Identification of radiopure titanium for the LZ dark matter experiment and future rare event searches

Akerib, D. S.; Akerlof, C.; Akimov, D.; Alsum, S.; Araújo, H. M.; Arnquist, I. J.; Arthurs, M.; Bai, X.; Bailey, A. J.; Balajthy, J.; Balashov, S.; Barry, M. J.; Belle, Jean Louis Van; Beltrame, P.; Benson, Theophilus; Bernard, E. P.; Bernstein, Adam; Biesiadzinski, T. P.; Boast, K. E.; Bolozdynya, A.; Boxer, B.; Bramante, R.; Brás, P.; Buckley, J. H.; Bugaev, V.; Bunker, R.; Burdin, S.; Busenitz, J.; Carels, C.; Carlsmith, D.; Carlson, Ben; Carmona-Benitez, M. C.; Chan, C.; Cherwinka, J. J.; Chiller, A. A.; Chiller, C.; Cottle, A.; Coughlen, R.; Craddock, W.; Currie, A.; Dahl, C. E.; Davison, T. J. R.; Dobi, A.; Dobson, J.; Druszkiewicz, E.; Edberg, T. K.; Edwards, W. R.; Emmet, W.; Faham, C.H.; Fiorucci, S.; Fruth, T.; Gaitskell, R. J.; Gantos, N. J.; Gehman, V. M.; Gerhard, R. M.; Ghag, C.; Gilchriese, M.; Gomber, B.; Hall, C.; Hans, S.; Hanzel, K.; Haselschwardt, S. J.; Hertel, S. A.; Hillbrand, Seth; Hjemfelt, C.; Hoff, M.; Holbrook, B.; Holtom, E.; Hoppe, E. W.; Hor, J. Y.K.; Horn, M.; Huang, Di; Hurteau, T. W.; Ignarra, C. M.; Jacobsen, R. G.; Ji, W.; Kaboth, A.; Kamdin, K.; Kazkaz, K.; Khaitan, D.; Khazov, A.; Хромов, А. В.; Konovalov, A. M.; Korolkova, E. V.; Koyuncu, M.; Kraus, H.; Krebs, H.; Kudryavtsev, V. A.; Kumpan, A.; Kyre, S.; Lee, C.; Lee, H.S.; Lee, J.; Leonard, D. S.; Leonard, R.; Lesko, K. T.; Lévy, C.; Liao, Fenglin; Lin, J.; Lindote, A.; Linehan, R.; Lippincott, W. H.; Liu, X.; Lopes, I.; Paredes, B. López; Lorenzon, W.; Luitz, S.; Majewski, P.; Manalaysay, A.; Manenti, L.; Mannino, R. L.; Markley, D.; Martin, Thierry; Marzioni, M. F.; McConnell, C. T.; McKinsey, D. N.; Mei, Dongming; Meng, Y.; Miller, E. H.; Mizrachi, E.; Möck, J.; Monzani, M. E.; Morad, J. A.; Mount, B. J.; Murphy, A. St. J.; Nehrkorn, C.; Nelson, H. N.; Neves, F.; Nikkel, J.; O'Dell, Joe; O’Sullivan, K.; Olcina, I.; Olevitch, M. A.; Oliver-Mallory, K. C.; Palladino, K. J.; Pease, E. K.; Piepke, A.; Powell, S.; Preece, R.; Pushkin, K.; Ratcliff, B. N.; Reichenbacher, J.; Reichhart, L.; Rhyne, C.; Richards, A.; Rodrigues, J. P.; Rose, H. J.; Rosero, R.; Rossiter, P.; Saba, J. S.; Sarychev, Michael; Schnee, R. W.; Schubnell, M.; Scovell, P. R.; Shaw, S.; Shutt, T.; Silva, C.; Skarpaas, K.; Skulski, W.; Solmaz, M.; Solovov, V.; Sørensen, P.; Sosnovtsev, V.; Stancu, I.; Stark, M.; Stephenson, S.; Stiegler, T.; Stifter, K.; Sumner, T. J.; Szydagis, M.; Taylor, D. J.; Taylor, WC; Temples, D.; Terman, P. A.; Thomas, Keenan; Thomson, J.; Tiedt, D. R.; Timalsina, M.; To, W. H.; Tomás, A.; Tope, T.; Tripathi, M.; Tvrznikova, L.; Va’vra, J.; Vacheret, A.; Grinten, M. G. D. van der; Verbus, J.R.; Vuosalo, C.; Waldron, W. L.; Wang, R.; Watson, R. A.; Webb, R.; Wei, Wenlu; While, M.; White, D.; Whitis, T. J.; Wisniewski, W. J.; Witherell, M. S.; Wolfs, F. L. H.; Woodward, David I.; Worm, S. D.; Xu, J.; Yeh, M.; Yin, Jun; Zhang, C.

doi:10.1016/j.astropartphys.2017.09.002

Cited by 39 publications

(34 citation statements)

References 27 publications

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“…1. The vacuum-insulated cryostat made from ultrapure titanium [10] holds 10 tonnes of LXe, including the LXe-TPC and its enveloping xenon skin veto. The cryostat is maintained at 175 K by a system of thermosyphons and is surrounded by a room-temperature liquid scintillator outer detector (OD).…”

