Radiogenic and muon-induced backgrounds in the LUX dark matter detector

D. S. Akerib; H. M. Araújo; X. Bai; A. J. Bailey; J. Balajthy; E. Bernard; A. Bernstein; A. Bradley; D. Byram; S. B. Cahn; M. C. Carmona-Benitez; C. Chan; J. J. Chapman; A. A. Chiller; C. Chiller; T. Coffey; A. Currie; L. De Viveiros; A. Dobi; J. Dobson; E. Druszkiewicz; B. Edwards; C. H. Faham; S. Fiorucci; C. Flores; R. J. Gaitskell; V. M. Gehman; C. Ghag; K. R. Gibson; M. G.D. Gilchriese; C. Hall; S. A. Hertel; M. Horn; D. Q. Huang; M. Ihm; R. G. Jacobsen; K. Kazkaz; R. Knoche; N. A. Larsen; C. Lee; A. Lindote; M. I. Lopes; D. C. Malling; R. Mannino; D. N. McKinsey; D. M. Mei; J. Mock; M. Moongweluwan; J. Morad; A. St J. Murphy; C. Nehrkorn; H. Nelson; F. Neves; R. A. Ott; M. Pangilinan; P. D. Parker; E. K. Pease; K. Pech; P. Phelps; L. Reichhart; T. Shutt; C. Silva; V. N. Solovov; P. Sorensen; K. O'Sullivan; T. J. Sumner; M. Szydagis; D. Taylor; B. Tennyson; D. R. Tiedt; M. Tripathi; S. Uvarov; J. R. Verbus; N. Walsh; R. Webb; J. T. White; M. S. Witherell; F. L.H. Wolfs; M. Woods; C. Zhang

doi:10.1016/j.astropartphys.2014.07.009

Radiogenic and muon-induced backgrounds in the LUX dark matter detector

D. S. Akerib, H. M. Araújo, X. Bai, A. J. Bailey, J. Balajthy, E. Bernard, A. Bernstein, A. Bradley, D. Byram, S. B. Cahn, M. C. Carmona-Benitez, C. Chan, J. J. Chapman, A. A. Chiller, C. Chiller, T. Coffey, A. Currie, L. De Viveiros, A. Dobi, J. DobsonE. Druszkiewicz, B. Edwards, C. H. Faham, S. Fiorucci, C. Flores, R. J. Gaitskell, V. M. Gehman, C. Ghag, K. R. Gibson, M. G.D. Gilchriese, C. Hall, S. A. Hertel, M. Horn, D. Q. Huang, M. Ihm, R. G. Jacobsen, K. Kazkaz, R. Knoche, N. A. Larsen, C. Lee, A. Lindote, M. I. Lopes, D. C. Malling, R. Mannino, D. N. McKinsey, D. M. Mei, J. Mock, M. Moongweluwan, J. Morad, A. St J. Murphy, C. Nehrkorn, H. Nelson, F. Neves, R. A. Ott, M. Pangilinan, P. D. Parker, E. K. Pease, K. Pech, P. Phelps, L. Reichhart, T. Shutt, C. Silva, V. N. Solovov, P. Sorensen, K. O'Sullivan, T. J. Sumner, M. Szydagis, D. Taylor, B. Tennyson, D. R. Tiedt, M. Tripathi, S. Uvarov, J. R. Verbus, N. Walsh, R. Webb, J. T. White, M. S. Witherell, F. L.H. Wolfs, M. Woods, C. Zhang

Research output: Contribution to journal › Article › peer-review

71 Scopus citations

Abstract

The Large Underground Xenon (LUX) dark matter experiment aims to detect rare low-energy interactions from Weakly Interacting Massive Particles (WIMPs). The radiogenic backgrounds in the LUX detector have been measured and compared with Monte Carlo simulation. Measurements of LUX high-energy data have provided direct constraints on all background sources contributing to the background model. The expected background rate from the background model for the 85.3 day WIMP search run is (2.6±0.2_stat±0.4_sys) ×10^-3 events keVee-1kg-¹day-¹ in a 118 kg fiducial volume. The observed background rate is (3.6±0.4 _stat)×10^-3 events keVee-1kg-¹day- ¹, consistent with model projections. The expectation for the radiogenic background in a subsequent one-year run is presented.

