Please use this identifier to cite or link to this item: https://hdl.handle.net/10316/112202
DC FieldValueLanguage
dc.contributor.authorBrás, P.-
dc.contributor.authorCabrita, R.-
dc.contributor.authorLindote, A.-
dc.contributor.authorLopes, M. I.-
dc.contributor.authorLopez-Asamar, E.-
dc.contributor.authorNeves, F.-
dc.contributor.authorPereira, G.-
dc.contributor.authorPorzio, D.-
dc.contributor.authorSilva, C.-
dc.contributor.authorSolovov, V. N.-
dc.contributor.authorThe LUX-ZEPLIN Collaboration-
dc.date.accessioned2024-01-24T12:03:47Z-
dc.date.available2024-01-24T12:03:47Z-
dc.date.issued2023-07-
dc.identifier.urihttps://hdl.handle.net/10316/112202-
dc.description.abstractThe LUX-ZEPLIN experiment recently reported limits on WIMP-nucleus interactions from its initial science run, down to 9.2 × 10−48 cm2 for the spin-independent interaction of a 36 GeV=c2 WIMP at 90% confidence level. In this paper, we present a comprehensive analysis of the backgrounds important for this result and for other upcoming physics analyses, including neutrinoless double-beta decay searches and effective field theory interpretations of LUX-ZEPLIN data. We confirm that the in-situ determinations of bulk and fixed radioactive backgrounds are consistent with expectations from the ex-situ assays. The observed background rate after WIMP search criteria were applied was ð6.3 0.5Þ × 10−5 events=keVee=kg=day in the low-energy region, approximately 60 times lower than the equivalent rate reported by the LUX experiment.pt
dc.description.sponsorshipThe research supporting this work took place in part at SURF in Lead, South Dakota. Funding for this work is supported by the U.S. Department of Energy, Office of Science, Office of High Energy Physics under Contracts No. DE-AC02-05CH11231, No. DE-SC0020216, No. DESC0012704, No. DE-SC0010010, No. DE-AC02- 07CH11359, No. DE-SC0012161, No. DE-SC0015910, No. DE-SC0014223, No. DE-SC0010813, No. DESC0009999, No. DE-NA0003180, No. DE-SC0011702, No. DE-SC0010072, No. DE-SC0015708, No. DESC0006605, No. DE-SC0008475, No. DE-SC0019193, No. DE-FG02-10ER46709, No. UW PRJ82AJ, No. DEFIG SC0013542, No. DE-AC02-76SF00515, No. DESC0018982, No. DE-SC0019066, No. DE-SC0015535, No. DE-SC0019319, No. DE-AC52-07NA27344, and No. DOE-SC0012447. This research was also supported by U.S. National Science Foundation (NSF); the UKRI’s Science and Technology Facilities Council under Awards No. ST/M003744/1, No. ST/M003655/1, No. ST/ M003639/1, No. ST/M003604/1, No. ST/M003779/1, No. ST/M003469/1, No. ST/M003981/1, No. ST/ N000250/1, No. ST/N000269/1, No. ST/N000242/1, No. ST/N000331/1, No. ST/N000447/1, No. ST/ N000277/1, No. ST/N000285/1, No. ST/S000801/1, No. ST/S000828/1, No. ST/S000739/1, No. ST/ S000879/1, No. ST/S000933/1, No. ST/S000844/1, No. ST/S000747/1, No. ST/S000666/1, and No. ST/ R003181/1; Portuguese Foundation for Science and Technology (FCT) under Award No. PTDC/FIS-PAR/ 2831/2020; the Institute for Basic Science, Korea (Budget No. IBS-R016-D1). We acknowledge additional support from the STFC Boulby Underground Laboratory in the U.K., the GridPP [66,67] and IRIS Collaborations, in particular at Imperial College London and additional support by the University College London (UCL) Cosmoparticle Initiative. We acknowledge additional support from the Center for the Fundamental Physics of the Universe, Brown University. K. T. Lesko acknowledges the support of Brasenose College and Oxford University. The LZ Collaboration acknowledges key contributions of Dr. Sidney Cahn, Yale University, in the production of calibration sources. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. We gratefully acknowledge support from GitLab through its GitLab for Education Program. The University of Edinburgh is a charitable body, registered in Scotland, with Registration No. SC005336. The assistance of SURF and its personnel in providing physical access and general logistical and technical support is acknowledged. We acknowledge the South Dakota Governor’s office, the South Dakota Community Foundation, the South Dakota State University Foundation, and the University of South Dakota Foundation for use of xenon. We also acknowledge the University of Alabama for providing xenon.pt
dc.language.isoengpt
dc.publisherAmerican Physical Societypt
dc.rightsopenAccesspt
dc.rights.urihttp://creativecommons.org/licenses/by/4.0/pt
dc.titleBackground determination for the LUX-ZEPLIN dark matter experimentpt
dc.typearticlept
degois.publication.firstPage012010pt
degois.publication.issue1pt
degois.publication.titlePhysical Review Dpt
dc.peerreviewedyespt
dc.identifier.doi10.1103/PhysRevD.108.012010-
degois.publication.volume108pt
dc.date.embargo2023-07-01*
uc.date.periodoEmbargo0pt
item.languageiso639-1en-
item.fulltextCom Texto completo-
item.grantfulltextopen-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.openairetypearticle-
item.cerifentitytypePublications-
crisitem.author.researchunitLIP – Laboratory of Instrumentation and Experimental Particle Physics-
crisitem.author.researchunitLIP – Laboratory of Instrumentation and Experimental Particle Physics-
crisitem.author.researchunitLIP – Laboratory of Instrumentation and Experimental Particle Physics-
crisitem.author.orcid0000-0002-1771-1517-
crisitem.author.orcid0000-0002-0659-7034-
Appears in Collections:LIP - Artigos em Revistas Internacionais
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