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Title: Chromatographic separation of radioactive noble gases from xenon

Abstract

The Large Underground Xenon (LUX) experiment operates at the Sanford Underground Research Facility to detect nuclear recoils from the hypothetical Weakly Interacting Massive Particles (WIMPs) on a liquid xenon target. Liquid xenon typically contains trace amounts of the noble radioactive isotopes $$^{85}$$Kr and $$^{39}$$Ar that are not removed by the in situ gas purification system. The decays of these isotopes at concentrations typical of research-grade xenon would be a dominant background for a WIMP search exmperiment. To remove these impurities from the liquid xenon, a chromatographic separation system based on adsorption on activated charcoal was built. 400 kg of xenon was processed, reducing the average concentration of krypton from 130 ppb to 3.5 ppt as measured by a cold-trap assisted mass spectroscopy system. A 50 kg batch spiked to 0.001 g/g of krypton was processed twice and reduced to an upper limit of 0.2 ppt.

Authors:
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Publication Date:
Research Org.:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
Contributing Org.:
LUX Collaboration
OSTI Identifier:
1398510
Grant/Contract Number:
AC02-05CH11231; FG02-08ER41549; FG02-91ER40688; FG02-95ER40917; FG02-91ER40674; NA0000979; FG02-11ER41738; SC0006605; AC52-07NA27344; FG01-91ER40618
Resource Type:
Journal Article: Accepted Manuscript
Journal Name:
Astroparticle Physics
Additional Journal Information:
Journal Volume: 97; Journal ID: ISSN 0927-6505
Publisher:
Elsevier
Country of Publication:
United States
Language:
English
Subject:
46 INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY; 38 RADIATION CHEMISTRY, RADIOCHEMISTRY, AND NUCLEAR CHEMISTRY; Xenon; Krypton; Adsorption; Chromatography; Gas Separation; Charcoal; Dark Matter