Original language	English (US)
Pages (from-to)	33-46
Number of pages	14
Journal	Astroparticle Physics
Volume	62
DOIs	https://doi.org/10.1016/j.astropartphys.2014.07.009
State	Published - Mar 2015

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics

Access to Document

10.1016/j.astropartphys.2014.07.009

Cite this

Akerib, D. S., Araújo, H. M., Bai, X., Bailey, A. J., Balajthy, J., Bernard, E., Bernstein, A., Bradley, A., Byram, D., Cahn, S. B., Carmona-Benitez, M. C., Chan, C., Chapman, J. J., Chiller, A. A., Chiller, C., Coffey, T., Currie, A., De Viveiros, L., Dobi, A., ... Zhang, C. (2015). Radiogenic and muon-induced backgrounds in the LUX dark matter detector. Astroparticle Physics, 62, 33-46. https://doi.org/10.1016/j.astropartphys.2014.07.009

@article{1205227524824e9a8d9c30255f91aef3,

title = "Radiogenic and muon-induced backgrounds in the LUX dark matter detector",

abstract = "The Large Underground Xenon (LUX) dark matter experiment aims to detect rare low-energy interactions from Weakly Interacting Massive Particles (WIMPs). The radiogenic backgrounds in the LUX detector have been measured and compared with Monte Carlo simulation. Measurements of LUX high-energy data have provided direct constraints on all background sources contributing to the background model. The expected background rate from the background model for the 85.3 day WIMP search run is (2.6±0.2stat±0.4sys) ×10-3 events keVee-1kg-1day-1 in a 118 kg fiducial volume. The observed background rate is (3.6±0.4 stat)×10-3 events keVee-1kg-1day- 1, consistent with model projections. The expectation for the radiogenic background in a subsequent one-year run is presented.",

author = "Akerib, {D. S.} and Ara{\'u}jo, {H. M.} and X. Bai and Bailey, {A. J.} and J. Balajthy and E. Bernard and A. Bernstein and A. Bradley and D. Byram and Cahn, {S. B.} and Carmona-Benitez, {M. C.} and C. Chan and Chapman, {J. J.} and Chiller, {A. A.} and C. Chiller and T. Coffey and A. Currie and {De Viveiros}, L. and A. Dobi and J. Dobson and E. Druszkiewicz and B. Edwards and Faham, {C. H.} and S. Fiorucci and C. Flores and Gaitskell, {R. J.} and Gehman, {V. M.} and C. Ghag and Gibson, {K. R.} and Gilchriese, {M. G.D.} and C. Hall and Hertel, {S. A.} and M. Horn and Huang, {D. Q.} and M. Ihm and Jacobsen, {R. G.} and K. Kazkaz and R. Knoche and Larsen, {N. A.} and C. Lee and A. Lindote and Lopes, {M. I.} and Malling, {D. C.} and R. Mannino and McKinsey, {D. N.} and Mei, {D. M.} and J. Mock and M. Moongweluwan and J. Morad and Murphy, {A. St J.} and C. Nehrkorn and H. Nelson and F. Neves and Ott, {R. A.} and M. Pangilinan and Parker, {P. D.} and Pease, {E. K.} and K. Pech and P. Phelps and L. Reichhart and T. Shutt and C. Silva and Solovov, {V. N.} and P. Sorensen and K. O'Sullivan and Sumner, {T. J.} and M. Szydagis and D. Taylor and B. Tennyson and Tiedt, {D. R.} and M. Tripathi and S. Uvarov and Verbus, {J. R.} and N. Walsh and R. Webb and White, {J. T.} and Witherell, {M. S.} and Wolfs, {F. L.H.} and M. Woods and C. Zhang",

note = "Funding Information: This work was partially supported by the U.S. Department of Energy (DOE) under Award numbers DE-FG02-08ER41549 , DE-FG02-91ER40688 , DE-FG02-95ER40917 , DE-FG02-91ER40674 , DE-NA0000979 , DE-FG02-11ER41738 , DE-SC0006605 , DE-AC02-05CH11231 , DE-AC52-07NA27344 , and DE-FG01-91ER40618 ; the U.S. National Science Foundation under Award numbers PHYS-0750671 , PHY-0801536 , PHY-1004661 , PHY-1102470 , PHY-1003660 , PHY-1312561 , PHY-1347449 ; the Research Corporation Grant RA0350 ; the Center for Ultra-low Background Experiments in the Dakotas (CUBED) ; and the South Dakota School of Mines and Technology (SDSMT) . LIP-Coimbra acknowledges funding from Funda{\c c}{\~a}o para a Ci{\^e}ncia e Tecnologia (FCT) through the Project-Grant CERN/FP/123610/2011 . Imperial College and Brown University thank the UK Royal Society for travel funds under the International Exchange Scheme ( IE120804 ). The UK groups acknowledge institutional support from Imperial College London, University College London and Edinburgh University, and from the Science & Technology Facilities Council for Ph. D. studentship ST/K502042/1 (AB). The University of Edinburgh is a charitable body, registered in Scotland, with registration number SC005336. This research was conducted using computational resources and services at the Center for Computation and Visualization, Brown University. ",

