First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment

The LUX-ZEPLIN (LZ) Collaboration

doi:10.1103/PhysRevLett.131.041002

First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment

The LUX-ZEPLIN (LZ) Collaboration

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Abstract

The LUX-ZEPLIN (LZ) experiment is a dark matter detector centered on a dual-phase xenon time projection chamber operating at the Sanford Underground Research Facility in Lead, South Dakota, USA. This Letter reports results from LZ's first search for Weakly Interacting Massive Particles (WIMPs) with an exposure of 60 live days using a fiducial mass of 5.5 t. A profile-likelihood ratio analysis shows the data to be consistent with a background-only hypothesis, setting new limits on spin-independent WIMP-nucleon, spin-dependent WIMP-neutron, and spin-dependent WIMP-proton cross-sections for WIMP masses above 9 GeV/c$^2$. The most stringent limit is set at 30 GeV/c$^2$, excluding cross sections above 6.5$\times 10^{-48}$ cm$^2$ at the 90\% confidence level.

Original language	English
Article number	041002
Journal	Physical Review Letters
Volume	131
Issue number	4
DOIs	https://doi.org/10.1103/PhysRevLett.131.041002
Publication status	Published - 28 Jul 2023

Bibliographical note

Funding Information:
The 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 awards no. DE-AC02-05CH11231, no. DE-SC0020216, no. DE-SC0012704, no. DE-SC0010010, no. DE-AC02-07CH11359, no. DE-SC0012161, no. DE-SC0015910, no. DE-SC0014223, no. DE-SC0010813, no. DE-SC0009999, no. DE-NA0003180, no. DE-SC0011702, no. DE-SC0010072, no. DE-SC0015708, no. DE-SC0006605, no. DE-SC0008475, no. DE-SC0019193, no. DE-FG02-10ER46709, no. UW PRJ82AJ, no. DE-SC0013542, no. DE-AC02-76SF00515, no. DE-SC0018982, 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 grants 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, no. ST/R003181/1; Portuguese Foundation for Science and Technology (FCT) under grant 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 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. L. 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. We acknowledge Martin Hoferichter and Achim Schwenk for useful discussions. 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 award 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 the registration number 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. We thank the journal reviewers for careful examination of our work, leading to some changes in our analysis and a more robust result. For the purpose of open access, the authors have applied a Creative Commons Attribution (CC BY) license to any Author Accepted Manuscript version arising from this submission.

Publisher Copyright:
© 2023 authors. Published by the American Physical Society.

Keywords

hep-ex
astro-ph.CO

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@article{b9884aa2a2e0476cab88dde5d570084c,

title = "First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment",

abstract = "The LUX-ZEPLIN (LZ) experiment is a dark matter detector centered on a dual-phase xenon time projection chamber operating at the Sanford Underground Research Facility in Lead, South Dakota, USA. This Letter reports results from LZ's first search for Weakly Interacting Massive Particles (WIMPs) with an exposure of 60 live days using a fiducial mass of 5.5 t. A profile-likelihood ratio analysis shows the data to be consistent with a background-only hypothesis, setting new limits on spin-independent WIMP-nucleon, spin-dependent WIMP-neutron, and spin-dependent WIMP-proton cross-sections for WIMP masses above 9 GeV/c$^2$. The most stringent limit is set at 30 GeV/c$^2$, excluding cross sections above 6.5$\times 10^{-48}$ cm$^2$ at the 90\% confidence level.",

keywords = "hep-ex, astro-ph.CO",

author = "{The LUX-ZEPLIN (LZ) Collaboration} and J. Aalbers and Akerib, {D. S.} and Akerlof, {C. W.} and Musalhi, {A. K. Al} and F. Alder and Alsum, {S. K.} and Amarasinghe, {C. S.} and A. Ames and N. Angelides and Ara{\'u}jo, {H. M.} and M. Arthurs and S. Azadi and J. Balajthy and S. Balashov and J. Bang and Bargemann, {J. W.} and J. Barthel and D. Bauer and A. Baxter and K. Beattie and J. Belle and P. Beltrame and Eriksen, {S. R.} and H. Flaecher and L. Korley and L. Kreczko and B. Krikler and B. Penning and Wang, {J. J.} and Wright, {C. J.}",

note = "Funding Information: The 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 awards no. DE-AC02-05CH11231, no. DE-SC0020216, no. DE-SC0012704, no. DE-SC0010010, no. DE-AC02-07CH11359, no. DE-SC0012161, no. DE-SC0015910, no. DE-SC0014223, no. DE-SC0010813, no. DE-SC0009999, no. DE-NA0003180, no. DE-SC0011702, no. DE-SC0010072, no. DE-SC0015708, no. DE-SC0006605, no. DE-SC0008475, no. DE-SC0019193, no. DE-FG02-10ER46709, no. UW PRJ82AJ, no. DE-SC0013542, no. DE-AC02-76SF00515, no. DE-SC0018982, 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{\textquoteright}s Science and Technology Facilities Council under grants 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, no. ST/R003181/1; Portuguese Foundation for Science and Technology (FCT) under grant 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 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. L. 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. We acknowledge Martin Hoferichter and Achim Schwenk for useful discussions. 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 award 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 the registration number 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{\textquoteright}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. We thank the journal reviewers for careful examination of our work, leading to some changes in our analysis and a more robust result. For the purpose of open access, the authors have applied a Creative Commons Attribution (CC BY) license to any Author Accepted Manuscript version arising from this submission. Publisher Copyright: {\textcopyright} 2023 authors. Published by the American Physical Society.",

