After LUX: The LZ Program-猫眼课题宝

DOI：

发表时间：

2011-10

期刊：

arXiv: Instrumentation and Methods for Astrophysics

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其他

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作者：

D. Malling;D. Akerib;H. Araújo;X. Bai;S. Bedikian;E. Bernard;A. Bernstein;A. Bradley;S. Cahn;M. Carmona-Benitez;D. Carr;J. Chapman;K. Clark;T. Classen;T. Coffey;A. Curioni;A. Currie;S. Dazeley;L. D. Viveiros;M. Dragowsky;E. Druszkiewicz;C. Faham;S. Fiorucci;R. Gaitskell;K. Gibson;C. Hall;M. Hanhardt;B. Holbrook;M. Ihm;R. Jacobsen;L. Kastens;K. Kazkaz;R. Lander;N. Larsen;C. Lee;D. Leonard;K. Lesko;A. Lindote;M. Lopes;A. Lyashenko;P. Majewski;R. Mannino;D. McKinsey;D. Mei;J. Mock;M. Morii;A. Murphy;H. Nelson;F. Neves;J. Nikkel;M. Pangilinan;P. Phelps;L. Reichhart;T. Shutt;C. Silva;W. Skulski;V. Solovov;P. Sorensen;J. Spaans;T. Stiegler;T. Sumner;R. Svoboda;M. Sweany;M. Szydagis;J. Thomson;M. Tripathi;J. Verbus;N. Walsh;R. Webb;J. White;M. Własenko;F. Wolfs;M. Woods;C. Zhang

作者：Malling，DC；阿克里布，DS；阿劳霍，HM；白X；贝迪基安，S；伯纳德，E；伯恩斯坦，A；布拉德利，A；卡恩，SB；卡莫纳-贝尼特斯，MC；卡尔，D；查普曼，JJ；克拉克，K；克拉森，T；科菲，T；库里奥尼，A；库里，A；达泽利，S；维韦罗斯，L de；德拉戈夫斯基，M；德鲁什凯维奇，E；法厄姆，CH；菲奥鲁奇，S；盖茨克尔，RJ；吉布森，KR；霍尔，C；汉哈特，M；霍尔布鲁克，B；嗯，M；雅各布森，RG；卡斯滕斯，L；卡兹卡兹，K；兰德，R；拉森，N；李，C；伦纳德，D；莱斯科，K；林多特，A；密歇根州洛佩斯；利亚申科，A；马耶夫斯基，P；曼尼诺，R；麦肯锡，DN；梅，D-M；莫克，J；森井，M；墨菲，A St J；纳尔逊，H；内维斯，F；尼克尔，JA；邦吉利南，M；菲尔普斯，P；赖克哈特，L；舒特，T；席尔瓦，C；斯库尔斯基，W；索洛沃夫，V；索伦森，P；斯潘斯，J；斯蒂格勒，T；萨姆纳，TJ；斯沃博达，R；斯威尼，M；西达吉斯，M；汤姆森，J；特里帕蒂，M；维布斯，JR；沃尔什，N；韦伯，R；白色，JT；弗拉森科，M；沃尔夫斯，FLH；伍兹，M；张C |摘要：LZ 计划包括使用液态 Xe 探测器进行直接暗物质搜索的两个阶段。第一级将是一个 1.5-3 吨探测器，而最后一级将是一个 20 吨探测器。这两款设备都将从 LUX 实验的研究和开发中受益匪浅，LUX 实验是目前在桑福德地下实验室运行的 350 公斤液态 Xe 暗物质探测器。特别是，用于低温和电馈通、循环和净化、低本底材料和屏蔽技术、电子、校准以及自动控制和恢复系统的技术都可以直接从 LUX 扩展到 LZ 探测器。已经对潜在的背景源进行了广泛的搜索，重点是先前未发现的可能对吨级探测器产生重大影响的背景源。 LZ 探测器将探测 100 GeV WIMP 的低至 5E-49 cm2 的自旋无关相互作用截面，这代表了液氙技术暗物质探测的最终极限。

Author(s): Malling, DC; Akerib, DS; Araujo, HM; Bai, X; Bedikian, S; Bernard, E; Bernstein, A; Bradley, A; Cahn, SB; Carmona-Benitez, MC; Carr, D; Chapman, JJ; Clark, K; Classen, T; Coffey, T; Curioni, A; Currie, A; Dazeley, S; Viveiros, L de; Dragowsky, M; Druszkiewicz, E; Faham, CH; Fiorucci, S; Gaitskell, RJ; Gibson, KR; Hall, C; Hanhardt, M; Holbrook, B; Ihm, M; Jacobsen, RG; Kastens, L; Kazkaz, K; Lander, R; Larsen, N; Lee, C; Leonard, D; Lesko, K; Lindote, A; Lopes, MI; Lyashenko, A; Majewski, P; Mannino, R; McKinsey, DN; Mei, D-M; Mock, J; Morii, M; Murphy, A St J; Nelson, H; Neves, F; Nikkel, JA; Pangilinan, M; Phelps, P; Reichhart, L; Shutt, T; Silva, C; Skulski, W; Solovov, V; Sorensen, P; Spaans, J; Stiegler, T; Sumner, TJ; Svoboda, R; Sweany, M; Szydagis, M; Thomson, J; Tripathi, M; Verbus, JR; Walsh, N; Webb, R; White, JT; Wlasenko, M; Wolfs, FLH; Woods, M; Zhang, C | Abstract: 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 5E-49 cm2 for 100 GeV WIMPs, which represents the ultimate limit for dark matter detection with liquid xenon technology.

After LUX: The LZ Program

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