year = "2015",

month = mar,

doi = "10.1016/j.astropartphys.2014.07.009",

language = "English (US)",

volume = "62",

pages = "33--46",

journal = "Astroparticle Physics",

issn = "0927-6505",

publisher = "Elsevier",

}

Akerib, DS, Araújo, HM, Bai, X, Bailey, AJ, Balajthy, J, Bernard, E, Bernstein, A, Bradley, A, Byram, D, Cahn, SB, Carmona-Benitez, MC, Chan, C, Chapman, JJ, Chiller, AA, Chiller, C, Coffey, T, Currie, A, De Viveiros, L, Dobi, A, Dobson, J, Druszkiewicz, E, Edwards, B, Faham, CH, Fiorucci, S, Flores, C, Gaitskell, RJ, Gehman, VM, Ghag, C, Gibson, KR, Gilchriese, MGD, Hall, C, Hertel, SA, Horn, M, Huang, DQ, Ihm, M, Jacobsen, RG, Kazkaz, K, Knoche, R, Larsen, NA, Lee, C, Lindote, A, Lopes, MI, Malling, DC, Mannino, R, McKinsey, DN, Mei, DM, Mock, J, Moongweluwan, M, Morad, J, Murphy, ASJ, Nehrkorn, C, Nelson, H, Neves, F, Ott, RA, Pangilinan, M, Parker, PD, Pease, EK, Pech, K, Phelps, P, Reichhart, L, Shutt, T, Silva, C, Solovov, VN, Sorensen, P, O'Sullivan, K, Sumner, TJ, Szydagis, M, Taylor, D, Tennyson, B, Tiedt, DR, Tripathi, M, Uvarov, S, Verbus, JR, Walsh, N, Webb, R, White, JT, Witherell, MS, Wolfs, FLH, Woods, M & Zhang, C 2015, 'Radiogenic and muon-induced backgrounds in the LUX dark matter detector', Astroparticle Physics, vol. 62, pp. 33-46. https://doi.org/10.1016/j.astropartphys.2014.07.009

TY - JOUR

T1 - Radiogenic and muon-induced backgrounds in the LUX dark matter detector

AU - Akerib, D. S.

AU - Araújo, H. M.

AU - Bai, X.

AU - Bailey, A. J.

AU - Balajthy, J.

AU - Bernard, E.

AU - Bernstein, A.

AU - Bradley, A.

AU - Byram, D.

AU - Cahn, S. B.

AU - Carmona-Benitez, M. C.

AU - Chan, C.

AU - Chapman, J. J.

AU - Chiller, A. A.

AU - Chiller, C.

AU - Coffey, T.

AU - Currie, A.

AU - De Viveiros, L.

AU - Dobi, A.

AU - Dobson, J.

AU - Druszkiewicz, E.

AU - Edwards, B.

AU - Faham, C. H.

AU - Fiorucci, S.

AU - Flores, C.

AU - Gaitskell, R. J.

AU - Gehman, V. M.

AU - Ghag, C.

AU - Gibson, K. R.

AU - Gilchriese, M. G.D.

AU - Hall, C.

AU - Hertel, S. A.

AU - Horn, M.

AU - Huang, D. Q.

AU - Ihm, M.

AU - Jacobsen, R. G.

AU - Kazkaz, K.

AU - Knoche, R.

AU - Larsen, N. A.

AU - Lee, C.

AU - Lindote, A.

AU - Lopes, M. I.

AU - Malling, D. C.

AU - Mannino, R.

AU - McKinsey, D. N.

AU - Mei, D. M.

AU - Mock, J.

AU - Moongweluwan, M.

AU - Morad, J.

AU - Murphy, A. St J.

AU - Nehrkorn, C.

AU - Nelson, H.

