2018
DOI: 10.1103/physrevlett.120.221301
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Search for Boosted Dark Matter Interacting with Electrons in Super-Kamiokande

Abstract: A search for boosted dark matter using 161.9 kt yr of Super-Kamiokande IV data is presented. We search for an excess of elastically scattered electrons above the atmospheric neutrino background, with a visible energy between 100 MeV and 1 TeV, pointing back to the Galactic center or the Sun. No such excess is observed. Limits on boosted dark matter event rates in multiple angular cones around the Galactic center and Sun are calculated. Limits are also calculated for a baseline model of boosted dark matter prod… Show more

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Cited by 63 publications
(84 citation statements)
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“…If the speed of these recoiling electrons is > 0.75c, they emit detectable Cherenkov light. Such events are detected by Super-Kamiokande for deposition energies above the threshold of 100 MeV [62]. The main target of the search is dark matter coming from the center of the galaxy, and constraints are put on events within a cone with a certain opening angle measured from the center of the galaxy.…”
Section: Relativistic Electron Recoil and Subsequent Cherenkov Lightmentioning
confidence: 99%
See 1 more Smart Citation
“…If the speed of these recoiling electrons is > 0.75c, they emit detectable Cherenkov light. Such events are detected by Super-Kamiokande for deposition energies above the threshold of 100 MeV [62]. The main target of the search is dark matter coming from the center of the galaxy, and constraints are put on events within a cone with a certain opening angle measured from the center of the galaxy.…”
Section: Relativistic Electron Recoil and Subsequent Cherenkov Lightmentioning
confidence: 99%
“…Below the dashed line, the maximum momentum of accelerated CHAMPs is below the threshold, m 100 MeV/m e . For q > 0.1, photomultiplier tubes (PMTs) in the outer detector typically receive more than one photon from the Cherenkov radiation of CHAMPs, giving events that are vetoed in the analysis of [62]. The integrated flux of atmospheric muons 2 km below the Antarctic ice is Φ µ /4π ≈ 10 −7 cm −2 s −1 sr −1 [64] and contributes 3% [63] of the background rate.…”
Section: Relativistic Electron Recoil and Subsequent Cherenkov Lightmentioning
confidence: 99%
“…For the dark-strahlung channel, we assume the all-sky survey (i.e., θ C = 180 • ) and negligible background, whereas for the leading-order, we consider two more search cones, θ C = 10 • (dot-dashed lines) and θ C = 40 • (dashed lines) as per suggestions in Refs. [1,4], in addition to the all-sky survey (solid lines). The number of neutrino-induced background events for the leading-order process is calculated with Eqs.…”
Section: Experimental Sensitivities Of Dunementioning
confidence: 99%
“…The models of boosted dark matter (BDM) are receiving rising attention [1,2] as an alternative scenario to reconcile the paradigm of thermal dark-matter with the null observation of dark-matter-induced signatures via non-gravitational interactions [3,4]. Many of them predict that some (subdominant) dark-matter components can be substantially boosted in the present universe and manifest themselves by relativistic scattering signatures in terrestrial detectors.…”
Section: Introductionmentioning
confidence: 99%
“…In this paper, we demonstrate that large underground neutrino detectors as well as large directional dark matter detectors can provide a new method to probe inelastic dark matter. Other proposed searches for dark matter that could yield a signal in neutrino detectors include dark matter that destroys target baryons [25][26][27][28], dark matter that yields annihilation or decay products detectable in these experiments [29][30][31][32][33][34][35][36][37][38][39], self-destructing dark matter [40], dark matter produced at high-intensity accelerators or radioactive sources [41], or dark matter bounced off energetic cosmic rays [41,42]. Consider a dark matter particle with mass of order a TeV traversing through the Earth.…”
Section: Introductionmentioning
confidence: 99%