Tunable Supermode Dielectric Resonators for Axion Dark-Matter Haloscopes

McAllister, Ben T.; Flower, Graeme; Tobar, Lucas E.; Tobar, Michael E.

doi:10.1103/physrevapplied.9.014028

Cited by 47 publications

(34 citation statements)

References 46 publications

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“…[91]. On the other hand, axion haloscope collaborations (ADMX [92][93][94], HAYSTAC [95][96][97], OR-GAN [98,99]) appear to have independently decided on the value ρ 0 = 0.45 GeV cm −3 .…”

Section: Local Dark Matter Densitymentioning

confidence: 99%

“…To identify the frequency of the axion mass, m a , the experiment may either enforce some resonance or constructive interference condition for a signal oscillating at ω = m a (as in e.g. ADMX [93,94], MADMAX [177][178][179], HAYSTAC [95-97, 180, 181], CULTASK [182][183][184], Orpheus [185], ORGAN [98,99], KLASH [186] and RADES [187]), or be sensitive to a wide bandwidth of frequencies simultaneously (e.g. ABRACADABRA [21,188,189], BEAST [190] and DM-Radio [191]).…”

Section: Axion Haloscopesmentioning

confidence: 99%

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Refinement of the standard halo model for dark matter searches in light of the Gaia Sausage

Evans

O’Hare

McCabe³

2019

Phys. Rev. D

179

165

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Predicting signals in experiments to directly detect dark matter (DM) requires a form for the local DM velocity distribution. Hitherto, the standard halo model (SHM), in which velocities are isotropic and follow a truncated Gaussian law, has performed this job. New data, however, suggest that a substantial fraction of our stellar halo lies in a strongly radially anisotropic population, the 'Gaia Sausage'. Inspired by this recent discovery, we introduce an updated DM halo model, the SHM ++ , which includes a 'Sausage' component, thus better describing the known features of our galaxy. The SHM ++ is a simple analytic model with five parameters: the circular speed, local escape speed and local DM density, which we update to be consistent with the latest data, and two new parameters: the anisotropy and the density of DM in the Sausage. The impact of the SHM ++ on signal models for WIMPs and axions is rather modest since the multiple changes and updates have competing effects. In particular, this means that the older exclusion limits derived for WIMPS are still reasonably accurate. However, changes do occur for directional detectors, which have sensitivity to the full three-dimensional velocity distribution.

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Section: Local Dark Matter Densitymentioning

confidence: 99%

Section: Axion Haloscopesmentioning

confidence: 99%

Refinement of the standard halo model for dark matter searches in light of the Gaia Sausage

Evans

O’Hare

McCabe³

2019

Phys. Rev. D

179

165

View full text Add to dashboard Cite

show abstract

“…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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“…Recently, there was a study that showed a potential application of Bragg reflectors with a dielectric hollow using the TM 030 mode of cylindrical cavities [15]. The study presented a frequency tuning scheme which breaks the field symmetry along the cavity axis by splitting a dielectric cylindrical hollow in the longitudinal direction.…”

Section: Along the Longitudinal Directionmentioning

confidence: 99%

“…We modeled a cylindrical cavity with the same dimension as in Ref. [15] to reproduce the results for the longitudinal mechanism to check consistency. For each scheme, we introduced a tuning system with optimal dimensions and repeated the evaluation.…”

Section: Performance Comparisonmentioning

confidence: 99%

Exploiting higher-order resonant modes for axion haloscopes

Kim

Youn

Jeong

et al. 2020

J. Phys. G: Nucl. Part. Phys.

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The haloscope is one of the most sensitive approaches to the QCD axion physics within the region where the axion is considered to be a dark matter candidate. Current experimental sensitivities, which rely on the lowest fundamental TM 010 mode of a cylindrical cavity, are limited to relatively low mass regions. Exploiting higherorder resonant modes would be beneficial because it will enable us to extend the search range with no volume loss and higher quality factors. This approach has been discarded mainly because of the significant degradation of form factor, and difficulty with frequency tuning. Here we introduce a new tuning mechanism concept which both enhances the form factor and yields reasonable frequency tunability. A proof of concept demonstration proved that this design is feasible for high mass axion search experiments.

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Tunable Supermode Dielectric Resonators for Axion Dark-Matter Haloscopes

Cited by 47 publications

References 46 publications

Refinement of the standard halo model for dark matter searches in light of the Gaia Sausage

Refinement of the standard halo model for dark matter searches in light of the Gaia Sausage

Velocity substructure from Gaia and direct searches for dark matter

Exploiting higher-order resonant modes for axion haloscopes

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