Tritium calibration of the LUX dark matter experiment

Tritium calibration of the LUX dark matter experiment
复制标题

DOI：
10.1103/physrevd.93.072009
复制
发表时间：
2015-12
期刊：
Physical Review D
影响因子：
5
通讯作者：
D. Akerib;H. Araújo;X. Bai;A. Bailey;J. Balajthy;P. Beltrame;E. Bernard;A. Bernstein;T. Biesiadzinski;E. Boulton;A. Bradley;R. Bramante;S. Cahn;M. Carmona-Benitez;C. Chan;J. J. Chapman-J. ;A. A. Chiller-A.;C. Chiller;A. Currie;J. Cutter;T. Davison;L. de Viveiros;A. Dobi;J. Dobson;E. Druszkiewicz;B. Edwards;C. Faham;S. Fiorucci;R. Gaitskell;V. Gehman;C. Ghag;K. Gibson;M. Gilchriese;C. Hall;M. Hanhardt;S. Haselschwardt;S. A. Hertel;D. P. Hogan;M. Horn;D. Huang;C. Ignarra;M. Ihm;R. Jacobsen;W. Ji;K. Kazkaz;D. Khaitan;R. Knoche;N. Larsen;C. Lee;B. Lenardo;K. Lesko;A. Lindote;M. Lopes;D. Malling;A. Manalaysay;R. Mannino;M. F. Marzioni;D. Mckinsey;D. Mei;J. Mock;M. Moongweluwan;J. Morad;A. Murphy;C. Nehrkorn;H. Nelson;F. Neves;K. OSullivan;K. Oliver-Mallory;R. Ott;K. Palladino;M. Pangilinan;E. K. Pease;P. Phelps;L. Reichhart;C. Rhyne;S. Shaw;T. Shutt;C. Silva;V. Solovov;P. Sorensen;S. Stephenson;T. Sumner;M. Szydagis;D. Taylor;W. Taylor;B. Tennyson;P. Terman;D. Tiedt;W. To;M. Tripathi;L. Tvrznikova;S. Uvarov;J. Verbus;R. Webb;J. White;T. J. Whitis;M. Witherell;F. Wolfs;S. Young;C. Zhang
D. Akerib;H. Araújo;X. Bai;A. Bailey;J. Balajthy;P. Beltrame;E. Bernard;A. Bernstein;T. Biesiadzinski;E. Boulton;A. Bradley;R. Bramante;S. Cahn;M. Carmona-Benitez;C. Chan;J. J. Chapman-J. ;A. A. Chiller-A.;C. Chiller;A. Currie;J. Cutter;T. Davison;L. de Viveiros;A. Dobi;J. Dobson;E. Druszkiewicz;B. Edwards;C. Faham;S. Fiorucci;R. Gaitskell;V. Gehman;C. Ghag;K. Gibson;M. Gilchriese;C. Hall;M. Hanhardt;S. Haselschwardt;S. A. Hertel;D. P. Hogan;M. Horn;D. Huang;C. Ignarra;M. Ihm;R. Jacobsen;W. Ji;K. Kazkaz;D. Khaitan;R. Knoche;N. Larsen;C. Lee;B. Lenardo;K. Lesko;A. Lindote;M. Lopes;D. Malling;A. Manalaysay;R. Mannino;M. F. Marzioni;D. Mckinsey;D. Mei;J. Mock;M. Moongweluwan;J. Morad;A. Murphy;C. Nehrkorn;H. Nelson;F. Neves;K. OSullivan;K. Oliver-Mallory;R. Ott;K. Palladino;M. Pangilinan;E. K. Pease;P. Phelps;L. Reichhart;C. Rhyne;S. Shaw;T. Shutt;C. Silva;V. Solovov;P. Sorensen;S. Stephenson;T. Sumner;M. Szydagis;D. Taylor;W. Taylor;B. Tennyson;P. Terman;D. Tiedt;W. To;M. Tripathi;L. Tvrznikova;S. Uvarov;J. Verbus;R. Webb;J. White;T. J. Whitis;M. Witherell;F. Wolfs;S. Young;C. Zhang
中科院分区：
物理与天体物理2区
文献类型：
--
作者：
D. Akerib;H. Araújo;X. Bai;A. Bailey;J. Balajthy;P. Beltrame;E. Bernard;A. Bernstein;T. Biesiadzinski;E. Boulton;A. Bradley;R. Bramante;S. Cahn;M. Carmona-Benitez;C. Chan;J. J. Chapman-J. ;A. A. Chiller-A.;C. Chiller;A. Currie;J. Cutter;T. Davison;L. de Viveiros;A. Dobi;J. Dobson;E. Druszkiewicz;B. Edwards;C. Faham;S. Fiorucci;R. Gaitskell;V. Gehman;C. Ghag;K. Gibson;M. Gilchriese;C. Hall;M. Hanhardt;S. Haselschwardt;S. A. Hertel;D. P. Hogan;M. Horn;D. Huang;C. Ignarra;M. Ihm;R. Jacobsen;W. Ji;K. Kazkaz;D. Khaitan;R. Knoche;N. Larsen;C. Lee;B. Lenardo;K. Lesko;A. Lindote;M. Lopes;D. Malling;A. Manalaysay;R. Mannino;M. F. Marzioni;D. Mckinsey;D. Mei;J. Mock;M. Moongweluwan;J. Morad;A. Murphy;C. Nehrkorn;H. Nelson;F. Neves;K. OSullivan;K. Oliver-Mallory;R. Ott;K. Palladino;M. Pangilinan;E. K. Pease;P. Phelps;L. Reichhart;C. Rhyne;S. Shaw;T. Shutt;C. Silva;V. Solovov;P. Sorensen;S. Stephenson;T. Sumner;M. Szydagis;D. Taylor;W. Taylor;B. Tennyson;P. Terman;D. Tiedt;W. To;M. Tripathi;L. Tvrznikova;S. Uvarov;J. Verbus;R. Webb;J. White;T. J. Whitis;M. Witherell;F. Wolfs;S. Young;C. Zhang

文献摘要

被引文献

相似文献

我们提出了测量的电子反冲（ER）的LUX暗物质探测器的响应的基础上170 000高纯度和空间均匀的氚衰变。我们重建的氚能谱使用组合的能量模型，并找到良好的协议与预期。我们报告的平均电荷和光产额的ER事件在液体氙在180和105 V/cm，并比较结果的NEST模型。我们还测量了平均电荷复合分数及其波动，我们调查的位置和宽度的LUX ER带。这些结果为LUX运行3弱相互作用大质量粒子搜索的重新分析提供了输入。
We present measurements of the electron-recoil (ER) response of the LUX dark matter detector based upon 170 000 highly pure and spatially uniform tritium decays. We reconstruct the tritium energy spectrum using the combined energy model and find good agreement with expectations. We report the average charge and light yields of ER events in liquid xenon at 180 and 105 V/cm and compare the results to the NEST model. We also measure the mean charge recombination fraction and its fluctuations, and we investigate the location and width of the LUX ER band. These results provide input to a reanalysis of the LUX run 3 weakly interacting massive particle search.