Cosmogenic production of 
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi>Ar</mml:mi></mml:mrow><mml:mprescripts/><mml:none/><mml:mrow><mml:mn>37</mml:mn></mml:mrow></mml:mmultiscripts></mml:mrow></mml:math>
 in the context of the LUX-ZEPLIN experiment

Aalbers, J.; Akerib, D. S.; Musalhi, A. K. Al; Alder, F.; Alsum, S.; Amarasinghe, C. S.; Ames, Adelaide; Anderson, Tyler; Angelides, N.; Araújo, H. M.; Armstrong, J. E.; Arthurs, M.; Bai, X.; Baker, Alexander A.; Balajthy, J.; Balashov, S.; Bang, J.; Bargemann, J. W.; Bauer, D.; Baxter, A.; Beattie, K.; Bernard, E. P.; Bhatti, A.; Biekert, A.; Biesiadzinski, T. P.; Birch, H. J.; Blockinger, G. M.; Bodnia, E.; Boxer, B.; Brew, C.; Brás, P.; Burdin, S.; Busenitz, J.; Buuck, M.; Cabrita, R.; Carmona-Benitez, M. C.; Cascella, M.; Chan, C.; Chawla, Aviral; Chen, H.; Chott, N.; Cole, A. A.; Converse, M. V.; Cottle, A.; Cox, G. A.; Creaner, Oisín; Cutter, J. E.; Dahl, C. E.; David, A.; Viveiros, L. de; Dobson, J.; Druszkiewicz, E.; Eriksen, S. R.; Fan, A.; Fayer, S.; Fearon, N. M.; Fiorucci, S.; Flaecher, H.; Fraser, E. D.; Fruth, T.; Gaitskell, R. J.; Genovesi, J.; Ghag, C.; Gibson, E. F.; Gilchriese, M.; Gokhale, S.; Grinten, M. G. D. van der; Gwilliam, C. B.; Hall, C.; Haselschwardt, S. J.; Hertel, S. A.; Horn, M.; Huang, D. Q.; Hunt, D.; Ignarra, C. M.; Jahangir, O.; James, R. S.; Ji, W.; Johnson, James Turner; Kaboth, A.; Kamaha, A.; Kamdin, K.; Khaitan, D.; Khazov, A.; Khurana, I.; Kodroff, D.; Korley, L.; Korolkova, E. V.; Kraus, H.; Kravitz, S.; Kreczko, L.; Kudryavtsev, V. A.; Leason, E. A.; Leonard, D. S.; Lesko, K. T.; Lévy, C.; J., Lee,; Lin, J.; Lindote, A.; Linehan, R.; Lippincott, W. H.; X., Liu,; Lopes, M. I.; Asamar, E. López; Lopez-Paredes, B.; Lorenzon, W.; Luitz, S.; Majewski, P.; Manalaysay, A.; Manenti, L.; Mannino, R. L.; Marangou, N.; McCarthy, M.; McKinsey, D. N.; McLaughlin, J.; Miller, E. H.; Mizrachi, E.; Monte, A.; Monzani, M. E.; Morad, J. A.; Mendoza, J. D. Morales; Morrison, E.; Mount, B. J.; Murphy, A. St. J.; Naim, D.; Naylor, Andrew; Nedlik, C.; Nelson, H. N.; Neves, F.; Nikoleyczik, J. A.; Nilima, A.; Olcina, I.; Oliver-Mallory, K. C.; Pal, Surajit; Palladino, K. J.; Palmer, J. D.; Parveen, N.; Patton, S.; Pease, E. K.; Penning, B.; Pereira, G.; Perry, E.; Pershing, J.; Piepke, A.; Porzio, D.; Qie, Y.; Reichenbacher, J.; Rhyne, C.; Richards, A.; Riffard, Q.; Rischbieter, G. R. C.; Rosero, R.; Rossiter, P.; Rushton, T.; Santone, D.; Sazzad, A. B. M. R.; Schnee, R. W.; Scovell, P. R.; Shaw, S.; Shutt, T.; Silk, Joseph; Silva, C.; Sinev, G.; Smith, R.; Solmaz, M.; Solovov, V.; Sørensen, P.; Soria, Jason; Stancu, I.; Stevens, A.; Stifter, K.; Suerfu, B.; Sumner, T. J.; Swanson, N.; Szydagis, M.; Taylor, WC; Taylor, R.; Temples, D.; Terman, P. A.; Tiedt, D. R.; Timalsina, M.; To, W. H.; Tong, Z.; Tovey, D. R.; Trask, M.; Tripathi, M.; Tronstad, D. R.; Turner, W.; Utku, U.; Vaitkus, Audrius; B., Wang,; Y., Wang,; J., Wang, J.; Wang, W.; Watson, J. R.; Webb, R.; White, R.; Whitis, T. J.; Williams, Michael; Wolfs, F. L. H.; Woodford, S.; Woodward, David I.; Wright, C.; Xia, Q.; Xiang, X.; Xu, J.; Yeh, M.

