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@article{Akerib:2020:10.1103/PhysRevD.101.052002,
author = {Akerib, DS and Akerlof, CW and Alsum, SK and Araujo, HM and Arthurs, M and Bai, X and Bailey, AJ and Balajthy, J and Balashov, S and Bauer, D and Belle, J and Beltrame, P and Benson, T and Bernard, EP and Biesiadzinski, TP and Boast, KE and Boxer, B and Bras, P and Buckley, JH and Bugaev, VV and Burdin, S and Busenitz, JK and Carels, C and Carlsmith, DL and Carlson, B and Carmona-Benitez, MC and Chan, C and Cherwinka, JJ and Cole, A and Cottle, A and Craddock, WW and Currie, A and Cutter, JE and Dahl, CE and de, Viveiros L and Dobi, A and Dobson, JEY and Druszkiewicz, E and Edberg, TK and Edwards, WR and Fan, A and Fayer, S and Fiorucci, S and Fruth, T and Gaitskell, RJ and Genovesi, J and Ghag, C and Gilchriese, MGD and van, der Grinten MGD and Hall, CR and Hans, S and Hanzel, K and Haselschwardt, SJ and Hertel, SA and Hillbrand, S and Hjemfelt, C and Hoff, MD and Hor, JY-K and Huang, DQ and Ignarra, CM and Ji, W and Kaboth, AC and Kamdin, K and Keefner, J and Khaitan, D and Khazov, A},
doi = {10.1103/PhysRevD.101.052002},
journal = {Physical Review D: Particles, Fields, Gravitation and Cosmology},
pages = {1--17},
title = {Projected WIMP sensitivity of the LUX-ZEPLIN dark matter experiment},
url = {http://dx.doi.org/10.1103/PhysRevD.101.052002},
volume = {101},
year = {2020}
}

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TY  - JOUR
AB  - 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  cm2 for a 40  GeV/c2 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  cm2 (7.1×10−42  cm2) for a 40  GeV/c2 mass WIMP is expected. With underground installation well underway, LZ is on track for commissioning at SURF in 2020.
AU  - Akerib,DS
AU  - Akerlof,CW
AU  - Alsum,SK
AU  - Araujo,HM
AU  - Arthurs,M
AU  - Bai,X
AU  - Bailey,AJ
AU  - Balajthy,J
AU  - Balashov,S
AU  - Bauer,D
AU  - Belle,J
AU  - Beltrame,P
AU  - Benson,T
AU  - Bernard,EP
AU  - Biesiadzinski,TP
AU  - Boast,KE
AU  - Boxer,B
AU  - Bras,P
AU  - Buckley,JH
AU  - Bugaev,VV
AU  - Burdin,S
AU  - Busenitz,JK
AU  - Carels,C
AU  - Carlsmith,DL
AU  - Carlson,B
AU  - Carmona-Benitez,MC
AU  - Chan,C
AU  - Cherwinka,JJ
AU  - Cole,A
AU  - Cottle,A
AU  - Craddock,WW
AU  - Currie,A
AU  - Cutter,JE
AU  - Dahl,CE
AU  - de,Viveiros L
AU  - Dobi,A
AU  - Dobson,JEY
AU  - Druszkiewicz,E
AU  - Edberg,TK
AU  - Edwards,WR
AU  - Fan,A
AU  - Fayer,S
AU  - Fiorucci,S
AU  - Fruth,T
AU  - Gaitskell,RJ
AU  - Genovesi,J
AU  - Ghag,C
AU  - Gilchriese,MGD
AU  - van,der Grinten MGD
AU  - Hall,CR
AU  - Hans,S
