Design and operational experience of a microwave cavity axion detector for the <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" altimg="si0006.gif" overflow="scroll"><mml:mrow><mml:mn>20</mml:mn><mml:mo>–</mml:mo><mml:mn>100</mml:mn><mml:mspace width="0.25em"/><mml:mi mathvariant="normal">μ</mml:mi><mml:mi>eV</mml:mi></mml:mrow></mml:math> range

Kenany, S. Al; Anıl, Mehmet Ali; Backes, Kelly; Brubaker, Benjamin; Cahn, S. B.; Carosi, G.; Gurevich, Yulia V.; Kindel, William; Lamoreaux, S. K.; Lehnert, K. W.; Lewis, Samantha M.; Malnou, M.; Palken, Daniel; Rapidis, N. M.; Root, Jaben; Simanovskaia, Maria; Shokair, T. M.; Urdinaran, I.; Bibber, Karl A. van; Zhong, L.

doi:10.1016/j.nima.2017.02.012

Cited by 89 publications

(76 citation statements)

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“…Without squeezing (G s = 1), R is maximized when the cavity is twice-overcoupled (κ m = 2κ l ), and at this optimal coupling the scan rate scales as R max u ∝ κ 2 a /κ l , a known result [28]. When G s 1, the optimal coupling is κ m = 2G s κ l and the scan rate scales as R max s ∝ G s κ 2 a /κ l .…”

Section: Amp Sqmentioning

confidence: 98%

Squeezed Vacuum Used to Accelerate the Search for a Weak Classical Signal

et al. 2019

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Many experiments that interrogate fundamental theories require detectors whose sensitivities are limited by the laws of quantum mechanics. In cavity-based searches for axionic dark matter, vacuum fluctuations in the two quadratures of the cavity electromagnetic field limit the sensitivity to an axion-induced field. In an apparatus designed to partially mimic existing axion detectors, we demonstrate experimentally that such quantum limits can be overcome through the use of squeezed states. By preparing a microwave cavity in a squeezed state and measuring just the squeezed quadrature, we enhance the spectral scan rate by a factor of 2.12 ± 0.08. This enhancement is in excellent quantitative agreement with a theoretical model accounting for both imperfect squeezing and measurement. arXiv:1809.06470v2 [quant-ph]

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Section: Amp Sqmentioning

confidence: 98%

Squeezed Vacuum Used to Accelerate the Search for a Weak Classical Signal

et al. 2019

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“…Post-inflationary scenarios restrict this range to (10 − 10 3 ) µeV [4], where a rich experimental program will probe the axion existence in the next decade. Among the experiments, ADMX [5], HAYSTAC [6], ORGAN [7], CULTASK [8] and KLASH [9] will use a haloscope, i.e. a detector composed of a resonant cavity immersed in a strong magnetic field as proposed by P. Sikivie [10].…”

Section: Introductionmentioning

confidence: 99%

“…a detector composed of a resonant cavity immersed in a strong magnetic field as proposed by P. Sikivie [10]. When the resonant frequency of the cavity ν c is tuned to the corresponding axion mass m a c 2 /h, the expected * Corresponding author divora@pd.infn.it † Corresponding author claudio.gatti@lnf.infn.it ‡ Corresponding author alessio.rettaroli@lnf.infn.it power deposited by DM axions is given by [6] P a = g 2 γ α 2 π 2…”

Section: Introductionmentioning

confidence: 99%

Galactic axions search with a superconducting resonant cavity

et al. 2019

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To account for the dark matter content in our Universe, post-inflationary scenarios predict for the QCD axion a mass in the range (10 − 10 3 ) µeV. Searches with haloscope experiments in this mass range require the monitoring of resonant cavity modes with frequency above 5 GHz, where several experimental limitations occur due to linear amplifiers, small volumes, and low quality factors of Cu resonant cavities. In this paper we deal with the last issue, presenting the result of a search for galactic axions using a haloscope based on a 36 cm 3 NbTi superconducting cavity. The cavity worked at T = 4 K in a 2 T magnetic field and exhibited a quality factor Q0 = 4.5 × 10 5 for the TM010 mode at 9 GHz. With such values of Q the axion signal is significantly increased with respect to copper cavity haloscopes. Operating this setup we set the limit gaγγ < 1.03 × 10 −12 GeV −1 on the axion photon coupling for a mass of about 37 µeV. A comprehensive study of the NbTi cavity at different magnetic fields, temperatures, and frequencies is also presented.

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“…A precise knowledge of the m a that gives the observed DM density is of critical importance for axion direct detection experiments [31][32][33][34][35][36][37][38][39][40][41].…”

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confidence: 99%

Early-Universe Simulations of the Cosmological Axion

2020

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Ultracompact dark matter (DM) minihalos at masses at and below 10 −12 M arise in axion DM models where the Peccei-Quinn (PQ) symmetry is broken after inflation. The minihalos arise from density perturbations that are generated from the non-trivial axion self interactions during and shortly after the collapse of the axion-string and domain-wall network. We perform highresolution simulations of this scenario starting at the epoch before the PQ phase transition and ending at matter-radiation equality. We characterize the spectrum of primordial perturbations that are generated and comment on implications for efforts to detect axion DM. We also measure the DM density at different simulated masses and argue that the correct DM density is obtained for ma = 25.2 ± 11.0 µeV.

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Design and operational experience of a microwave cavity axion detector for the 20–100μeV range

Cited by 89 publications

References 20 publications

Squeezed Vacuum Used to Accelerate the Search for a Weak Classical Signal

Squeezed Vacuum Used to Accelerate the Search for a Weak Classical Signal

Galactic axions search with a superconducting resonant cavity

Early-Universe Simulations of the Cosmological Axion

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