doi:10.1103/physrevd.105.082004

Cited by 6 publications

(4 citation statements)

References 36 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The 37 Ar and 127 Xe initial rates are consistent with expectation from above-ground cosmogenic activation (see Refs. [12,58]) and the subsequent rates are consistent with exponential decay at the expected half-lives (see Ref. [12]).…”

Section: Discussionsupporting

confidence: 71%

“…Given the significant rate of ER backgrounds in the ER signal region of {S1c, log 10 S2c}, the inclusion of time potentially allows for increased sensitivity. Specifically, the rates of the 37 Ar and 127 Xe components are modeled as exponentially falling with their 35.0 d and 36.3 d half-lives, respectively [56][57][58]. The 37 Ar and 127 Xe initial rates are consistent with expectation from above-ground cosmogenic activation (see Refs.…”

Section: Discussionmentioning

confidence: 86%

See 1 more Smart Citation

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

Aalbers¹

2023

Phys. Rev. Lett.

Self Cite

221

View full text Add to dashboard Cite

The LUX-ZEPLIN (LZ) experiment is a dark matter detector centered on a dual-phase xenon time projection chamber. We report searches for new physics appearing through few-keV-scale electron recoils, using the experiment's first exposure of 60 live days and a fiducial mass of 5.5 t. The data are found to be consistent with a background-only hypothesis, and limits are set on models for new physics including solar axion electron coupling, solar neutrino magnetic moment and millicharge, and electron couplings to galactic axion-like particles and hidden photons. Similar limits are set on weakly interacting massive particle (WIMP) dark matter producing signals through ionized atomic states from the Migdal effect.

show abstract

Section: Discussionsupporting

confidence: 71%

Section: Discussionmentioning

confidence: 86%

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

Aalbers¹

2023

Phys. Rev. Lett.

Self Cite

221

View full text Add to dashboard Cite

show abstract

“…However, purification to very high levels has already been demonstrated in dark matter [63,96,136,137] and neutrinoless double-beta decay experiments [138]. Cosmogenically-produced 37 Ar decays away quickly [139], and purity levels achieved for 85 Kr are already sufficient for the next-generation detector discussed here. Further advantages of xenon are obtained through its high charge number Z, mass number A, and density; these allow for self-shielding of gamma-ray and neutron backgrounds, which will multiply-scatter, especially in the outer limits of the fiducial volume (FV).…”

Section: Xenon As a Detector Mediummentioning

confidence: 88%

“…Thus, the 137 Xe induced background strongly depends on the muon rate at the experimental site. Short-lived cosmogenic isotopes such as 37 Ar are of little concern for the anticipated experiment [139].…”

Section: Intrinsic Background Mitigationmentioning

confidence: 99%

A next-generation liquid xenon observatory for dark matter and neutrino physics

Aalbers

AbdusSalam

Abe

et al. 2022

J. Phys. G: Nucl. Part. Phys.

View full text Add to dashboard Cite

The nature of dark matter and properties of neutrinos are among the most pressing issues in contemporary particle physics. The dual-phase xenon time-projection chamber is the leading technology to cover the available parameter space for weakly interacting massive particles, while featuring extensive sensitivity to many alternative dark matter candidates. These detectors can also study neutrinos through neutrinoless double-beta decay and through a variety of astrophysical sources. A next-generation xenon-based detector will therefore be a true multi-purpose observatory to significantly advance particle physics, nuclear physics, astrophysics, solar physics, and cosmology. This review article presents the science cases for such a detector.

show abstract