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Projected WIMP sensitivity of the LUX-ZEPLIN (LZ) dark matter experiment | | D.S. Akerib
; C.W. Akerlof
; S.K. Alsum
; H.M. Araújo
; M. Arthurs
; X. Bai
; A.J. Bailey
; J. Balajthy
; S. Balashov
; D. Bauer
; J. Belle
; P. Beltrame
; T. Benson
; E.P. Bernard
; T.P. Biesiadzinski
; K.E. Boast
; B. Boxer
; P. Brás
; J.H. Buckley
; V.V. Bugaev
; S. Burdin
; J.K. Busenitz
; C. Carels
; D.L. Carlsmith
; B. Carlson
; M.C. Carmona-Benitez
; C. Chan
; J.J. Cherwinka
; A. Cole
; A. Cottle
; W.W. Craddock
; A. Currie
; J.E. Cutter
; C.E. Dahl
; L. de Viveiros
; A. Dobi
; J.E.Y. Dobson
; E. Druszkiewicz
; T.K. Edberg
; W.R. Edwards
; A. Fan
; S. Fayer
; S. Fiorucci
; T. Fruth
; R.J. Gaitskell
; J. Genovesi
; C. Ghag
; M.G.D. Gilchriese
; M.G.D.van der Grinten
; C.R. Hall
; S. Hans
; K. Hanzel
; S.J. Haselschwardt
; S.A. Hertel
; S. Hillbrand
; C. Hjemfelt
; M.D. Hoff
; J.Y-K. Hor
; D.Q. Huang
; C.M. Ignarra
; W. Ji
; A.C. Kaboth
; K. Kamdin
; J. Keefner
; D. Khaitan
; A. Khazov
; Y.D. Kim
; C.D. Kocher
; E.V. Korolkova
; H. Kraus
; H.J. Krebs
; L. Kreczko
; B. Krikler
; V.A. Kudryavtsev
; S. Kyre
; J. Lee
; B.G. Lenardo
; D.S. Leonard
; K.T. Lesko
; C. Levy
; J. Li
; J. Liao
; F.-T. Liao
; J. Lin
; A. Lindote
; R. Linehan
; W.H. Lippincott
; X. Liu
; M.I. Lopes
; B. López Paredes
; W. Lorenzon
; S. Luitz
; J.M. Lyle
; P. Majewski
; A. Manalaysay
; R.L. Mannino
; C. Maupin
; D.N. McKinsey
; Y. Meng
; E.H. Miller
; J. Mock
; M.E. Monzani
; J.A. Morad
; E. Morrison
; B.J. Mount
; A.St.J. Murphy
; H.N. Nelson
; F. Neves
; J. Nikoleyczik
; K. O'Sullivan
; I. Olcina
; M.A. Olevitch
; K.C. Oliver-Mallory
; K.J. Palladino
; S.J. Patton
; E.K. Pease
; B. Penning
; A. Piepke
; S. Powell
; R.M. Preece
; K. Pushkin
; B.N. Ratcliff
; J. Reichenbacher
; C.A. Rhyne
; A. Richards
; J.P. Rodrigues
; R. Rosero
; P. Rossiter
; J.S. Saba
; M. Sarychev
; R.W. Schnee
; M. Schubnell
; P.R. Scovell
; S. Shaw
; T.A. Shutt
; J.J. Silk
; C. Silva
; K. Skarpaas
; W. Skulski
; M. Solmaz
; V.N. Solovov
; P. Sorensen
; I. Stancu
; M.R. Stark
; T.M. Stiegler
; K. Stifter
; M. Szydagis
; W.C. Taylor
; R. Taylor
; D.J. Taylor
; D. Temples
; P.A. Terman
; K.J. Thomas
; M. Timalsina
; W.H. To
; A. Tomás
; T.E. Tope
; M. Tripathi
; C.E. Tull
; L. Tvrznikova
; U. Utku
; J. Va'vra
; A. Vacheret
; J.R. Verbus
; E. Voirin
; W.L. Waldron
; J.R. Watson
; R.C. Webb
; D.T. White
; T.J. Whitis
; W.J. Wisniewski
; M.S. Witherell
; F.L.H. Wolfs
; D. Woodward
; S.D. Worm
; M. Yeh
; J. Yin
; I. Young
; | | Date: |
Fri, 16 Feb 2018 17:26:57 GMT (1824kb,D) | | Abstract: | 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 $1.6 imes 10^{-48}$
cm$^{2}$ for a 40 $mathrm{GeV}/c^{2}$ mass WIMP. Additionally, a $5sigma$
discovery potential is projected reaching cross sections below the existing and
projected exclusion limits of similar experiments that are currently operating.
For spin-dependent WIMP-neutron(-proton) scattering, a sensitivity of $2.7
imes 10^{-43}$ cm$^{2}$ ($8.1 imes 10^{-42}$ cm$^{2}$) for a 40
$mathrm{GeV}/c^{2}$ mass WIMP is expected. With construction well underway, LZ
is on track for underground installation at SURF in 2019 and will start
collecting data in 2020. | | Source: | arXiv, 1802.6039 | | Services: | Forum | Review | PDF | Favorites | |
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