Design and implementation of the ABRACADABRA-10 cm axion dark matter search

Ouellet, J. L.; Salemi, C.; Foster, Joshua W.; Henning, R.; Bogorad, Zachary; Conrad, J. M.; Formaggio, J. A.; Kahn, Yonatan; Minervini, J.V.; Radovinsky, A.; Rodd, Nicholas L.; Safdi, Benjamin R.; Thaler, Jesse; Winklehner, Daniel; Winslow, L. A.

doi:10.1103/physrevd.99.052012

Cited by 61 publications

(62 citation statements)

References 36 publications

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“…This conclusion was also reached in [38] using the Einstein-Cartan theory of gravity . This conclusion agrees with the experimental lack of evidence for various hypothetical particles that have been proposed as candidates for dark matter, such as axions [64][65][66] or weakly interacting massive particles [67,68] that are predicted by supersymmetric scenarios [69,70].…”

supporting

confidence: 87%

Non-particle dark matter from Hubble parameter

Popławski

2019

Eur. Phys. J. C

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The measurements of the Hubble parameter using the cosmic microwave background radiation appear to be inconsistent with the measurements of this parameter using Cepheid variable stars. This inconsistency may be a result of using the CDM cosmology, which assumes pressureless dark matter, in extrapolating the data from the recombination time to the present time. We show that both measurements are consistent if dark matter satisfies an equation of state in which the pressure p and the energy density are related by p = w with a negative value of w. The data give w ≈ −0.01. The negative value of w indicates that dark matter would not be formed by particles, which is consistent with the lack of experimental evidence for them.The observations of the temperature angular power spectrum of the cosmic microwave background (CMB) radiation provide the information about the composition of the universe [1]. The measurements of the position of the first acoustic peak show that the universe is nearly flat, with the density parameter ≈ 1. The measurements of the amplitudes of the peaks determine the values of b h 2 and c h 2 , where b is the density parameter for baryonic matter, c is the density parameter for dark matter, and the present-day Hubble parameter H 0 = 100h km/s/Mpc. Combining these values with the measured h = 0.674 ± 0.005 gives (omitting errors) b = 0.049 and c = 0.265, as obtained by the Planck satellite [2,3]. Consequently, the density parameter for total matter is m = 0.314.Before the Planck measurements, most measured values of h also clustered around 0.68, including the data from high-redshift type Ia supernovae (SN Ia) [4,5], Wilkinson Microwave Anisotropy Probe CMB data [6], baryon acoustic oscillations (BAO) [7], SN Ia and BAO data [8], measurements of the Hubble parameter at intermediate redshifts [9], and large-scale-structure data [10]. Assuming a flat universe, = 1 − m = 0.686 for dark energy (cosmological constant). The resulting age of the universe is t univ = a e-mail: NPoplawski@newhaven.edu da/(a H) =

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supporting

confidence: 87%

Non-particle dark matter from Hubble parameter

Popławski

2019

Eur. Phys. J. C

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“…In figure 1, we show the regions excluded by CAST [27] in blue shading, ADMX [28][29][30][31] in red shading, ABRACADABRA [32][33][34] in brown shading, SHAFT [35] in purple shading, RBF and UF experiments [36][37][38] in orange shading, and HAYSTAC [39,40] in magenta shading. The constraints from astrophysical searches are shown by transparent shadings, including horizontal branch (HB) stars [41] in red, PKS 2155-304 by HESS [42] in magenta, NGC 1275 by Fermi [43] in orange, SN1987A [44] in green, and Chandra's observation of Hydra A [45], M87 [46], and NGC 1275 [47] in pink.…”

Section: Photonsmentioning

confidence: 99%

“…The constraints from astrophysical searches are shown by transparent shadings, including horizontal branch (HB) stars [41] in red, PKS 2155-304 by HESS [42] in magenta, NGC 1275 by Fermi [43] in orange, SN1987A [44] in green, and Chandra's observation of Hydra A [45], M87 [46], and NGC 1275 [47] in pink. The prospects for future proposed and planned experiments are shown individually by the red dashed curves for BabyIAXO and IAXO [48], black dashed curve for ALPS-II [49], blue dot-dashed lines for ABRA-CADABRA [32][33][34] with a broadband search, blue dashed lines for DM Radio-50L and DM Radio-m 3 [50][51][52], which has merged with ABRACADABRA, for a resonant search, 2 cyan dashed lines for CULTASK [53,54], magenta lines for MADMAX [55], orange dashed JHEP01(2021)172…”

Section: Photonsmentioning

confidence: 99%

Predictions for axion couplings from ALP cogenesis

Hall

Harigaya

2021

J. High Energ. Phys.

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Adding an axion-like particle (ALP) to the Standard Model, with a field velocity in the early universe, simultaneously explains the observed baryon and dark matter densities. This requires one or more couplings between the ALP and photons, nucleons, and/or electrons that are predicted as functions of the ALP mass. These predictions arise because the ratio of dark matter to baryon densities is independent of the ALP field velocity, allowing a correlation between the ALP mass, ma, and decay constant, fa. The predicted couplings are orders of magnitude larger than those for the QCD axion and for dark matter from the conventional ALP misalignment mechanism. As a result, this scheme, ALP cogenesis, is within reach of future experimental ALP searches from the lab and stellar objects, and for dark matter.

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“…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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Design and implementation of the ABRACADABRA-10 cm axion dark matter search

Cited by 61 publications

References 36 publications

Non-particle dark matter from Hubble parameter

Non-particle dark matter from Hubble parameter

Predictions for axion couplings from ALP cogenesis

Velocity substructure from Gaia and direct searches for dark matter

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