AU  - Hanzel,K
AU  - Haselschwardt,SJ
AU  - Hertel,SA
AU  - Hillbrand,S
AU  - Hjemfelt,C
AU  - Hoff,MD
AU  - Hor,JY-K
AU  - Huang,DQ
AU  - Ignarra,CM
AU  - Ji,W
AU  - Kaboth,AC
AU  - Kamdin,K
AU  - Keefner,J
AU  - Khaitan,D
AU  - Khazov,A
AU  - Kim,YD
AU  - Kocher,CD
AU  - Korolkova,E
AU  - Kraus,H
AU  - Krebs,HJ
AU  - Kreczko,L
AU  - Krikler,B
AU  - Kudryavtsev,VA
AU  - Kyre,S
AU  - Lee,J
AU  - Lenardo,BG
AU  - Leonard,DS
AU  - Lesko,KT
AU  - Levy,C
AU  - Li,J
AU  - Liao,J
AU  - Liao,F-T
AU  - Lin,J
AU  - Lindote,A
AU  - Linehan,R
AU  - Lippincott,WH
AU  - Liu,X
AU  - Lopes,M
AU  - Paredes,BL
AU  - Lorenzon,W
AU  - Luitz,S
AU  - Lyle,JM
AU  - Majewski,P
AU  - Manalaysay,A
AU  - Mannino,RL
AU  - Maupin,C
AU  - McKinsey,DN
AU  - Meng,Y
AU  - Miller,EH
AU  - Mock,J
AU  - Monzani,ME
AU  - Morad,JA
AU  - Morrison,E
AU  - Mount,BJ
AU  - Murphy,ASJ
AU  - Nelson,HN
AU  - Neves,F
AU  - Nikoleyczik,J
AU  - O'Sullivan,K
AU  - Olcina,I
AU  - Olevitch,MA
AU  - Oliver-Mallory,KC
AU  - Palladino,KJ
AU  - Patton,SJ
AU  - Pease,EK
AU  - Penning,B
AU  - Piepke,A
AU  - Powell,S
AU  - Preece,RM
AU  - Pushkin,K
AU  - Ratcliff,BN
AU  - Reichenbacher,J
AU  - Rhyne,CA
AU  - Richards,A
AU  - Rodrigues,JP
AU  - Rosero,R
AU  - Rossiter,P
AU  - Saba,JS
AU  - Sarychev,M
AU  - Schnee,RW
AU  - Schubnell,M
AU  - Scovell,PR
AU  - Shaw,S
AU  - Shutt,TA
AU  - Silk,JJ
AU  - Silva,C
AU  - Skarpaas,K
AU  - Skulski,W
AU  - Solmaz,M
AU  - Solovov,VN
AU  - Sorensen,P
AU  - Stancu,I
AU  - Stark,MR
AU  - Stiegler,TM
AU  - Stifter,K
AU  - Szydagis,M
AU  - Taylor,WC
AU  - Taylor,R
AU  - Taylor,DJ
AU  - Temples,D
AU  - Terman,PA
AU  - Thomas,KJ
AU  - Timalsina,M
AU  - To,WH
AU  - Tomas,A
AU  - Tope,TE
AU  - Tripathi,M
AU  - Tull,CE
AU  - Tvrznikova,L
AU  - Utku,U
AU  - Vavra,J
AU  - Vacheret,A
AU  - Verbus,JR
AU  - Voirin,E
AU  - Waldron,WL
AU  - Watson,JR
AU  - Webb,RC
AU  - White,DT
AU  - Whitis,TJ
AU  - Wisniewski,WJ
AU  - Witherell,MS
AU  - Wolfs,FLH
AU  - Woodward,D
AU  - Worm,SD
AU  - Yeh,M
AU  - Yin,J
AU  - Young,I
DO  - 10.1103/PhysRevD.101.052002
EP  - 17
PY  - 2020///
SN  - 1550-2368
SP  - 1
TI  - Projected WIMP sensitivity of the LUX-ZEPLIN dark matter experiment
T2  - Physical Review D: Particles, Fields, Gravitation and Cosmology
UR  - http://dx.doi.org/10.1103/PhysRevD.101.052002
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000517963200002&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - https://journals.aps.org/prd/abstract/10.1103/PhysRevD.101.052002
UR  - http://hdl.handle.net/10044/1/77619
VL  - 101
ER  -

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