Abstract
The LUX-ZEPLIN dark matter search aims to achieve a sensitivity to the WIMP-nucleon spin-independent cross-section down to (1–2)×10−12 pb at a WIMP mass of 40 GeV/c2. This paper describes the simulations framework that, along with radioactivity measurements, was used to support this projection, and also to provide mock data for validating reconstruction and analysis software. Of particular note are the event generators, which allow us to model the background radiation, and the detector response physics used in the production of raw signals, which can be converted into digitized waveforms similar to data from the operational detector. Inclusion of the detector response allows us to process simulated data using the same analysis routines as developed to process the experimental data.
| Original language | English (US) |
|---|---|
| Article number | 102480 |
| Journal | Astroparticle Physics |
| Volume | 125 |
| DOIs | |
| State | Published - Feb 2021 |
ASJC Scopus subject areas
- Astronomy and Astrophysics
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Simulations of events for the LUX-ZEPLIN (LZ) dark matter experiment. / Akerib, D. S.; Akerlof, C. W.; Alqahtani, A.; Alsum, S. K.; Anderson, T. J.; Angelides, N.; Araújo, H. M.; Armstrong, J. E.; Arthurs, M.; Bai, X.; Balajthy, J.; Balashov, S.; Bang, J.; Bauer, D.; Baxter, A.; Bensinger, J.; Bernard, E. P.; Bernstein, A.; Bhatti, A.; Biekert, A.; Biesiadzinski, T. P.; Birch, H. J.; Boast, K. E.; Boxer, B.; Brás, P.; Buckley, J. H.; Bugaev, V. V.; Burdin, S.; Busenitz, J. K.; Cabrita, R.; Carels, C.; Carlsmith, D. L.; Carmona-Benitez, M. C.; Cascella, M.; Chan, C.; Chott, N. I.; Cole, A.; Cottle, A.; Cutter, J. E.; Dahl, C. E.; de Viveiros, L.; Dobson, J. E.Y.; Druszkiewicz, E.; Edberg, T. K.; Eriksen, S. R.; Fan, A.; Fayer, S.; Fiorucci, S.; Flaecher, H.; Fraser, E. D.; Fruth, T.; Gaitskell, R. J.; Genovesi, J.; Ghag, C.; Gibson, E.; Gilchriese, M. G.D.; Gokhale, S.; van der Grinten, M. G.D.; Hall, C. R.; Harrison, A.; Haselschwardt, S. J.; Hertel, S. A.; Hor, J. Y.K.; Horn, M.; Huang, D. Q.; Ignarra, C. M.; Jahangir, O.; Ji, W.; Johnson, J.; Kaboth, A. C.; Kamaha, A. C.; Kamdin, K.; Kazkaz, K.; Khaitan, D.; Khazov, A.; Khurana, I.; Kocher, C. D.; Korley, L.; Korolkova, E. V.; Kras, J.; Kraus, H.; Kravitz, S.; Kreczko, L.; Krikler, B.; Kudryavtsev, V. A.; Leason, E. A.; Lee, J.; Leonard, D. S.; Lesko, K. T.; Levy, C.; Li, J.; Liao, J.; Liao, F. T.; Lin, J.; Lindote, A.; Linehan, R.; Lippincott, W. H.; Liu, R.; Liu, X.; Loniewski, C.; Lopes, M. I.; López Paredes, B.; Lorenzon, W.; Luitz, S.; Lyle, J. M.; Majewski, P. A.; Manalaysay, A.; Manenti, L.; Mannino, R. L.; Marangou, N.; Marzioni, M. F.; McKinsey, D. N.; McLaughlin, J.; Meng, Y.; Miller, E. H.; Mizrachi, E.; Monte, A.; Monzani, M. E.; Morad, J. A.; Morrison, E.; Mount, B. J.; Murphy, A. St J.; Naim, D.; Naylor, A.; Nedlik, C.; Nehrkorn, C.; Nelson, H. N.; Neves, F.; Nikoleyczik, J. A.; Nilima, A.; Olcina, I.; Oliver-Mallory, K. C.; Pal, S.; Palladino, K. J.; Palmer, J.; Parveen, N.; Pease, E. K.; Penning, B.; Pereira, G.; Piepke, A.; Pushkin, K.; Reichenbacher, J.; Rhyne, C. A.; Richards, A.; Riffard, Q.; Rischbieter, G. R.C.; Rosero, R.; Rossiter, P.; Rutherford, G.; Santone, D.; Sazzad, A. B.M.R.; Schnee, R. W.; Schubnell, M.; Scovell, P. R.; Seymour, D.; Shaw, S.; Shutt, T. A.; Silk, J. J.; Silva, C.; Smith, R.; Solmaz, M.; Solovov, V. N.; Sorensen, P.; Stancu, I.; Stevens, A.; Stifter, K.; Sumner, T. J.; Swanson, N.; Szydagis, M.; Tan, M.; Taylor, W. C.; Taylor, R.; Temples, D. J.; Terman, P. A.; Tiedt, D. R.; Timalsina, M.; Tomás, A.; Tripathi, M.; Tronstad, D. R.; Turner, W.; Tvrznikova, L.; Utku, U.; Vacheret, A.; Vaitkus, A.; Wang, J. J.; Wang, W.; Watson, J. R.; Webb, R. C.; White, R. G.; Whitis, T. J.; Wolfs, F. L.H.; Woodward, D.; Xiang, X.; Xu, J.; Yeh, M.; Zarzhitsky, P.