Citation Formats

Akerib, DS, Araújo, HM, Bai, X, Bailey, AJ, Balajthy, J, Beltrame, P, Bernard, EP, Bernstein, A, Biesiadzinski, TP, Boulton, EM, Bramante, R, Cahn, SB, Carmona-Benitez, MC, Chan, C, Chiller, AA, Chiller, C, Coffey, T, Currie, A, Cutter, JE, Davison, TJR, Dobi, A, Dobson, JEY, Druszkiewicz, E, Edwards, BN, Faham, CH, Fiorucci, S, Gaitskell, RJ, Gehman, VM, Ghag, C, Gibson, KR, Gilchriese, MGD, Hall, CR, Hanhardt, M, Haselschwardt, SJ, Hertel, SA, Hogan, DP, Horn, M, Huang, DQ, Ignarra, CM, Ihm, M, Jacobsen, RG, Ji, W, Kamdin, K, Kazkaz, K, Khaitan, D, Knoche, R, Larsen, NA, Lee, C, Lenardo, BG, Lesko, KT, Lindote, A, Lopes, MI, Manalaysay, A, Mannino, RL, Marzioni, MF, McKinsey, DN, Mei, D-M, Mock, J, Moongweluwan, M, Morad, JA, Murphy, ASJ, Nehrkorn, C, Nelson, HN, Neves, F, O'Sullivan, K, Oliver-Mallory, KC, Palladino, KJ, Pease, EK, Pech, K, Phelps, P, Reichhart, L, Rhyne, C, Shaw, S, Shutt, TA, Silva, C, Solovov, VN, Sorensen, P, Stephenson, S, Sumner, TJ, Szydagis, M, Taylor, DJ, Taylor, W, Tennyson, BP, Terman, PA, Tiedt, DR, To, WH, Tripathi, M, Tvrznikova, L, Uvarov, S, Verbus, JR, Webb, RC, White, JT, Whitis, TJ, Witherell, MS, Wolfs, FLH, Yazdani, K, Young, SK, and Zhang, C. Chromatographic separation of radioactive noble gases from xenon. United States: N. p., 2017. Web. doi:10.1016/j.astropartphys.2017.10.014.
Akerib, DS, Araújo, HM, Bai, X, Bailey, AJ, Balajthy, J, Beltrame, P, Bernard, EP, Bernstein, A, Biesiadzinski, TP, Boulton, EM, Bramante, R, Cahn, SB, Carmona-Benitez, MC, Chan, C, Chiller, AA, Chiller, C, Coffey, T, Currie, A, Cutter, JE, Davison, TJR, Dobi, A, Dobson, JEY, Druszkiewicz, E, Edwards, BN, Faham, CH, Fiorucci, S, Gaitskell, RJ, Gehman, VM, Ghag, C, Gibson, KR, Gilchriese, MGD, Hall, CR, Hanhardt, M, Haselschwardt, SJ, Hertel, SA, Hogan, DP, Horn, M, Huang, DQ, Ignarra, CM, Ihm, M, Jacobsen, RG, Ji, W, Kamdin, K, Kazkaz, K, Khaitan, D, Knoche, R, Larsen, NA, Lee, C, Lenardo, BG, Lesko, KT, Lindote, A, Lopes, MI, Manalaysay, A, Mannino, RL, Marzioni, MF, McKinsey, DN, Mei, D-M, Mock, J, Moongweluwan, M, Morad, JA, Murphy, ASJ, Nehrkorn, C, Nelson, HN, Neves, F, O'Sullivan, K, Oliver-Mallory, KC, Palladino, KJ, Pease, EK, Pech, K, Phelps, P, Reichhart, L, Rhyne, C, Shaw, S, Shutt, TA, Silva, C, Solovov, VN, Sorensen, P, Stephenson, S, Sumner, TJ, Szydagis, M, Taylor, DJ, Taylor, W, Tennyson, BP, Terman, PA, Tiedt, DR, To, WH, Tripathi, M, Tvrznikova, L, Uvarov, S, Verbus, JR, Webb, RC, White, JT, Whitis, TJ, Witherell, MS, Wolfs, FLH, Yazdani, K, Young, SK, & Zhang, C. Chromatographic separation of radioactive noble gases from xenon. United States. doi:10.1016/j.astropartphys.2017.10.014.
Akerib, DS, Araújo, HM, Bai, X, Bailey, AJ, Balajthy, J, Beltrame, P, Bernard, EP, Bernstein, A, Biesiadzinski, TP, Boulton, EM, Bramante, R, Cahn, SB, Carmona-Benitez, MC, Chan, C, Chiller, AA, Chiller, C, Coffey, T, Currie, A, Cutter, JE, Davison, TJR, Dobi, A, Dobson, JEY, Druszkiewicz, E, Edwards, BN, Faham, CH, Fiorucci, S, Gaitskell, RJ, Gehman, VM, Ghag, C, Gibson, KR, Gilchriese, MGD, Hall, CR, Hanhardt, M, Haselschwardt, SJ, Hertel, SA, Hogan, DP, Horn, M, Huang, DQ, Ignarra, CM, Ihm, M, Jacobsen, RG, Ji, W, Kamdin, K, Kazkaz, K, Khaitan, D, Knoche, R, Larsen, NA, Lee, C, Lenardo, BG, Lesko, KT, Lindote, A, Lopes, MI, Manalaysay, A, Mannino, RL, Marzioni, MF, McKinsey, DN, Mei, D-M, Mock, J, Moongweluwan, M, Morad, JA, Murphy, ASJ, Nehrkorn, C, Nelson, HN, Neves, F, O'Sullivan, K, Oliver-Mallory, KC, Palladino, KJ, Pease, EK, Pech, K, Phelps, P, Reichhart, L, Rhyne, C, Shaw, S, Shutt, TA, Silva, C, Solovov, VN, Sorensen, P, Stephenson, S, Sumner, TJ, Szydagis, M, Taylor, DJ, Taylor, W, Tennyson, BP, Terman, PA, Tiedt, DR, To, WH, Tripathi, M, Tvrznikova, L, Uvarov, S, Verbus, JR, Webb, RC, White, JT, Whitis, TJ, Witherell, MS, Wolfs, FLH, Yazdani, K, Young, SK, and Zhang, C. Tue . "Chromatographic separation of radioactive noble gases from xenon". United States. doi:10.1016/j.astropartphys.2017.10.014.
@article{osti_1398510,
title = {Chromatographic separation of radioactive noble gases from xenon},
author = {Akerib, DS and Araújo, HM and Bai, X and Bailey, AJ and Balajthy, J and Beltrame, P and Bernard, EP and Bernstein, A and Biesiadzinski, TP and Boulton, EM and Bramante, R and Cahn, SB and Carmona-Benitez, MC and Chan, C and Chiller, AA and Chiller, C and Coffey, T and Currie, A and Cutter, JE and Davison, TJR and Dobi, A and Dobson, JEY and Druszkiewicz, E and Edwards, BN and Faham, CH and Fiorucci, S and Gaitskell, RJ and Gehman, VM and Ghag, C and Gibson, KR and Gilchriese, MGD and Hall, CR and Hanhardt, M and Haselschwardt, SJ and Hertel, SA and Hogan, DP and Horn, M and Huang, DQ and Ignarra, CM and Ihm, M and Jacobsen, RG and Ji, W and Kamdin, K and Kazkaz, K and Khaitan, D and Knoche, R and Larsen, NA and Lee, C and Lenardo, BG and Lesko, KT and Lindote, A and Lopes, MI and Manalaysay, A and Mannino, RL and Marzioni, MF and McKinsey, DN and Mei, D-M and Mock, J and Moongweluwan, M and Morad, JA and Murphy, ASJ and Nehrkorn, C and Nelson, HN and Neves, F and O'Sullivan, K and Oliver-Mallory, KC and Palladino, KJ and Pease, EK and Pech, K and Phelps, P and Reichhart, L and Rhyne, C and Shaw, S and Shutt, TA and Silva, C and Solovov, VN and Sorensen, P and Stephenson, S and Sumner, TJ and Szydagis, M and Taylor, DJ and Taylor, W and Tennyson, BP and Terman, PA and Tiedt, DR and To, WH and Tripathi, M and Tvrznikova, L and Uvarov, S and Verbus, JR and Webb, RC and White, JT and Whitis, TJ and Witherell, MS and Wolfs, FLH and Yazdani, K and Young, SK and Zhang, C},
abstractNote = {The Large Underground Xenon (LUX) experiment operates at the Sanford Underground Research Facility to detect nuclear recoils from the hypothetical Weakly Interacting Massive Particles (WIMPs) on a liquid xenon target. Liquid xenon typically contains trace amounts of the noble radioactive isotopes $^{85}$Kr and $^{39}$Ar that are not removed by the in situ gas purification system. The decays of these isotopes at concentrations typical of research-grade xenon would be a dominant background for a WIMP search exmperiment. To remove these impurities from the liquid xenon, a chromatographic separation system based on adsorption on activated charcoal was built. 400 kg of xenon was processed, reducing the average concentration of krypton from 130 ppb to 3.5 ppt as measured by a cold-trap assisted mass spectroscopy system. A 50 kg batch spiked to 0.001 g/g of krypton was processed twice and reduced to an upper limit of 0.2 ppt.},
doi = {10.1016/j.astropartphys.2017.10.014},
journal = {Astroparticle Physics},
number = ,
volume = 97,
place = {United States},
year = {Tue Oct 31 00:00:00 EDT 2017},
month = {Tue Oct 31 00:00:00 EDT 2017}
}

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