Abstract
A search for boosted dark matter using 161.9kt 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 100MeV and 1TeV, 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 produced from cold dark matter annihilation or decay. This is the first experimental search for boosted dark matter from the Galactic center or the Sun interacting in a terrestrial detector.
Highlights
Published by the American Physical SocietyThis Letter reports the results of a search for boosted dark matter coupling to electrons in Super-Kamiokande (SK), with the boosted dark matter originating in the Galactic center or the Sun and with scattered electron energies ranging from 100 MeV to 1 TeV
A search for boosted dark matter using 161.9 kt yr of Super-Kamiokande IV data is presented
This is the first experimental search for boosted dark matter from the Galactic center or the Sun interacting in a terrestrial detector
Summary
This Letter reports the results of a search for boosted dark matter coupling to electrons in Super-Kamiokande (SK), with the boosted dark matter originating in the Galactic center or the Sun and with scattered electron energies ranging from 100 MeV to 1 TeV This is the first time that this class of high-energy “electron elastic scatterlike” events has been studied at SK. This way, the results can be applied to any model that predicts a source of particles from the Galactic center or Sun which would scatter electrons to energies greater than 100 MeV. The importance of the decay electron and neutron tagging cuts is evident in the highest-energy sample (Evis > 20 GeV), where they together reduce the background by about a factor of 10 while having a minimal effect on the signal efficiency. While the off-source method works well for the two lower-energy samples, there are too few events in the highest-energy sample (Evis > 20 GeV) for it to be
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