In: Astroparticle Physics, Vol. 125, 102480, 02.2021.Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - Simulations of events for the LUX-ZEPLIN (LZ) dark matter experiment
AU - Akerib, D. S.
AU - Akerlof, C. W.
AU - Alqahtani, A.
AU - Alsum, S. K.
AU - Anderson, T. J.
AU - Angelides, N.
AU - Araújo, H. M.
AU - Armstrong, J. E.
AU - Arthurs, M.
AU - Bai, X.
AU - Balajthy, J.
AU - Balashov, S.
AU - Bang, J.
AU - Bauer, D.
AU - Baxter, A.
AU - Bensinger, J.
AU - Bernard, E. P.
AU - Bernstein, A.
AU - Bhatti, A.
AU - Biekert, A.
AU - Biesiadzinski, T. P.
AU - Birch, H. J.
AU - Boast, K. E.
AU - Boxer, B.
AU - Brás, P.
AU - Buckley, J. H.
AU - Bugaev, V. V.
AU - Burdin, S.
AU - Busenitz, J. K.
AU - Cabrita, R.
AU - Carels, C.
AU - Carlsmith, D. L.
AU - Carmona-Benitez, M. C.
AU - Cascella, M.
AU - Chan, C.
AU - Chott, N. I.
AU - Cole, A.
AU - Cottle, A.
AU - Cutter, J. E.
AU - Dahl, C. E.
AU - de Viveiros, L.
AU - Dobson, J. E.Y.
AU - Druszkiewicz, E.
AU - Edberg, T. K.
AU - Eriksen, S. R.
AU - Fan, A.
AU - Fayer, S.
AU - Fiorucci, S.
AU - Flaecher, H.
AU - Fraser, E. D.
AU - Fruth, T.
AU - Gaitskell, R. J.
AU - Genovesi, J.
AU - Ghag, C.
AU - Gibson, E.
AU - Gilchriese, M. G.D.
AU - Gokhale, S.
AU - van der Grinten, M. G.D.
AU - Hall, C. R.
AU - Harrison, A.
AU - Haselschwardt, S. J.
AU - Hertel, S. A.
AU - Hor, J. Y.K.
AU - Horn, M.
AU - Huang, D. Q.
AU - Ignarra, C. M.
AU - Jahangir, O.
AU - Ji, W.
AU - Johnson, J.
AU - Kaboth, A. C.
AU - Kamaha, A. C.
AU - Kamdin, K.
AU - Kazkaz, K.
AU - Khaitan, D.
AU - Khazov, A.
AU - Khurana, I.
AU - Kocher, C. D.
AU - Korley, L.
AU - Korolkova, E. V.
AU - Kras, J.
AU - Kraus, H.
AU - Kravitz, S.
AU - Kreczko, L.
AU - Krikler, B.
AU - Kudryavtsev, V. A.
AU - Leason, E. A.
AU - Lee, J.
AU - Leonard, D. S.
AU - Lesko, K. T.
AU - Levy, C.
