2021
DOI: 10.1103/physrevd.104.115022
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Atmospheric neutrinos in next-generation xenon and argon dark matter experiments

Abstract: We study the sensitivity of future xenon-and argon-based dark matter and neutrino detection experiments to low-energy atmospheric neutrinos. Not accounting for experimental backgrounds, the primary obstacle for identifying nuclear recoils induced by atmospheric neutrinos in xenon is the tail of the electron recoil distribution due to pp solar neutrinos. We use the NEST code to model the solar and atmospheric neutrino signals in a xenon detector and find that an exposure of 700 tonne-years will produce a 5σ det… Show more

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Cited by 22 publications
(18 citation statements)
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“…As such dark matter detectors grow in size and sensitivity, neutrinos from the sun [40,41], cosmic rays in the atmosphere [42,43,44], and diffuse supernovae [45,46,47] will become significant backgrounds to dark matter searches [48,49,50,51,52,53,54,55]. These neutrinos can scatter coherently with the target nucleus as a whole [56], as recently measured for the first time (for reactor neutrinos) in CsI(Na) [57] and argon [58].…”
Section: Introductionmentioning
confidence: 99%
“…As such dark matter detectors grow in size and sensitivity, neutrinos from the sun [40,41], cosmic rays in the atmosphere [42,43,44], and diffuse supernovae [45,46,47] will become significant backgrounds to dark matter searches [48,49,50,51,52,53,54,55]. These neutrinos can scatter coherently with the target nucleus as a whole [56], as recently measured for the first time (for reactor neutrinos) in CsI(Na) [57] and argon [58].…”
Section: Introductionmentioning
confidence: 99%
“…The neutrino recoil spectra, as well as flux uncertainties on the different components, are taken to be the same as in [84], with spectra from Ref. [147][148][149][150]. WIMP recoil spectra are computed using the wimprates package [151], with spin-independent computations from Ref.…”
Section: B Wimp Sensitivity Projections: Methodsmentioning
confidence: 99%
“…The 8 B flux is measured at the 2% level from Solar neutrino data [444]. The atmospheric flux on the other hand, is difficult to measure and to theoretically predict at the relevant sub-100 MeV energies, so it still has a ∼20% uncertainty (section V C and [150]). Any reduction in these uncertainties will, in effect, "lower" the neutrino fog.…”
Section: Q Confronting the Neutrino Fogmentioning
confidence: 99%
“…State-of-the-art experiments aiming for the direct detection of WIMP dark matter (DM), like XENONnT [1] and LZ [2], deploy a liquid xenon target inside a TPC instrumented with photosensors to detect light signals. Future DM-search experiments, like the DARWIN observatory [3], expand their science reach to nuclear physics, like the hypothetically neutrinoless second-order weak decays of 136 Xe [4] and 124 Xe [5], and the physics of solar and atmospheric neutrinos [6,7]. Any particle interacting with the liquid xenon target deposits energy in the form of scintillation, ionisation and heat.…”
Section: Introductionmentioning
confidence: 99%