter. Ordinary baryonic matter is relegated to a small fraction of the latter, within which the luminous part is an order of magnitude smaller yet. Particle dark matter, i.e., one or more relic particle species from the big bang, is thus strongly suggested as the dominant component of matter in the Universe. The axion, a hypothetical elementary pseudoscalar arising from the Peccei-Quinn solution to the strong-CP problem, is a well-motivated candidate. If the axion exists, it must be extremely light, in the mass range of 10 Ϫ6-10 Ϫ3 eV, and possess extraordinarily feeble couplings to matter and radiation. Nevertheless, as proposed by Sikivie in 1983, the axion's two-photon coupling lends itself to a feasible search strategy with currently available technology. In this scheme, axions resonantly convert to single microwave photons by a Primakoff interaction, in a tunable microwave cavity permeated by a strong magnetic field. Present experiments utilizing heterostructure transistor microwave amplifiers have achieved total system noise temperatures of ϳ3 K and represent the world's quietest spectral radio receivers. Exclusion regions have already been published well into the band of realistic axion model couplings, within the lowest decade of mass range. Recent breakthroughs in the development of near-quantum-limited superconducting quantum interference device amplifiers should reduce the system noise temperature to ϳ100 mK or less. Ongoing research into using Rydberg-atom single-quantum detectors as the detector in a microwave cavity experiment could further reduce the effective noise temperature. In parallel with improvements in amplifier technology, promising concepts for higher-frequency cavity resonators are being explored to open up the higher decades in mass range. Definitive experiments to find or exclude the axion may therefore be at hand in the next few years. As the microwave cavity technique measures the total energy of the axion, a positive discovery could well reveal fine structure of the signal due to flows of nonthermalized axions. Manifesting diurnal and sidereal modulation, such detailed features would contain a wealth of information about the history, structure, and dynamics of our Milky Way galaxy. CONTENTS I. Overview 778 II. Review of Axion Theory 779 A. Particle physics and the axion 779 B. Constraints from laboratory searches and astrophysics 780 C. Axions and cosmology 781 D. Phase-space structure of halo dark-matter axions 783 III. The Sikivie Microwave Cavity Experiment 783 A. Principles and techniques 783 B. First-generation experiments 784 1. The Rochester-Brookhaven-Fermilab experiment 784 2. The University of Florida experiment 785 C. Second-generation experiments IV. The U.S. Large-Scale Search A. Hardware 1. Cavity and tuning rods 2. The cavity mode structure and form factor B. Balanced heterostructure field-effect transisto...

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Searching for dark matter axions with Berry phase

Lambiase

Papini

2022

Eur. Phys. J. C

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We discuss novel aspects of the interaction of axions-like particles (ALP) with superfluids, superconductors in particular, and determine an induced Berry phase that is topologically singular and contributes to the generation of string-like structures. The latter are similar to vortices in superfluids. We suggest that measuring the currents generated by the Berry phase of ALP axions would enable the study of low mass regions of the ALP spectrum otherwise unobservable.

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Axion Search Experiment in Kyoto

Cited by 3 publications

References 0 publications

Searching for WISPy cold dark matter with a dish antenna

Searching for WISPy cold dark matter with a dish antenna

Microwave cavity searches for dark-matter axions

Searching for dark matter axions with Berry phase

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