AU - Li, J.
AU - Liao, J.
AU - Liao, F. T.
AU - Lin, J.
AU - Lindote, A.
AU - Linehan, R.
AU - Lippincott, W. H.
AU - Liu, R.
AU - Liu, X.
AU - Loniewski, C.
AU - Lopes, M. I.
AU - López Paredes, B.
AU - Lorenzon, W.
AU - Luitz, S.
AU - Lyle, J. M.
AU - Majewski, P. A.
AU - Manalaysay, A.
AU - Manenti, L.
AU - Mannino, R. L.
AU - Marangou, N.
AU - Marzioni, M. F.
AU - McKinsey, D. N.
AU - McLaughlin, J.
AU - Meng, Y.
AU - Miller, E. H.
AU - Mizrachi, E.
AU - Monte, A.
AU - Monzani, M. E.
AU - Morad, J. A.
AU - Morrison, E.
AU - Mount, B. J.
AU - Murphy, A. St J.
AU - Naim, D.
AU - Naylor, A.
AU - Nedlik, C.
AU - Nehrkorn, C.
AU - Nelson, H. N.
AU - Neves, F.
AU - Nikoleyczik, J. A.
AU - Nilima, A.
AU - Olcina, I.
AU - Oliver-Mallory, K. C.
AU - Pal, S.
AU - Palladino, K. J.
AU - Palmer, J.
AU - Parveen, N.
AU - Pease, E. K.
AU - Penning, B.
AU - Pereira, G.
AU - Piepke, A.
AU - Pushkin, K.
AU - Reichenbacher, J.
AU - Rhyne, C. A.
AU - Richards, A.
AU - Riffard, Q.
AU - Rischbieter, G. R.C.
AU - Rosero, R.
AU - Rossiter, P.
AU - Rutherford, G.
AU - Santone, D.
AU - Sazzad, A. B.M.R.
AU - Schnee, R. W.
AU - Schubnell, M.
AU - Scovell, P. R.
AU - Seymour, D.
AU - Shaw, S.
AU - Shutt, T. A.
AU - Silk, J. J.
AU - Silva, C.
AU - Smith, R.
AU - Solmaz, M.
AU - Solovov, V. N.
AU - Sorensen, P.
AU - Stancu, I.
AU - Stevens, A.
AU - Stifter, K.
AU - Sumner, T. J.
AU - Swanson, N.
AU - Szydagis, M.
AU - Tan, M.
AU - Taylor, W. C.
AU - Taylor, R.
AU - Temples, D. J.
AU - Terman, P. A.
AU - Tiedt, D. R.
AU - Timalsina, M.
AU - Tomás, A.
AU - Tripathi, M.
AU - Tronstad, D. R.
AU - Turner, W.
AU - Tvrznikova, L.
AU - Utku, U.
AU - Vacheret, A.
AU - Vaitkus, A.
AU - Wang, J. J.
AU - Wang, W.
AU - Watson, J. R.
AU - Webb, R. C.
AU - White, R. G.
AU - Whitis, T. J.
AU - Wolfs, F. L.H.
AU - Woodward, D.
AU - Xiang, X.
AU - Xu, J.
AU - Yeh, M.
AU - Zarzhitsky, P.