Section: A Overviewmentioning

confidence: 99%

Projected WIMP sensitivity of the LUX-ZEPLIN dark matter experiment

Akerib¹,

Akerlof²,

Alsum³

et al. 2020

Phys. Rev. D

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311

362

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LUX-ZEPLIN (LZ) is a next-generation dark matter direct detection experiment that will operate 4850 feet underground at the Sanford Underground Research Facility (SURF) in Lead, South Dakota, USA. Using a two-phase xenon detector with an active mass of 7 tonnes, LZ will search primarily for low-energy interactions with weakly interacting massive particles (WIMPs), which are hypothesized to make up the dark matter in our galactic halo. In this paper, the projected WIMP sensitivity of LZ is presented based on the latest background estimates and simulations of the detector. For a 1000 live day run using a 5.6-tonne fiducial mass, LZ is projected to exclude at 90% confidence level spin-independent WIMP-nucleon cross sections above 1.4 × 10 −48 cm 2 for a 40 GeV=c 2 mass WIMP. Additionally, a 5σ discovery potential is projected, reaching cross sections below the exclusion limits of recent experiments. For spin-dependent WIMP-neutron(-proton) scattering, a sensitivity of 2.3 × 10 −43 cm 2 (7.1 × 10 −42 cm 2) for a 40 GeV=c 2 mass WIMP is expected. With underground installation well underway, LZ is on track for commissioning at SURF in 2020.

show abstract

Section: A Overviewmentioning

confidence: 99%

Projected WIMP sensitivity of the LUX-ZEPLIN dark matter experiment

Akerib¹,

Akerlof²,

Alsum³

et al. 2020

Phys. Rev. D

Self Cite

311

362

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show abstract

“…Materials that give measurable lines in Wilton will generally be of too high activity for use in low-background experiments and, as such are not screened in our more sensitive detectors. Since 2015, BUGS has supported primarily the LUX-ZEPLIN 1 (LZ) construction material radio-assay campaign [12,13,14], as well as performing assays for the SuperNEMO 0νββ experiment [15] and the SuperKamiokande experiment [16]. The current capacity of BUGS allows for ∼100 sample assays per year with some samples assayed in a matter of days and others requiring several weeks to reach the required sensitivity.…”

Section: Boulby Underground Germanium Suite (Bugs)mentioning

confidence: 99%

Low-background gamma spectroscopy at the Boulby Underground Laboratory

Scovell

Meehan²,

Araújo

et al. 2018

Astroparticle Physics

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The Boulby Underground Germanium Suite (BUGS) comprises three low-background, high-purity germanium detectors operating in the Boulby Underground Laboratory, located 1.1 km underground in the north-east of England, UK. BUGS utilises three types of detector to facilitate a high-sensitivity, high-throughput radio-assay programme to support the development of rare-event search experiments. A Broad Energy Germanium (BEGe) detector delivers sensitivity to low-energy gamma-rays such as those emitted by 210 Pb and 234 Th. A Small Anode Germanium (SAGe) well-type detector is employed for efficient screening of small samples. Finally, a standard p-type coaxial detector provides fast screening of standard samples. This paper presents the steps used to characterise the performance of these detectors for a variety of sample geometries, including the corrections applied to account for cascade summing effects. For low-density materials, BUGS is able to radio-assay to specific activities down to 3.6 mBq kg −1 for 234 Th and 6.6 mBq kg −1 for 210 Pb both of which have uncovered some significant equilibrium breaks in the 238 U chain. In denser materials, where gamma-ray self-absorption increases, sensitivity is demonstrated to specific activities of 0.9 mBq kg −1 for 226 Ra, 1.1 mBq kg −1 for 228 Ra, 0.3 mBq kg −1 for 224 Ra, and 8.6 mBq kg −1 for 40 K with all upper limits at a 90% confidence level. These meet the requirements of most screening campaigns presently under way for rare-event search experiments, such as the LUX-ZEPLIN (LZ) dark matter experiment. We also highlight the ability of the BEGe detector to probe the X-ray fluorescence region which can be important to identify the presence of radioisotopes associated with neutron production; this is of particular relevance in experiments sensitive to nuclear recoils.

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“…In the frame of the LUX experiment, radiopurity of different titanium samples was analyzed 117,118 and the activity of cosmogenic 46 Sc was quantified, ranging from 0.2 to 23 mBq/kg. Other scandium isotopes with shorter half-lives were also observed but are not relevant.…”

Section: Titaniummentioning

confidence: 99%

Cosmogenic activation of materials

Cebrián

2017

Int. J. Mod. Phys. A

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Experiments looking for rare events like the direct detection of dark matter particles, neutrino interactions or the nuclear double beta decay are operated deep underground to suppress the effect of cosmic rays. But the production of radioactive isotopes in materials due to previous exposure to cosmic rays is an hazard when ultra-low background conditions are required. In this context, the generation of long-lived products by cosmic nucleons has been studied for many detector media and for other materials commonly used. Here, the main results obtained on the quantification of activation yields on the Earth's surface will be summarized, considering both measurements and calculations following different approaches. The isotope production cross sections and the cosmic ray spectrum are the two main ingredients when calculating this cosmogenic activation; the different alternatives for implementing them will be discussed. Activation that can take place deep underground mainly due to cosmic muons will be briefly commented too. Presently, the experimental results for the cosmogenic production of radioisotopes are scarce and discrepancies between different calculations are important in many cases, but the increasing interest on this background source which is becoming more and more relevant can help to change this situation.

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Identification of radiopure titanium for the LZ dark matter experiment and future rare event searches

Cited by 39 publications

References 27 publications

Projected WIMP sensitivity of the LUX-ZEPLIN dark matter experiment

Projected WIMP sensitivity of the LUX-ZEPLIN dark matter experiment

Low-background gamma spectroscopy at the Boulby Underground Laboratory

Cosmogenic activation of materials

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