Sub-MeV bosonic dark matter, misalignment mechanism, and galactic dark matter halo luminosities

Yang, Qiaoli; Di, Haoran

doi:10.1103/physrevd.95.075032

Cited by 5 publications

(3 citation statements)

References 73 publications

(88 reference statements)

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“…Moving to the 'ultra-light' regime requires yet a new battery of techniques (including relaxing the energy threshold by studying absorption, and not only scattering, of DM), e.g. [22,[40][41][42][43][44][45][46][47][48]. For both light and ultra-light dark matter, a key idea is to use very precise set-ups that may be sensitive to small or even vanishing momentum transfer.…”

Section: Introductionmentioning

confidence: 99%

Exploring the ultra-light to sub-MeV dark matter window with atomic clocks and co-magnetometers

Alonso

Blas

Wolf

2019

J. High Energ. Phys.

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Particle dark matter could have a mass anywhere from that of ultralight candidates, m χ ∼ 10 −21 eV, to scales well above the GeV. Conventional laboratory searches are sensitive to a range of masses close to the weak scale, while new techniques are required to explore candidates outside this realm. In particular lighter candidates are difficult to detect due to their small momentum. Here we study two experimental set-ups which do not require transfer of momentum to detect dark matter: atomic clocks and co-magnetometers. These experiments probe dark matter that couples to the spin of matter via the very precise measurement of the energy difference between atomic states of different angular momenta. This coupling is possible (even natural) in most dark matter models, and we translate the current experimental sensitivity into implications for different dark matter models. It is found that the constraints from current atomic clocks and co-magnetometers can be competitive in the mass range m χ ∼ 10 −21 − 10 3 eV, depending on the model. We also comment on the (negligible) effect of different astrophysical neutrino backgrounds. 3 We take here the theory after EWSB, otherwise e L couplings come together with ν s and G u L = G d L . 4 For example the operatorψγ µ γ 5 ψ∂ µ χ 2 is proportional to the transferred momentum q so we discard it, but ∂ µ χ 2 is the only current that can be built with a real field; in contrast for a complex scalar we have two: ∂ µ (χ † χ) and (∂ µ χ † )χ − χ † ∂ µ χ. The second one is proportional to the sum of incoming and outgoing DM momenta in a scattering process.

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Section: Introductionmentioning

confidence: 99%

Exploring the ultra-light to sub-MeV dark matter window with atomic clocks and co-magnetometers

Alonso

Blas

Wolf

2019

J. High Energ. Phys.

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“…After becoming massive, axions may intuitively evolve like ordinary dark matter, without special phenomena. But thanks to the bosonic nature of axions and their very high phase space density, a number of novel condensation-derived effects have been suggested to occur [25][26][27][114][115][116], as we will explore in this section.…”

Section: Iiib2 the Condensation Of Axion Dark Mattermentioning

confidence: 99%

Natural Explanation for 21 cm Absorption Signals via Axion-Induced Cooling

Houston

et al. 2018

Phys. Rev. Lett.

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The EDGES Collaboration has reported an anomalously strong 21 cm absorption feature corresponding to the era of first star formation, which may indirectly betray the influence of dark matter during this epoch. We demonstrate that, by virtue of the ability to mediate cooling processes while in the condensed phase, a small amount of axion dark matter can explain these observations within the context of standard models of axions and axionlike particles. The EDGES best-fit result favors an axionlike particle mass in the (10, 450) meV range, which can be compressed for the QCD axion to (100, 450) meV in the absence of fine tuning. Future experiments and large scale surveys, particularly the International Axion Observatory (IAXO) and EUCLID, should have the capability to directly test this scenario.

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“…Constraints on their parameter space can also be set using current gravitational wave detectors [30][31][32]. However, ultralight vector bosons are also conceivable fuzzy DM candidates [7,[33][34][35][36][37][38][39][40][41][42][43][44]. The tightest constraints on the mass of fuzzy DM come from observations of large scale structure in the Universe, and very recent studies suggest that m ϕ > 10 −21 eV may be required [10,12,45].…”

Section: Introductionmentioning

confidence: 99%

Fuzzy dark matter and nonstandard neutrino interactions

et al. 2018

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We discuss novel ways in which neutrino oscillation experiments can probe dark matter. In particular, we focus on interactions between neutrinos and ultralight ("fuzzy") dark matter particles with masses of order 10 −22 eV. It has been shown previously that such dark matter candidates are phenomenologically successful and might help ameliorate the tension between predicted and observed small scale structures in the Universe. We argue that coherent forward scattering of neutrinos on fuzzy dark matter particles can significantly alter neutrino oscillation probabilities. These effects could be observable in current and future experiments. We set new limits on fuzzy dark matter interacting with neutrinos using T2K and solar neutrino data, and we estimate the sensitivity of reactor neutrino experiments and of future long-baseline accelerator experiments. These results are based on detailed simulations in GLoBES. We allow the dark matter particle to be either a scalar or a vector boson. In the latter case, we find potentially interesting connections to models addressing various B physics anomalies.

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Sub-MeV bosonic dark matter, misalignment mechanism, and galactic dark matter halo luminosities

Cited by 5 publications

References 73 publications

Exploring the ultra-light to sub-MeV dark matter window with atomic clocks and co-magnetometers

Exploring the ultra-light to sub-MeV dark matter window with atomic clocks and co-magnetometers

Natural Explanation for 21 cm Absorption Signals via Axion-Induced Cooling

Fuzzy dark matter and nonstandard neutrino interactions

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