N1 - Funding Information: The research supporting this work took place in whole or in part at the Sanford Underground Research Facility (SURF) in Lead, South Dakota. Funding for this work is supported by the U.S. Department of Energy, Office of Science, Office of High Energy Physics under Contract Numbers DE-AC02-05CH11231, DE-SC0020216, DE-SC0012704, DE-SC0010010, DE-AC02-07CH11359, DE-SC0012161, DE-SC0014223, DE-FG02-13ER42020, DE-SC0009999, DE-NA0003180, DE-SC0011702, DESC0010072, DE-SC0015708, DE-SC0006605, DE-FG02-10ER46709, UW PRJ82AJ, DE-SC0013542, DE-AC02-76SF00515, DE-SC0018982, DE-SC0019066, DE-AC52-07NA27344 and DOE-SC0012447. This research was also supported by U.S. National Science Foundation (NSF); the U.K. Science & Technology Facilities Council under award numbers, ST/M003655/1, ST/M003981/1, ST/M003744/1, ST/M003639/1, ST/M003604/1, and ST/M003469/1; Portuguese Foundation for Science and Technology (FCT) under award numbers PTDC/FIS-PAR/28567/2017; the Institute for Basic Science, Korea (budget numbers IBS-R016-D1); University College London and Lawrence Berkeley National Laboratory thank the U.K. Royal Society for travel funds under the International Exchange Scheme (IE141517). We acknowledge additional support from the STFC Boulby Underground Laboratory in the U.K. the GridPP Collaboration [89,90], in particular at Imperial College London and additional support by the University College London (UCL) Cosmoparticle Initiative. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. The University of Edinburgh is a charitable body, registered in Scotland, with the registration number SC005336. The assistance of SURF and its personnel in providing physical access and general logistical and technical support is acknowledged. Funding Information: We acknowledge additional support from the STFC Boulby Underground Laboratory in the U.K., the GridPP Collaboration [89,90] , in particular at Imperial College London and additional support by the University College London (UCL) Cosmoparticle Initiative. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. The University of Edinburgh is a charitable body, registered in Scotland, with the registration number SC005336. The assistance of SURF and its personnel in providing physical access and general logistical and technical support is acknowledged. Funding Information: The research supporting this work took place in whole or in part at the Sanford Underground Research Facility (SURF) in Lead, South Dakota. Funding for this work is supported by the U.S. Department of Energy, Office of Science, Office of High Energy Physics under Contract Numbers DE-AC02-05CH11231, DE-SC0020216, DE-SC0012704, DE-SC0010010, DE-AC02-07CH11359, DE-SC0012161, DE-SC0014223, DE-FG02-13ER42020, DE-SC0009999, DE-NA0003180, DE-SC0011702, DESC0010072, DE-SC0015708, DE-SC0006605, DE-FG02-10ER46709, UW PRJ82AJ, DE-SC0013542, DE-AC02-76SF00515, DE-SC0018982, DE-SC0019066, DE-AC52-07NA27344 and DOE-SC0012447. This research was also supported by U.S. National Science Foundation (NSF); the U.K. Science & Technology Facilities Council under award numbers, ST/M003655/1, ST/M003981/1, ST/M003744/1, ST/M003639/1, ST/M003604/1, and ST/M003469/1; Portuguese Foundation for Science and Technology (FCT) under award numbers PTDC/FIS-PAR/28567/2017; the Institute for Basic Science, Korea (budget numbers IBS-R016-D1); University College London and Lawrence Berkeley National Laboratory thank the U.K. Royal Society for travel funds under the International Exchange Scheme (IE141517).
PY - 2021/2
Y1 - 2021/2
N2 - The LUX-ZEPLIN dark matter search aims to achieve a sensitivity to the WIMP-nucleon spin-independent cross-section down to (1–2)×10−12 pb at a WIMP mass of 40 GeV/c2. This paper describes the simulations framework that, along with radioactivity measurements, was used to support this projection, and also to provide mock data for validating reconstruction and analysis software. Of particular note are the event generators, which allow us to model the background radiation, and the detector response physics used in the production of raw signals, which can be converted into digitized waveforms similar to data from the operational detector. Inclusion of the detector response allows us to process simulated data using the same analysis routines as developed to process the experimental data.
AB - The LUX-ZEPLIN dark matter search aims to achieve a sensitivity to the WIMP-nucleon spin-independent cross-section down to (1–2)×10−12 pb at a WIMP mass of 40 GeV/c2. This paper describes the simulations framework that, along with radioactivity measurements, was used to support this projection, and also to provide mock data for validating reconstruction and analysis software. Of particular note are the event generators, which allow us to model the background radiation, and the detector response physics used in the production of raw signals, which can be converted into digitized waveforms similar to data from the operational detector. Inclusion of the detector response allows us to process simulated data using the same analysis routines as developed to process the experimental data.
UR - http://www.scopus.com/inward/record.url?scp=85091764386&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85091764386&partnerID=8YFLogxK
U2 - 10.1016/j.astropartphys.2020.102480
DO - 10.1016/j.astropartphys.2020.102480
M3 - Article
AN - SCOPUS:85091764386
VL - 125
JO - Astroparticle Physics
JF - Astroparticle Physics
SN - 0927-6505
M1 - 102480
ER -