Parametrically enhanced hidden photon search

Graham, Peter W.; Mardon, Jeremy; Rajendran, Surjeet; Zhao, Yue

doi:10.1103/physrevd.90.075017

Cited by 55 publications

(81 citation statements)

References 49 publications

(115 reference statements)

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“…(5.18), for light DM scattering off electrons via a kinetically mixed hidden photon, which obtains its mass via the Stuckelberg mechanism, for a variety of different mediator masses (solid colored curves). Constraints include stellar cooling [87], CMB [91], CROWS [89,90], measurements of Coulomb's law [91], decoupling at recombination [67,68] and self-interactions [59]. Bottom: direct detection cross section between light DM and electrons, for several benchmarks of heavy mediators (same as in figure 5).…”

Section: Kinetically Mixed Resultsmentioning

confidence: 99%

“…For even lighter mediator masses, is bound by photon-dark photon mixing through level-crossing in the CMB [91], as well as from the CROWS experiment [89,90] and measurements of deviations from Coulomb's law [91]; these are lifted for m φ 10 −14 eV, where measurements of the shape of the static magnetic field of Jupiter allows kinetic mixing as large as O(10 −2 − 1) (see e.g. refs.…”

Section: Kinetically Mixed Stellar Constraintsmentioning

confidence: 99%

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Detecting superlight dark matter with Fermi-degenerate materials

Hochberg

Pyle

Zhao

et al. 2016

J. High Energ. Phys.

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202

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We examine in greater detail the recent proposal of using superconductors for detecting dark matter as light as the warm dark matter limit of O(keV). Detection of such light dark matter is possible if the entire kinetic energy of the dark matter is extracted in the scattering, and if the experiment is sensitive to O(meV) energy depositions. This is the case for Fermi-degenerate materials in which the Fermi velocity exceeds the dark matter velocity dispersion in the Milky Way of ∼ 10 −3 . We focus on a concrete experimental proposal using a superconducting target with a transition edge sensor in order to detect the small energy deposits from the dark matter scatterings. Considering a wide variety of constraints, from dark matter self-interactions to the cosmic microwave background, we show that models consistent with cosmological/astrophysical and terrestrial constraints are observable with such detectors. A wider range of viable models with dark matter mass below an MeV is available if dark matter or mediator properties (such as couplings or masses) differ at BBN epoch or in stellar interiors from those in superconductors. We also show that metal targets pay a strong in-medium suppression for kinetically mixed mediators; this suppression is alleviated with insulating targets.

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Section: Kinetically Mixed Resultsmentioning

confidence: 99%

Section: Kinetically Mixed Stellar Constraintsmentioning

confidence: 99%

Detecting superlight dark matter with Fermi-degenerate materials

Hochberg

Pyle

Zhao

et al. 2016

J. High Energ. Phys.

Self Cite

202

239

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show abstract

“…However, if such interactions exist, massive vector boson dark matter can be searched for over this range of masses using well developed electromagnetic resonator technologies, as suggested in [18,48]. Further, the existence of new vector bosons in this frequency range can also be directly probed by various "Light-Shining-Through-aWall" experiments wherein these vector bosons are produced by a laboratory source and then subsequently detected [30,56]. Thus, in this range of parameters, this scenario leads to an exciting set of experiments.…”

Section: Discussionmentioning

confidence: 99%

“…These bounds include stellar production of the vector [51,52], precision tests of electromagnetism [29,30,53], and distortion of the CMB due to conversion of photons into the vector [54]. Since these are bounds on ε rather than ε √ ρ γ , an assumption about the vector abundance was needed in order to put the bounds on the plot.…”

Section: Dark Matter Phenomenologymentioning

confidence: 99%

Vector dark matter from inflationary fluctuations

2016

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We calculate the production of a massive vector boson by quantum fluctuations during inflation.This gives a novel dark-matter production mechanism quite distinct from misalignment or thermal production. While scalars and tensors are typically produced with a nearly scale-invariant spectrum, surprisingly the vector is produced with a power spectrum peaked at intermediate wavelengths. Thus dangerous, long-wavelength, isocurvature perturbations are suppressed. Further, at long wavelengths the vector inherits the usual adiabatic, nearly scale-invariant perturbations of the inflaton, allowing it to be a good dark matter candidate. The final abundance can be calculated precisely from the mass and the Hubble scale of inflation, HI . Saturating the dark matter abundance we find a prediction for the mass m ≈ 10 −5 eV×(10 14 GeV/HI ) 4 . High-scale inflation, potentially observable in the CMB, motivates an exciting mass range for recently proposed direct detection experiments for hidden photon dark matter. Such experiments may be able to reconstruct the distinctive, peaked power spectrum, verifying that the dark matter was produced by quantum fluctuations during inflation and providing a direct measurement of the scale of inflation. Thus a detection would not only be the discovery of dark matter, it would also provide an unexpected probe of inflation itself.

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“…This coupling can cause anomalous oscillating electromagnetic effects that have been the subject of other experiments [36,37]. This kinetic mixing coupling term can be diagonalized into the form…”

Section: Vector Couplingsmentioning

confidence: 98%

Spin precession experiments for light axionic dark matter

et al. 2018

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Axionlike particles are promising candidates to make up the dark matter of the Universe, but it is challenging to design experiments that can detect them over their entire allowed mass range. Dark matter in general, and, in particular, axionlike particles and hidden photons, can be as light as roughly 10 −22 eV (∼10 −8 Hz), with astrophysical anomalies providing motivation for the lightest masses ("fuzzy dark matter"). We propose experimental techniques for direct detection of axionlike dark matter in the mass range from roughly 10 −13 eV (∼10 2 Hz) down to the lowest possible masses. In this range, these axionlike particles act as a time-oscillating magnetic field coupling only to spin, inducing effects such as a timeoscillating torque and periodic variations in the spin-precession frequency with the frequency and direction of these effects set by the axion field. We describe how these signals can be measured using existing experimental technology, including torsion pendulums, atomic magnetometers, and atom interferometry. These experiments demonstrate a strong discovery capability, with future iterations of these experiments capable of pushing several orders of magnitude past current astrophysical bounds.

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Parametrically enhanced hidden photon search

Cited by 55 publications

References 49 publications

Detecting superlight dark matter with Fermi-degenerate materials

Detecting superlight dark matter with Fermi-degenerate materials

Vector dark matter from inflationary fluctuations

Spin precession experiments for light axionic dark matter

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