year = "2023",

month = jul,

day = "28",

doi = "10.1103/PhysRevLett.131.041002",

language = "English",

volume = "131",

journal = "Physical Review Letters",

issn = "0031-9007",

publisher = "American Physical Society (APS)",

number = "4",

}

TY - JOUR

T1 - First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment

AU - The LUX-ZEPLIN (LZ) Collaboration

AU - Aalbers, J.

AU - Akerib, D. S.

AU - Akerlof, C. W.

AU - Musalhi, A. K. Al

AU - Alder, F.

AU - Alsum, S. K.

AU - Amarasinghe, C. S.

AU - Ames, A.

AU - Angelides, N.

AU - Araújo, H. M.

AU - Arthurs, M.

AU - Azadi, S.

AU - Balajthy, J.

AU - Balashov, S.

AU - Bang, J.

AU - Bargemann, J. W.

AU - Barthel, J.

AU - Bauer, D.

AU - Baxter, A.

AU - Beattie, K.

AU - Belle, J.

AU - Beltrame, P.

AU - Eriksen, S. R.

AU - Flaecher, H.

AU - Korley, L.

AU - Kreczko, L.

AU - Krikler, B.

AU - Penning, B.

AU - Wang, J. J.

AU - Wright, C. J.

N1 - Funding Information: The 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 awards no. DE-AC02-05CH11231, no. DE-SC0020216, no. DE-SC0012704, no. DE-SC0010010, no. DE-AC02-07CH11359, no. DE-SC0012161, no. DE-SC0015910, no. DE-SC0014223, no. DE-SC0010813, no. DE-SC0009999, no. DE-NA0003180, no. DE-SC0011702, no. DE-SC0010072, no. DE-SC0015708, no. DE-SC0006605, no. DE-SC0008475, no. DE-SC0019193, no. DE-FG02-10ER46709, no. UW PRJ82AJ, no. DE-SC0013542, no. DE-AC02-76SF00515, no. DE-SC0018982, 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 grants 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, no. ST/R003181/1; Portuguese Foundation for Science and Technology (FCT) under grant 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 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. L. 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. We acknowledge Martin Hoferichter and Achim Schwenk for useful discussions. 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 award 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 the registration number 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. We thank the journal reviewers for careful examination of our work, leading to some changes in our analysis and a more robust result. For the purpose of open access, the authors have applied a Creative Commons Attribution (CC BY) license to any Author Accepted Manuscript version arising from this submission. Publisher Copyright: © 2023 authors. Published by the American Physical Society.

PY - 2023/7/28

Y1 - 2023/7/28

N2 - The LUX-ZEPLIN (LZ) experiment is a dark matter detector centered on a dual-phase xenon time projection chamber operating at the Sanford Underground Research Facility in Lead, South Dakota, USA. This Letter reports results from LZ's first search for Weakly Interacting Massive Particles (WIMPs) with an exposure of 60 live days using a fiducial mass of 5.5 t. A profile-likelihood ratio analysis shows the data to be consistent with a background-only hypothesis, setting new limits on spin-independent WIMP-nucleon, spin-dependent WIMP-neutron, and spin-dependent WIMP-proton cross-sections for WIMP masses above 9 GeV/c$^2$. The most stringent limit is set at 30 GeV/c$^2$, excluding cross sections above 6.5$\times 10^{-48}$ cm$^2$ at the 90\% confidence level.

AB - The LUX-ZEPLIN (LZ) experiment is a dark matter detector centered on a dual-phase xenon time projection chamber operating at the Sanford Underground Research Facility in Lead, South Dakota, USA. This Letter reports results from LZ's first search for Weakly Interacting Massive Particles (WIMPs) with an exposure of 60 live days using a fiducial mass of 5.5 t. A profile-likelihood ratio analysis shows the data to be consistent with a background-only hypothesis, setting new limits on spin-independent WIMP-nucleon, spin-dependent WIMP-neutron, and spin-dependent WIMP-proton cross-sections for WIMP masses above 9 GeV/c$^2$. The most stringent limit is set at 30 GeV/c$^2$, excluding cross sections above 6.5$\times 10^{-48}$ cm$^2$ at the 90\% confidence level.

KW - hep-ex

KW - astro-ph.CO

U2 - 10.1103/PhysRevLett.131.041002

DO - 10.1103/PhysRevLett.131.041002

M3 - Article (Academic Journal)

C2 - 37566836

SN - 0031-9007

VL - 131

JO - Physical Review Letters

JF - Physical Review Letters

IS - 4

M1 - 041002

ER -

First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment

Abstract

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