AU - Neves, F.

AU - Ott, R. A.

AU - Pangilinan, M.

AU - Parker, P. D.

AU - Pease, E. K.

AU - Pech, K.

AU - Phelps, P.

AU - Reichhart, L.

AU - Shutt, T.

AU - Silva, C.

AU - Solovov, V. N.

AU - Sorensen, P.

AU - O'Sullivan, K.

AU - Sumner, T. J.

AU - Szydagis, M.

AU - Taylor, D.

AU - Tennyson, B.

AU - Tiedt, D. R.

AU - Tripathi, M.

AU - Uvarov, S.

AU - Verbus, J. R.

AU - Walsh, N.

AU - Webb, R.

AU - White, J. T.

AU - Witherell, M. S.

AU - Wolfs, F. L.H.

AU - Woods, M.

AU - Zhang, C.

N1 - Funding Information: This work was partially supported by the U.S. Department of Energy (DOE) under Award numbers DE-FG02-08ER41549 , DE-FG02-91ER40688 , DE-FG02-95ER40917 , DE-FG02-91ER40674 , DE-NA0000979 , DE-FG02-11ER41738 , DE-SC0006605 , DE-AC02-05CH11231 , DE-AC52-07NA27344 , and DE-FG01-91ER40618 ; the U.S. National Science Foundation under Award numbers PHYS-0750671 , PHY-0801536 , PHY-1004661 , PHY-1102470 , PHY-1003660 , PHY-1312561 , PHY-1347449 ; the Research Corporation Grant RA0350 ; the Center for Ultra-low Background Experiments in the Dakotas (CUBED) ; and the South Dakota School of Mines and Technology (SDSMT) . LIP-Coimbra acknowledges funding from Fundação para a Ciência e Tecnologia (FCT) through the Project-Grant CERN/FP/123610/2011 . Imperial College and Brown University thank the UK Royal Society for travel funds under the International Exchange Scheme ( IE120804 ). The UK groups acknowledge institutional support from Imperial College London, University College London and Edinburgh University, and from the Science & Technology Facilities Council for Ph. D. studentship ST/K502042/1 (AB). The University of Edinburgh is a charitable body, registered in Scotland, with registration number SC005336. This research was conducted using computational resources and services at the Center for Computation and Visualization, Brown University.

PY - 2015/3

Y1 - 2015/3

N2 - The Large Underground Xenon (LUX) dark matter experiment aims to detect rare low-energy interactions from Weakly Interacting Massive Particles (WIMPs). The radiogenic backgrounds in the LUX detector have been measured and compared with Monte Carlo simulation. Measurements of LUX high-energy data have provided direct constraints on all background sources contributing to the background model. The expected background rate from the background model for the 85.3 day WIMP search run is (2.6±0.2stat±0.4sys) ×10-3 events keVee-1kg-1day-1 in a 118 kg fiducial volume. The observed background rate is (3.6±0.4 stat)×10-3 events keVee-1kg-1day- 1, consistent with model projections. The expectation for the radiogenic background in a subsequent one-year run is presented.

AB - The Large Underground Xenon (LUX) dark matter experiment aims to detect rare low-energy interactions from Weakly Interacting Massive Particles (WIMPs). The radiogenic backgrounds in the LUX detector have been measured and compared with Monte Carlo simulation. Measurements of LUX high-energy data have provided direct constraints on all background sources contributing to the background model. The expected background rate from the background model for the 85.3 day WIMP search run is (2.6±0.2stat±0.4sys) ×10-3 events keVee-1kg-1day-1 in a 118 kg fiducial volume. The observed background rate is (3.6±0.4 stat)×10-3 events keVee-1kg-1day- 1, consistent with model projections. The expectation for the radiogenic background in a subsequent one-year run is presented.

UR - http://www.scopus.com/inward/record.url?scp=84906087192&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84906087192&partnerID=8YFLogxK

U2 - 10.1016/j.astropartphys.2014.07.009

DO - 10.1016/j.astropartphys.2014.07.009

M3 - Article

AN - SCOPUS:84906087192

SN - 0927-6505

VL - 62

SP - 33

EP - 46

JO - Astroparticle Physics

JF - Astroparticle Physics

ER -

Radiogenic and muon-induced backgrounds in the LUX dark matter detector

Abstract

All Science Journal Classification (ASJC) codes

Access to Document

Other files and links

Fingerprint

Cite this