HAYSTAC axion search analysis procedure

Brubaker, Benjamin; Zhong, L.; Lamoreaux, S. K.; Lehnert, K. W.; Bibber, Karl A. van

doi:10.1103/physrevd.96.123008

Cited by 127 publications

(120 citation statements)

References 38 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%

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

Evans

O’Hare

McCabe³

2019

Phys. Rev. D

178

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%

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

Evans

O’Hare

McCabe³

2019

Phys. Rev. D

178

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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“…where F i is the predicted signal flux within each synthesized beam. The significance of the detection is given by δχ 2 ; note that in the single-beam case, the significance is simply the SNR as given in (37).…”

Section: Simplified Likelihood For Radio Arraysmentioning

confidence: 99%

“…For example, the Axion Dark Matter eXperiment (ADMX), which is a resonant cavity experiment, has already constrained a narrow region of axion DM parameter space with axion masses around 10 −6 eV, and ongoing as well as future runs of ADMX may be able to cover nearly a decade of possible axion masses, from ∼10 −6 eV to ∼10 −5 eV [32][33][34]. At higher frequencies, planned experiments such as HAYSTAC [35][36][37] and MADMAX [38] may extend the reach in axion mass to ∼10 −4 eV, while at lower masses experiments including ABRACADABRA [39][40][41][42], DM-Radio [43,44], and CASPEr [45] may potentially reach all the way down to ∼10 −9 eV or below. The indirect radio searches proposed in this work may reach sensitivity to the QCD axion from masses in the range few × 10 −7 eV to few × 10 −5 eV, depending on the target, telescope, and systematics such as the DM density profiles and the distributions of NS properties.…”

Section: Introductionmentioning

confidence: 99%

Detecting axion dark matter with radio lines from neutron star populations

2019

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It has been suggested that radio telescopes may be sensitive to axion dark matter that resonantly converts to radio photons in the magnetospheres surrounding neutron stars (NSs). In this work, we closely examine this possibility by calculating the radiated power from and projected sensitivity to axion dark matter conversion in ensembles of NSs within astrophysical systems like galaxies and globular clusters. We use population synthesis and evolution models to describe the spatial distributions of NSs within these systems and the distributions of NS properties. Focusing on three specific targets for illustration, the Galactic Center of the Milky Way, the globular cluster M54 in the Sagittarius dwarf galaxy, and the Andromeda galaxy, we show that narrow-band radio observations with telescopes such as the Green Bank Telescope and the future Square Kilometer Array may be able to probe the quantum chromodynamics axion over roughly two orders of magnitude in mass, starting at a fraction of a µeV.

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HAYSTAC axion search analysis procedure

Cited by 127 publications

References 38 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

Detecting axion dark matter with radio lines from neutron star populations

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