@Article{AristizabalSierra_etal2024,
author="Aristizabal Sierra, D.
and De Romeri, V.
and Ternes, C. A.",
title="Reactor neutrino background in next-generation dark matter detectors",
journal="Physical Review D",
year="2024",
publisher="Amer Physical Soc",
volume="109",
number="11",
pages="115026--7pp",
abstract="Third -generation dark matter detectors will be fully sensitive to the 8 B solar neutrino flux. Because of this, the characterization of such a background has been the subject of extensive analyses over the last few years. In contrast, little is known about the impact of reactor neutrinos. In this paper, we report on the implications of such a flux for dark matter direct -detection searches. We consider five potential detector deployment sites envisioned by the recently established XLZD Consortium: SURF, SNOLAB, Kamioka, LNGS, and Boulby. By using public reactor data, we construct five reactor clusters -involving about 100 currently operating commercial nuclear reactors each -and determine the net neutrino flux at each detector site. Assuming a xenon -based detector and a 50 ton -year exposure, we show that in all cases the neutrino event rate may be sizable, depending on energy recoil thresholds. Of all possible detector sites, SURF and LNGS are those with the smallest reactor neutrino background. On the contrary, SNOLAB and Boulby are subject to the strongest reactor neutrino fluxes, with Kamioka being subject to a more moderate background. Our findings demonstrate that reactor neutrino fluxes should be taken into account in the next round of dark matter searches. We argue that this background may be particularly relevant for directional detectors, provided they meet the requirements we have employed in this analysis.",
optnote="WOS:001255433200010",
optnote="exported from refbase (https://references.ific.uv.es/refbase/show.php?record=6167), last updated on Tue, 09 Jul 2024 06:47:35 +0000",
issn="2470-0010",
doi="10.1103/PhysRevD.109.115026",
opturl="https://arxiv.org/abs/2402.06416",
opturl="https://doi.org/10.1103/PhysRevD.109.115026",
language="English"
}