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@inproceedings{Malling:2011,
author = {Malling, DC and Chapman, JJ and Faham, CH and Fiorucci, S and Gaitskell, RJ and Pangilinan, M and Verbus, JR and Akerib, DS and Bradley, A and Carmona-Benitez, MC and Clark, K and Coffey, T and Dragowsky, M and Gibson, KR and Lee, C and Phelps, P and Shutt, T and Araújo, HM and Currie, A and Sumner, TJ and Bai, X and Hanhardt, M and Bedikian, S and Bernard, E and Cahn, SB and Kastens, L and Larsen, N and Lyashenko, A and McKinsey, DN and Nikkel, JA and Bernstein, A and Carr, D and Dazeley, S and Kazkaz, K and Sorensen, P and Classen, T and Holbrook, B and Lander, R and Mock, J and Svoboda, R and Sweany, M and Szydagis, M and Thomson, J and Tripathi, M and Walsh, N and Woods, M and de, Viveiros L and Lindote, A and Lopes, MI and Neves, F and Silva, C and Solovov, V and Druszkiewicz, E and Skulski, W and Wolfs, FLH and Hall, C and Leonard, D and Ihm, M and Jacobsen, RG and Lesko, K and Majewski, P and Mannino, R and Stiegler, T and Webb, R and White, JT and Mei, DM and Spaans, J a},
title = {After LUX: The LZ program},
year = {2011}
}
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TY  - CPAPER
AB  - The LZ program consists of two stages of direct dark matter searches using liquid Xe detectors. The first stage will be a 1.5-3 tonne detector, while the last stage will be a 20 tonne detector. Both devices will benefit tremendously from research and development performed for the LUX experiment, a 350 kg liquid Xe dark matter detector currently operating at the Sanford Underground Laboratory. In particular, the technology used for cryogenics and electrical feedthroughs, circulation and purification, low-background materials and shielding techniques, electronics, calibrations, and automated control and recovery systems are all directly scalable from LUX to the LZ detectors. Extensive searches for potential background sources have been performed, with an emphasis on previously undiscovered background sources that may have a significant impact on tonne-scale detectors. The LZ detectors will probe spin-independent interaction cross sections as low as 5 × 10-<sup>49</sup> cm<sup>2</sup> for 100 GeV WIMPs, which represents the ultimate limit for dark matter detection with liquid xenon technology.
AU  - Malling,DC
AU  - Chapman,JJ
AU  - Faham,CH
AU  - Fiorucci,S
AU  - Gaitskell,RJ
AU  - Pangilinan,M
AU  - Verbus,JR
AU  - Akerib,DS
AU  - Bradley,A
AU  - Carmona-Benitez,MC
AU  - Clark,K
AU  - Coffey,T
AU  - Dragowsky,M
AU  - Gibson,KR
AU  - Lee,C
AU  - Phelps,P
AU  - Shutt,T
AU  - Araújo,HM
AU  - Currie,A
AU  - Sumner,TJ
AU  - Bai,X
AU  - Hanhardt,M
AU  - Bedikian,S
AU  - Bernard,E
AU  - Cahn,SB
AU  - Kastens,L
AU  - Larsen,N
AU  - Lyashenko,A
AU  - McKinsey,DN
AU  - Nikkel,JA
AU  - Bernstein,A
AU  - Carr,D
AU  - Dazeley,S
AU  - Kazkaz,K
AU  - Sorensen,P
AU  - Classen,T
AU  - Holbrook,B
AU  - Lander,R
AU  - Mock,J
AU  - Svoboda,R
AU  - Sweany,M
AU  - Szydagis,M
AU  - Thomson,J
AU  - Tripathi,M
AU  - Walsh,N
AU  - Woods,M
AU  - de,Viveiros L
AU  - Lindote,A
AU  - Lopes,MI
AU  - Neves,F
AU  - Silva,C
AU  - Solovov,V
AU  - Druszkiewicz,E
AU  - Skulski,W
AU  - Wolfs,FLH
AU  - Hall,C
AU  - Leonard,D
AU  - Ihm,M
AU  - Jacobsen,RG
AU  - Lesko,K
AU  - Majewski,P
AU  - Mannino,R
AU  - Stiegler,T
AU  - Webb,R
AU  - White,JT
AU  - Mei,DM
AU  - Spaans,J
AU  - Zhang,C
AU  - Morii,M
AU  - Wlasenko,M
AU  - Murphy,ASJ
AU  - Reichhart,L
AU  - Nelson,H
PY  - 2011///
TI  - After LUX: The LZ program
ER  -
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