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Measurement of the Gamma Ray Background in the Davis Cavern at the Sanford Underground Research Facility
Astroparticle Physics ( IF 3.5 ) Pub Date : 2020-03-01 , DOI: 10.1016/j.astropartphys.2019.102391 D.S. Akerib , C.W. Akerlof , S.K. Alsum , N. Angelides , H.M. Araújo , J.E. Armstrong , M. Arthurs , X. Bai , J. Balajthy , S. Balashov , A. Baxter , E.P. Bernard , A. Biekert , 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 , M.C. Carmona-Benitez , M. Cascella , C. Chan , A. Cole , A. Cottle , J.E. Cutter , C.E. Dahl , L. de Viveiros , J.E.Y. Dobson , E. Druszkiewicz , T.K. Edberg , A. Fan , S. Fiorucci , H. Flaecher , T. Fruth , R.J. Gaitskell , J. Genovesi , C. Ghag , M.G.D. Gilchriese , S. Gokhale , M.G.D. van der Grinten , C.R. Hall , S. Hans , J. Harrison , S.J. Haselschwardt , S.A. Hertel , J.Y-K. Hor , M. Horn , D.Q. Huang , C.M. Ignarra , O. Jahangir , W. Ji , J. Johnson , A.C. Kaboth , K. Kamdin , D. Khaitan , A. Khazov , W.T. Kim , C.D. Kocher , L. Korley , E.V. Korolkova , J. Kras , H. Kraus , S.W. Kravitz , L. Kreczko , B. Krikler , V.A. Kudryavtsev , E.A. Leason , J. Lee , D.S. Leonard , K.T. Lesko , C. Levy , J. Li , J. Liao , F.-T. Liao , J. Lin , A. Lindote , R. Linehan , W.H. Lippincott , R. Liu , X. Liu , C. Loniewski , M.I. Lopes , B. López Paredes , W. Lorenzon , S. Luitz , J.M. Lyle , P.A. Majewski , A. Manalaysay , L. Manenti , R.L. Mannino , N. Marangou , M.F. Marzioni , D.N. McKinsey , J. McLaughlin , Y. Meng , E.H. Miller , M.E. Monzani , J.A. Morad , E. Morrison , B.J. Mount , A.St.J. Murphy , D. Naim , A. Naylor , C. Nedlik , C. Nehrkorn , H.N. Nelson , F. Neves , J. Nikoleyczik , A. Nilima , I. Olcina , K.C. Oliver-Mallory , S. Pal , K.J. Palladino , E.K. Pease , B.P. Penning , G. Pereira , A. Piepke , K. Pushkin , J. Reichenbacher , C.A. Rhyne , Q. Riffard , G.R.C. Rischbieter , J.P. Rodrigues , R. Rosero , P. Rossiter , G. Rutherford , A.B.M.R. Sazzad , R.W. Schnee , M. Schubnell , P.R. Scovell , D. Seymour , S. Shaw , T.A. Shutt , J.J. Silk , C. Silva , M. Solmaz , V.N. Solovov , P. Sorensen , I. Stancu , A. Stevens , T.M. Stiegler , K. Stifter , M. Szydagis , W.C. Taylor , R. Taylor , D. Temples , P.A. Terman , D.R. Tiedt , M. Timalsina , A. Tomás , M. Tripathi , L. Tvrznikova , U. Utku , S. Uvarov , A. Vacheret , J.J. Wang , J.R. Watson , R.C. Webb , R.G. White , T.J. Whitis , F.L.H. Wolfs , D. Woodward , J. Yin
Astroparticle Physics ( IF 3.5 ) Pub Date : 2020-03-01 , DOI: 10.1016/j.astropartphys.2019.102391 D.S. Akerib , C.W. Akerlof , S.K. Alsum , N. Angelides , H.M. Araújo , J.E. Armstrong , M. Arthurs , X. Bai , J. Balajthy , S. Balashov , A. Baxter , E.P. Bernard , A. Biekert , 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 , M.C. Carmona-Benitez , M. Cascella , C. Chan , A. Cole , A. Cottle , J.E. Cutter , C.E. Dahl , L. de Viveiros , J.E.Y. Dobson , E. Druszkiewicz , T.K. Edberg , A. Fan , S. Fiorucci , H. Flaecher , T. Fruth , R.J. Gaitskell , J. Genovesi , C. Ghag , M.G.D. Gilchriese , S. Gokhale , M.G.D. van der Grinten , C.R. Hall , S. Hans , J. Harrison , S.J. Haselschwardt , S.A. Hertel , J.Y-K. Hor , M. Horn , D.Q. Huang , C.M. Ignarra , O. Jahangir , W. Ji , J. Johnson , A.C. Kaboth , K. Kamdin , D. Khaitan , A. Khazov , W.T. Kim , C.D. Kocher , L. Korley , E.V. Korolkova , J. Kras , H. Kraus , S.W. Kravitz , L. Kreczko , B. Krikler , V.A. Kudryavtsev , E.A. Leason , J. Lee , D.S. Leonard , K.T. Lesko , C. Levy , J. Li , J. Liao , F.