Overview of the Cosmic Axion Spin Precession Experiment (CASPEr)

Kimball, Derek F. Jackson; Afach, S.; Aybas, Deniz; Blanchard, John W.; Budker, Dmitry; Centers, Gary P.; Engler, M.; Figueroa, Nataniel L.; Garcon, Antoine; Graham, Peter W.; Luo, Haibo; Rajendran, Surjeet; Sendra, M. G.; Sushkov, Alexander O.; Wang, Tao; Wickenbrock, Arne; Wilzewski, Alexander; Wu, Teng

doi:10.1007/978-3-030-43761-9_13

Cited by 56 publications

(51 citation statements)

References 68 publications

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“…We refer the reader to appendix A and to the original refs. [7,8,73,74] for more details on the detection technique and bound extraction from sensitivity estimate. In figure 5, we show a comparison between the reach of CASPEr, both for the axion halo and for the standard axion DM scenario.…”

Section: Alp Search Using Nuclear Magnetic Resonancementioning

confidence: 99%

“…For a solar halo, the ratio can be 1-2 orders of magnitude even if M 10 −12 M , whereas for the Earth halo it could exceed a factor of 10 5 . For the projected sensitivities in the presence of local DM, we refer readers to [8,73].…”

Section: For Further Details)mentioning

confidence: 99%

“…The sensitivity of CASPEr-Wind can be obtained by the same procedure. Since the noise sources are not explicitly discussed in [73], we instead compute the relative sensitivity in the halo scenario compared to local dark matter scenario for CASPEr-Wind. The modification in sensitivities is estimated as…”

Section: Jhep09(2020)004mentioning

confidence: 99%

“…In this regime standard NMR techniques are not ideal, and so the sensitivity estimates we have used may not be appropriate. However, the apparatus can be modified through the use of hyper-polarization techniques as well as modified encoding and detection methods not based on Faraday induction [73]. Such techniques are being employed in CASPEr-ZULF (Zero to Ultra-Low Field) [86,87] as an extension of CASPEr-Wind, and will allow the experiment to probe axion masses in the range 10 −22 eV m φ 10 −13 eV.…”

Section: Jhep09(2020)004mentioning

confidence: 99%

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Searching for Earth/Solar axion halos

Banerjee

Budker

Eby

et al. 2020

J. High Energ. Phys.

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We discuss the sensitivity of the present and near-future axion dark matter experiments to a halo of axions or axion-like particles gravitationally bound to the Earth or the Sun. Such halos, assuming they are formed, can be searched for in a wide variety of experiments even when the axion couplings to matter are small, while satisfying all the present experimental bounds on the local properties of dark matter. The structure and coherence properties of these halos also imply novel signals, which can depend on the latitude or orientation of the detector. We demonstrate this by analyzing the sensitivity of several distinct types of axion dark matter experiments.

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Section: Alp Search Using Nuclear Magnetic Resonancementioning

confidence: 99%

Section: For Further Details)mentioning

confidence: 99%

Section: Jhep09(2020)004mentioning

confidence: 99%

Section: Jhep09(2020)004mentioning

confidence: 99%

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Searching for Earth/Solar axion halos

Banerjee

Budker

Eby

et al. 2020

J. High Energ. Phys.

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“…For instance, via the measurement of the axion coupling to the neutron electric dipole moment (nEDM) operator at CASPER-electric[16,17], in case the axion would also account for dark matter (DM). The axion-to-nEDM coupling directly follows from the m a -f a relation and so it is unmodified in standard approaches to axion coupling enhancements (left panel in figure1) that still rely on eq.…”

mentioning

confidence: 99%

An even lighter QCD axion

Luzio

Gavela

Quílez

et al. 2021

J. High Energ. Phys.

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We explore whether the axion which solves the strong CP problem can naturally be much lighter than the canonical QCD axion. The $$ {Z}_{\mathcal{N}} $$ Z N symmetry proposed by Hook, with $$ \mathcal{N} $$ N mirror and degenerate worlds coexisting in Nature and linked by the axion field, is considered in terms of generic effective axion couplings. We show that the total potential is safely approximated by a single cosine in the large $$ \mathcal{N} $$ N limit, and we determine the analytical formula for the exponentially suppressed axion mass. The resulting universal enhancement of all axion interactions relative to those of the canonical QCD axion has a strong impact on the prospects of axion-like particle experiments such as ALPS II, IAXO and many others: experiments searching for generic axion-like particles have in fact discovery potential to solve the strong CP problem. The finite density axion potential is also analyzed and we show that the $$ {Z}_{\mathcal{N}} $$ Z N asymmetric background of high-density stellar environments sets already significant model-independent constraints: 3 ≤ $$ \mathcal{N} $$ N ≲ 47 for an axion scale fa ≲ 2.4 × 1015 GeV, with tantalizing discovery prospects for any value of fa and down to $$ \mathcal{N} $$ N ∼ 9 with future neutron star and gravitational wave data, down to the ultra-light mass region. In addition, two specific ultraviolet $$ {Z}_{\mathcal{N}} $$ Z N completions are developed: a composite axion one and a KSVZ-like model with improved Peccei-Quinn quality.

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Measuring the Quantum State of Dark Matter

Marsh

2023

Annalen der Physik

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It is shown how the time series obtained from searches for ultralight bosonic dark matter (DM), such as the axion, can be used to determine whether it is in a coherent or incoherent quantum state. The example is essentially trivial, but it is hoped that explicitly addressing it will provoke experimental exploration. In the standard coherent state, oscillations in the number density occur over the coherence time, , where m is the particle mass and v is the galactic virial velocity, leading to a reduction in the constraining power of experiments operating on timescales , due to the unknown global phase. On the other hand, if the DM is incoherent then no such strong number oscillations occur since the ensemble average over particles in different streams gives an effective phase average. If an experiment detects a signal then the coherent or incoherent nature of DM can be determined by time series analysis over the coherence time. This finding is observationally relevant for DM masses, (corresponding to coherence times between a year and 100 s).

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Overview of the Cosmic Axion Spin Precession Experiment (CASPEr)

Cited by 56 publications

References 68 publications

Searching for Earth/Solar axion halos

Searching for Earth/Solar axion halos

An even lighter QCD axion

Measuring the Quantum State of Dark Matter

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