Axion searches with microwave filters: the RADES project

Melcón, Alejandro Álvarez; Cuendis, S. Arguedas; Cogollos, C.; Díaz‐Morcillo, Alejandro; Döbrich, Babette; Gallego, Juan Daniel; Gimeno, B.; Irastorza, I.G.; Guerrero, Antonio José Lozano; Malbrunot, C.; Navarro, P.; Peña-Garay, Carlos; Redondo, Javier; Vafeiadis, T.; Wuensch, Walter

doi:10.1088/1475-7516/2018/05/040

Cited by 109 publications

(157 citation statements)

References 36 publications

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“…Along with the list of instruments presented in Introduction we also want to mention another possible design, advocated in [78], which is based on quantum coherence of the propagating axions, and which may also benefit from the large coherence length (61) mentioned above. Finally, we want to mention the idea advocated in [79][80][81] that the combination of large number of cavities can drastically enhance the axion signal. The design advocated in [79][80][81] may benefit from large wave length (61) of the gravitationally bound axions.…”

Section: Discussionmentioning

confidence: 99%

Gravitationally trapped axions on the Earth

et al. 2019

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We advocate for the idea that there is a fundamentally new mechanism for axion production on Earth, as recently suggested in [1,2]. We specifically focus on production of axions within Earth, with low velocities such that they will be trapped in the gravitational field. Our computations are based on the so-called Axion Quark Nugget (AQN) dark matter model, which was originally invented to explain the similarity of the dark and visible cosmological matter densities. This occurs in the model irrespective of the axion mass ma or initial misalignment angle θ0. Annihilation of antimatter AQNs with visible matter inevitably produce axions when AQNs hit Earth. The emission rate of axions with velocities below escape velocity is very tiny compared to the overall emission, however these axions will be accumulated over the 4.5 billion year life time of the Earth, which greatly enhances the discovery potential. We perform numerical simulations with a realistically modeled incoming AQN velocity and mass distribution, and explore how AQNs interact as they travel through the interior of the Earth. We use this to estimate the axion flux on the surface of the Earth, the velocity-spectral features of trapped axions, the typical annihilation pattern of AQN, and the density profile of the axion halo around the Earth. Knowledge of these properties is necessary to make predictions for the observability of trapped axions using CAST, ADMX, MADMAX, CULTASK, ORPHEUS, ARIADNE, CASPEr, ABRACADABRA, QUAX, ORGAN, TOORAD, DM Radio.2 In particular, a first-order phase transition is not required as the axion domain wall plays the role of the squeezer. Another problem with [34,35] is that nuggets will likely evaporate on a Hubble time-scale even. For the AQN model this argument is not applicable because the vacuum-ground-state energies inside (color-superconducting phase) and outside (hadronic phase) the nugget are drastically different. Therefore, these two systems can arXiv:1905.00022v2 [astro-ph.CO]

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Section: Discussionmentioning

confidence: 99%

Gravitationally trapped axions on the Earth

et al. 2019

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“…The central problem in detecting the axion however is that we do not know the frequency, ω m a (1 + v 2 /2) at which the electromagnetic response to the axion field should be monitored. To search for this frequency, haloscopes either enforce a resonance or constructive interference condition for a signal oscillating at ∼ m a (as in e.g., ADMX [116,117], MADMAX [118,119], HAYSTAC [120][121][122][123], CULTASK [124][125][126], OR-GAN [127,128], KLASH [129] and RADES [130]), or are sensitive to a wide bandwidth of frequencies simultaneously (e.g., ABRACADABRA [131][132][133], BEAST [134] and DM-Radio [135]). See Ref.…”

Section: Axion Searchesmentioning

confidence: 99%

Velocity substructure from Gaia and direct searches for dark matter

et al. 2020

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Data from the Gaia satellite show that the solar neighbourhood of the Milky Way's stellar halo is imprinted with substructure from several accretion events. Evidence of these events is found in "the Shards", stars clustering with high significance in both action space and metallicity. Stars in the Shards share a common origin, likely as ancient satellite galaxies of the Milky Way, so will be embedded in dark matter (DM) counterparts. These "Dark Shards" contain two substantial streams (S1 and S2), as well as several retrograde, prograde and lower energy objects. The retrograde stream S1 has a very high Earth-frame speed of ∼ 550 km s −1 while S2 moves on a prograde, but highly polar orbit and enhances peak of the speed distribution at around 300 km s −1 . The presence of the Dark Shards locally leads to modifications of many to the fundamental properties of experimental DM signals. The S2 stream in particular gives rise to an array of effects in searches for axions and in the time dependence of nuclear recoils: shifting the peak day, inducing non-sinusoidal distortions, and increasing the importance of the gravitational focusing of DM by the Sun. Dark Shards additionally bring new features for directional signals, while also enhancing the DM flux towards Cygnus.

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“…However, the technique is still under development. Similarly, the high mass performance of cavity haloscopes relies on unproven techniques such as combining large numbers of cavities [16,22,23].…”

Section: Introductionmentioning

confidence: 99%

Tunable Axion Plasma Haloscopes

et al. 2019

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We propose a new strategy to search for dark matter axions using tunable cryogenic plasmas. Unlike current experiments, which repair the mismatch between axion and photon masses by breaking translational invariance (cavity and dielectric haloscopes), a plasma haloscope enables resonant conversion by matching the axion mass to a plasma frequency. A key advantage is that the plasma frequency is unrelated to the physical size of the device, allowing large conversion volumes. We identify wire metamaterials as a promising candidate plasma, wherein the plasma frequency can be tuned by varying the interwire spacing. For realistic experimental sizes we estimate competitive sensitivity for axion masses 35 − 400 µeV, at least.

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Axion searches with microwave filters: the RADES project

Cited by 109 publications

References 36 publications

Gravitationally trapped axions on the Earth

Gravitationally trapped axions on the Earth

Velocity substructure from Gaia and direct searches for dark matter

Tunable Axion Plasma Haloscopes

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