Experimental Constraints on the Axion Dark Matter Halo Density

Asztalos, S. J.; Daw, E. J.; Peng, H.; Rosenberg, L.; Yu, Dongrui; Hagmann, C.; Kinion, D.; Stoeffl, W.; Bibber, K. van; LaVeigne, J.; Sikivie, P.; Sullivan, N. S.; Tanner, D. B.; Nezrick, F. A.; Moltz, D. M.

doi:10.1086/341130

Cited by 97 publications

(87 citation statements)

References 44 publications

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“…On top of a T p,cavity of 0.1 K, quantum-noise-limited superconducting amplifiers were employed as the 1st amplifiers whose noise temperatures are proportional to not only the frequencies (T n,amp ∼ hν/k B ln 2) [28] but also the ambient temperatures (T p,cavity in axion haloscopes) to achieve fast DFSZ scanning rates from the small AC-TION experiment. Figure 5 shows the exclusion limits expected from the large and small ACTION experiments, and therein the exclusion limits from RBF [12], UF [13], ADMX [14,15], HAYSTAC [16], and CAST [22] are also shown.…”

Section: Figmentioning

confidence: 99%

“…The simplified ACTION experiment excludes the axion-photon coupling g aγγ down to [12], UF [13], ADMX [14,15], HAYSTAC [16], and CAST [22] are also shown.…”

Section: Figmentioning

confidence: 99%

“…Assuming the axions have an isothermal distribution, the signal power given in Eq. (1) would then distribute over a Maxwellian shape with an axion rms speed of about 270 km/s in our galaxy [11], which is the basic model considered in this paper.Most of the axion haloscope searches to date [12][13][14][15][16] have employed a cylindrical resonator without an open resonator [17]. In this paper, we report the first axion haloscope search with toroidal geometry.…”

mentioning

confidence: 99%

“…Most of the axion haloscope searches to date [12][13][14][15][16] have employed a cylindrical resonator without an open resonator [17]. In this paper, we report the first axion haloscope search with toroidal geometry.…”

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confidence: 99%

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First axion dark matter search with toroidal geometry

et al. 2017

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We firstly report an axion haloscope search with toroidal geometry. In this pioneering search, we exclude the axion-photon coupling gaγγ down to about 5 × 10 −8 GeV −1 over the axion mass range from 24.7 to 29.1 µeV at a 95% confidence level. The prospects for axion dark matter searches with larger scale toroidal geometry are also considered. PACS numbers: 95.35.+d, 14.80.Va According to precision cosmological measurements [1], more than 80% of the matter content in the Universe is now believed to be cold dark matter (CDM). However, the CDM composition is beyond the standard model of particle physics, and thus is still unknown to date. One of the most compelling candidates for CDM is the axion [2], provided its mass is above 1 µeV [3] and below 3 meV [4]. The axion is the result of the breakdown of a new symmetry proposed by Peccei and Quinn [5] to solve the strong CP (Charge-conjugation and P arity) problem in Quantum Chromodynamics [6]. As a result of the axion production mechanism, the axion mass range is very large with the above range being optimum for CDM.The axion search method proposed by Sikivie [7], also known as the axion haloscope search, involves a microwave resonant cavity with a static magnetic field that induces axion conversions into microwave photons. The conversion power corresponding to the axion signal should be enhanced when the axion mass m a matches the resonant frequency of the cavity mode ν, m a = hν/c 2 . The power would be detected as the axion signal iswhere g aγγ is the axion-photon coupling strength, whose two popular benchmark models are KSVZ [8] for hadronic axions and DFSZ [9], which also includes axion coupling to leptons, ρ a ≈ 0.45 GeV/cm 3 is the local dark matter density, ω = 2πν, andB 2 dV is energy stored in a magnetic field in the cavity volume V , where B is a static magnetic field provided by magnets in the axion haloscopes. The cavitymode-dependent form factor C whose general definition can be found in Ref.[10] and quality factor Q are also shown in Eq. (1) and Q/(1+β) corresponds to the loaded quality factor Q L , where β denotes the mode coupling to the load. Assuming the axions have an isothermal distribution, the signal power given in Eq. (1) would then distribute over a Maxwellian shape with an axion rms speed of about 270 km/s in our galaxy [11], which is the basic model considered in this paper.Most of the axion haloscope searches to date [12][13][14][15][16] have employed a cylindrical resonator without an open resonator [17]. In this paper, we report the first axion haloscope search with toroidal geometry. As reported in our previous publication [10], as long as ∇ × B ∼ 0 is valid, Eq.(1) and the definition of the cavity-modedependent form factor C therein are valid as they are in axion haloscopes in spite of the lack of an axion to a photon magnetic field coupling in the form factor C, which is also true for toroidal geometry. We refer to this axion dark matter search as ACTION for "Axion haloscopes at CAPP with ToroIdal resONators". The prospects for la...

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Section: Figmentioning

confidence: 99%

“…The simplified ACTION experiment excludes the axion-photon coupling g aγγ down to [12], UF [13], ADMX [14,15], HAYSTAC [16], and CAST [22] are also shown.…”

Section: Figmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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First axion dark matter search with toroidal geometry

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“…Almost every technique that has been discussed for the detection of dark matter requires that the dark matter is composed of heavy neutral particles with weak-interaction cross sections. (The axion search experiment [24] gives the only counterexample. )…”

Section: Why the Wimp Model Of Dark Matter Deserves Special Attentionmentioning

confidence: 99%

Determination of Dark Matter Properties at High-Energy Collider

Baltz¹,

Battaglia²,

Peskin³

et al. 2006

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If the cosmic dark matter consists of weakly-interacting massive particles, these particles should be produced in reactions at the next generation of high-energy accelerators. Measurements at these accelerators can then be used to determine the microscopic properties of the dark matter. From this, we can predict the cosmic density, the annihilation cross sections, and the cross sections relevant to direct detection. In this paper, we present studies in supersymmetry models with neutralino dark matter that give quantitative estimates of the accuracy that can be expected. We show that these are well matched to the requirements of anticipated astrophysical observations of dark matter. The capabilities of the proposed International Linear Collider (ILC) are expected to play a particularly important role in this study.

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Stars and Fundamental Physics

Raffelt¹

Eso Astrophysics Symposia

101

176

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Abstract. Stars are powerful sources for weakly interacting particles that are produced by nuclear or plasma processes in their hot interior. These fluxes can be used for direct measurements (e.g. solar or supernova neutrinos) or the back-reaction on the star can be used to derive limits on new particles. We discuss two examples of current interest, the search for solar axions by the CAST experiment at CERN and stellar-evolution limits on the size of putative large extra dimensions.

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Experimental Constraints on the Axion Dark Matter Halo Density

Cited by 97 publications

References 44 publications

First axion dark matter search with toroidal geometry

First axion dark matter search with toroidal geometry

Determination of Dark Matter Properties at High-Energy Collider

Stars and Fundamental Physics

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