-T. Liao , J. Lin , A. Lindote , R. Linehan , W.H. Lippincott , R. Liu , X. Liu , C. Loniewski , M.I. Lopes , B. López Paredes , W. Lorenzon , S. Luitz , J.M. Lyle , P.A. Majewski , A. Manalaysay , L. Manenti , R.L. Mannino , N. Marangou , M.F. Marzioni , D.N. McKinsey , J. McLaughlin , Y. Meng , E.H. Miller , M.E. Monzani , J.A. Morad , E. Morrison , B.J. Mount , A.St.J. Murphy , D. Naim , A. Naylor , C. Nedlik , C. Nehrkorn , H.N. Nelson , F. Neves , J. Nikoleyczik , A. Nilima , I. Olcina , K.C. Oliver-Mallory , S. Pal , K.J. Palladino , E.K. Pease , B.P. Penning , G. Pereira , A. Piepke , K. Pushkin , J. Reichenbacher , C.A. Rhyne , Q. Riffard , G.R.C. Rischbieter , J.P. Rodrigues , R. Rosero , P. Rossiter , G. Rutherford , A.B.M.R. Sazzad , R.W. Schnee , M. Schubnell , P.R. Scovell , D. Seymour , S. Shaw , T.A. Shutt , J.J. Silk , C. Silva , M. Solmaz , V.N. Solovov , P. Sorensen , I. Stancu , A. Stevens , T.M. Stiegler , K. Stifter , M. Szydagis , W.C. Taylor , R. Taylor , D. Temples , P.A. Terman , D.R. Tiedt , M. Timalsina , A. Tomás , M. Tripathi , L. Tvrznikova , U. Utku , S. Uvarov , A. Vacheret , J.J. Wang , J.R. Watson , R.C. Webb , R.G. White , T.J. Whitis , F.L.H. Wolfs , D. Woodward , J. Yin
Abstract Deep underground environments are ideal for low background searches due to the attenuation of cosmic rays by passage through the earth. However, they are affected by backgrounds from γ-rays emitted by 40K and the 238U and 232Th decay chains in the surrounding rock. The LUX-ZEPLIN (LZ) experiment will search for dark matter particle interactions with a liquid xenon TPC located within the Davis campus at the Sanford Underground Research Facility, Lead, South Dakota, at the 4850-foot level. In order to characterise the cavern background, in-situ γ-ray measurements were taken with a sodium iodide detector in various locations and with lead shielding. The integral count rates (0–3300 keV) varied from 596 Hz to 1355 Hz for unshielded measurements, corresponding to a total flux from the cavern walls of 1.9 ± 0.4 γ cm − 2 s − 1 . The resulting activity in the walls of the cavern can be characterised as 220 ± 60 Bq/kg of 40K, 29 ± 15 Bq/kg of 238U, and 13 ± 3 Bq/kg of 232Th.
中文翻译：
在桑福德地下研究设施测量戴维斯洞穴中的伽马射线背景
摘要 由于宇宙射线穿过地球而衰减，深地下环境是低背景搜索的理想选择。然而，它们受到 40K 发射的 γ 射线以及围岩中的 238U 和 232Th 衰变链的背景影响。LUX-ZEPLIN (LZ) 实验将搜索暗物质粒子与位于南达科他州利德市桑福德地下研究设施戴维斯校区内 4850 英尺高的液态氙 TPC 的相互作用。为了表征洞穴背景，使用碘化钠探测器在不同位置和铅屏蔽进行了原位 γ 射线测量。对于非屏蔽测量，积分计数率 (0–3300 keV) 从 596 Hz 到 1355 Hz 不等，对应于来自洞穴壁的总通量为 1.9 ± 0.4 γ cm - 2 s - 1 。
更新日期：2020-03-01
中文翻译：
在桑福德地下研究设施测量戴维斯洞穴中的伽马射线背景
摘要 由于宇宙射线穿过地球而衰减，深地下环境是低背景搜索的理想选择。然而，它们受到 40K 发射的 γ 射线以及围岩中的 238U 和 232Th 衰变链的背景影响。LUX-ZEPLIN (LZ) 实验将搜索暗物质粒子与位于南达科他州利德市桑福德地下研究设施戴维斯校区内 4850 英尺高的液态氙 TPC 的相互作用。为了表征洞穴背景，使用碘化钠探测器在不同位置和铅屏蔽进行了原位 γ 射线测量。对于非屏蔽测量，积分计数率 (0–3300 keV) 从 596 Hz 到 1355 Hz 不等，对应于来自洞穴壁的总通量为 1.9 ± 0.4 γ cm - 2 s - 1 。
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