Projected WIMP sensitivity of the LUX-ZEPLIN (LZ) dark matter experiment
Creators: name: Akerib, D. S.
name: Akerlof, C. W.
name: Alsum, S. K.
name: Araújo, H. M.
name: Arthurs, M.
name: Bai, X.
name: Bailey, A. J.
name: Balajthy, J.
name: Balashov, S.
name: Bauer, D.
name: Belle, J.
name: Beltrame, P.
name: Benson, T.
name: Bernard, E. P.
name: Biesiadzinski, T. P.
name: Boast, K. E.
name: Boxer, B.
name: Brás, P.
name: Buckley, J. H.
name: Bugaev, V. V.
name: Burdin, S.
name: Busenitz, J. K.
name: Carels, C.
name: Carlsmith, D. L.
name: Carlson, B.
name: Carmona-Benitez, M. C.
name: Chan, C.
name: Cherwinka, J. J.
name: Cole, A.
name: Cottle, A.
name: Craddock, W. W.
name: Currie, A.
name: Cutter, J. E.
name: Dahl, C. E.
name: de Viveiros, L.
name: Dobi, A.
name: Dobson, J. E. Y.
name: Druszkiewicz, E.
name: Edberg, T. K.
name: Edwards, W. R.
name: Fan, A.
name: Fayer, S.
name: Fiorucci, S.
name: Fruth, T.
name: Gaitskell, R. J.
name: Genovesi, J.
name: Ghag, C.
name: Gilchriese, M. G. D.
name: van der Grinten, M. G. D.
name: Hall, C. R.
name: Hans, S.
name: Hanzel, K.
name: Haselschwardt, S. J.
name: Hertel, S. A.
name: Hillbrand, S.
name: Hjemfelt, C.
name: Hoff, M. D.
name: Hor, J. Y-K.
name: Huang, D. Q.
name: Ignarra, C. M.
name: Ji, W.
name: Kaboth, A. C.
name: Kamdin, K.
name: Keefner, J.
name: Khaitan, D.
name: Khazov, A.
name: Kim, Y. D.
name: Kocher, C. D.
name: Korolkova, E. V.
name: Kraus, H.
name: Krebs, H. J.
name: Kreczko, L.
name: Krikler, B.
name: Kudryavtsev, V. A.
name: Kyre, S.
name: Lee, J.
name: Lenardo, B. G.
name: Leonard, D. S.
name: Lesko, K. T.
name: Levy, C.
name: Li, J.
name: Liao, J.
name: Liao, F. -T.
name: Lin, J.
name: Lindote, A.
name: Linehan, R.
name: Lippincott, W. H.
name: Liu, X.
name: Lopes, M. I.
name: Paredes, B. López
name: Lorenzon, W.
name: Luitz, S.
name: Lyle, J. M.
name: Majewski, P.
name: Manalaysay, A.
name: Mannino, R. L.
name: Maupin, C.
name: McKinsey, D. N.
name: Meng, Y.
name: Miller, E. H.
name: Mock, J.
name: Monzani, M. E.
name: Morad, J. A.
name: Morrison, E.
name: Mount, B. J.
name: Murphy, A. St. J.
name: Nelson, H. N.
name: Neves, F.
name: Nikoleyczik, J.
name: O'Sullivan, K.
name: Olcina, I.
name: Olevitch, M. A.
name: Oliver-Mallory, K. C.
name: Palladino, K. J.
name: Patton, S. J.
name: Pease, E. K.
name: Penning, B.
name: Piepke, A.
name: Powell, S.
name: Preece, R. M.
name: Pushkin, K.
name: Ratcliff, B. N.
name: Reichenbacher, J.
name: Rhyne, C. A.
name: Richards, A.
name: Rodrigues, J. P.
name: Rosero, R.
name: Rossiter, P.
name: Saba, J. S.
name: Sarychev, M.
name: Schnee, R. W.
name: Schubnell, M.
name: Scovell, P. R.
name: Shaw, S.
name: Shutt, T. A.
name: Silk, J. J.
name: Silva, C.
name: Skarpaas, K.
name: Skulski, W.
name: Solmaz, M.
name: Solovov, V. N.
name: Sorensen, P.
name: Stancu, I.
name: Stark, M. R.
name: Stiegler, T. M.
name: Stifter, K.
name: Szydagis, M.
name: Taylor, W. C.
name: Taylor, R.
name: Taylor, D. J.
name: Temples, D.
name: Terman, P. A.
name: Thomas, K. J.
name: Timalsina, M.
name: To, W. H.
name: Tomás, A.
name: Tope, T. E.
name: Tripathi, M.
name: Tull, C. E.
name: Tvrznikova, L.
name: Utku, U.
name: Va'vra, J.
name: Vacheret, A.
name: Verbus, J. R.
name: Voirin, E.
name: Waldron, W. L.
name: Watson, J. R.
name: Webb, R. C.
name: White, D. T.
name: Whitis, T. J.
name: Wisniewski, W. J.
name: Witherell, M. S.
name: Wolfs, F. L. H.
name: Woodward, D.
name: Worm, S. D.
name: Yeh, M.
name: Yin, J.
name: Young, I.
Publisher: name: arXiv
Year: 2018
Subjects: subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: High Energy Physics - Experiment (hep-ex)
subject: Instrumentation and Detectors (physics.ins-det)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: 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 $1.4 \times 10^{-48}$~cm$^{2}$ for a 40~$\mathrm{GeV}/c^{2}$ 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 $2.3 \times 10^{-43}$~cm$^{2}$ ($7.1 \times 10^{-42}$~cm$^{2}$) for a 40~$\mathrm{GeV}/c^{2}$ mass WIMP is expected. With underground installation well underway, LZ is on track for commissioning at SURF in 2020.
description: 14 pages, 11 figures