Sensitivity of future liquid argon dark matter search experiments to core-collapse supernova neutrinos,Journal of Cosmology and Astroparticle Physics

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Sensitivity of future liquid argon dark matter search experiments to core-collapse supernova neutrinos
Journal of Cosmology and Astroparticle Physics ( IF 5.3 ) Pub Date : 2021-03-15 , DOI: 10.1088/1475-7516/2021/03/043
P. Agnes ₁ , S. Albergo _{2,

3} , I.F.M. Albuquerque ₄ , T. Alexander ₅ , A. Alici _{6,

7} , A.K. Alton ₈ , P. Amaudruz ₉ , S. Arcelli _{6,

7} , M. Ave ₄ , I.Ch. Avetissov ₁₀ , R.I. Avetisov ₁₀ , O. Azzolini ₁₁ , H.O. Back ₅ , Z. Balmforth ₁₂ , V. Barbarian ₁₃ , A. BarradoOlmedo ₁₄ , P. Barrillon ₁₅ , A. Basco ₁₆ , G. Batignani _{17,

18} , A. Bondar _{19,

20} , W.M. Bonivento ₂₁ , E. Borisova _{19,

20} , B. Bottino _{22,

23} , M.G. Boulay ₂₄ , G. Buccino ₂₅ , S. Bussino _{26,

27} , J. Busto ₁₅ , A. Buzulutskov _{19,

20} , M. Cadeddu _{21,

28} , M. Cadoni _{21,

28} , A. Caminata ₂₃ , N. Canci ₂₉ , G. Cappello _{2,

3} , M. Caravati ₂₁ , M. Crdenas-Montes ₁₄ , M. Carlini ₃₀ , F. Carnesecchi _{6,

7,

31} , P. Castello _{21,

32} , S. Catalanotti _{16,

33} , V. Cataudella _{16,

33} , P. Cavalcante ₂₉ , S. Cavuoti _{16,

33,

34} , S. Cebrian ₃₅ , J.M. CelaRuiz ₁₄ , B. Celano ₁₆ , S. Chashin ₁₃ , A. Chepurnov ₁₃ , E Chyhyrynets ₁₁ , C. Cical ₂₁ , L. Cifarelli _{6,

7} , D. Cintas ₃₅ , F. Coccetti ₃₁ , V. Cocco ₂₁ , M. Colocci _{6,

7} , E. CondeVilda ₁₄ , L. Consiglio ₂₉ , S. Copello _{22,

23} , J. Corning ₃₆ , G. Covone _{16,

33} , P. Czudak ₃₇ , S. D'Auria ₃₈ , M.D. DaRochaRolo ₃₉ , O. Dadoun ₄₀ , M. Daniel ₁₄ , S. Davini ₂₃ , A. DeCandia _{16,

33} , S. DeCecco _{41,

42} , A. DeFalco _{21,

28} , G. DeFilippis _{16,

33} , D. DeGruttola _{43,

44} , G. DeGuido ₄₅ , G. DeRosa _{16,

33} , M. DellaValle _{16,

34} , G. Dellacasa ₃₉ , S. DePasquale _{43,

44} , A.V. Derbin ₄₆ , A. Devoto _{21,

28} , L. DiNoto ₂₃ , C. Dionisi _{41,

42} , P. DiStefano ₃₆ , G. Dolganov ₄₇ , F. Dordei ₂₁ , L. Doria ₄₈ , M. Downing ₄₉ , T. Erjavec ₅₀ , M. FernandezDiaz ₁₄ , G. Fiorillo _{16,

33} , A. Franceschi ₅₁ , D. Franco ₅₂ , E. Frolov _{19,

20} , N. Funicello _{43,

44} , F. Gabriele ₂₉ , C. Galbiati _{29,

30,

53} , M. Garbini _{7,

31} , P. GarciaAbia ₁₄ , A. Gendotti ₅₄ , C. Ghiano ₂₉ , R.A. Giampaolo _{39,

55} , C. Giganti ₄₀ , M.A. Giorgi _{17,

18} , G.K. Giovanetti ₅₆ , V. GoicoecheaCasanueva ₅₇ , A. Gola _{58,

59} , R. GracianiDiaz ₆₀ , G.Y. Grigoriev ₄₇ , A. Grobov _{47,

61} , M. Gromov _{13,

62} , M. Guan ₆₃ , M. Guerzoni ₇ , M. Gulino _{64,

65} , C. Guo ₆₃ , B.R. Hackett ₅ , A. Hallin ₆₆ , M. Haranczyk ₃₇ , S. Hill ₁₂ , S. Horikawa _{29,

30} , F. Hubaut ₁₅ , T. Hugues ₆₇ , E.V. Hungerford ₁ , An. Ianni _{29,

53} , V. Ippolito ₄₁ , C.C. James ₆₈ , C. Jillings _{69,

70} , P. Kachru _{29,

30} , A.A. Kemp ₃₆ , C.L. Kendziora ₆₈ , G. Keppel ₁₁ , A.V. Khomyakov ₁₀ , S. Kim ₇₁ , A. Kish ₅₇ , I. Kochanek ₂₉ , K. Kondo ₂₉ , G. Korga ₁₂ , A. Kubankin ₇₂ , R. Kugathasan _{39,

55} , M. Kuss ₁₇ , M. Kuźniak ₆₇ , M. LaCommara _{16,

73} , M. Lai _{21,

28,

52} , S. Langrock ₇₀ , M. Leyton ₁₆ , X. Li ₅₃ , L. Lidey ₅ , M. Lissia ₂₁ , G. Longo _{16,

33} , I.N. Machulin _{47,

61} , L. Mapelli ₅₃ , A. Marasciulli ₁₈ , A. Margotti ₇ , S.M. Mari _{26,

27} , J. Maricic ₅₇ , M. Martnez _{35,

74} , A.D. MartinezRojas _{39,

55} , C.J. Martoff ₇₁ , A. Masoni ₂₁ , A. Mazzi _{58,

59} , A.B. McDonald ₃₆ , J. Mclaughlin _{9,

12} , A. Messina _{41,

42} , P.D. Meyers ₅₃ , T. Miletic ₅₇ , R. Milincic ₅₇ , A. Moggi ₁₇ , A. Moharana _{29,

30} , S. Moioli ₄₅ , J. Monroe ₁₂ , S. Morisi _{16,

33} , M. Morrocchi _{17,

18} , E.N. Mozhevitina ₁₀ , T. Mrz ₃₇ , V.N. Muratova ₄₆ , C. Muscas _{21,

32} , L. Musenich _{22,

23} , P. Musico ₂₃ , R. Nania ₇ , T. Napolitano ₅₁ , A. NavrerAgasson ₄₀ , M. Nessi ₂₅ , I. Nikulin ₇₂ , J. Nowak ₇₅ , A. Oleinik ₇₂ , V. Oleynikov _{19,

20} , L. Pagani ₅₀ , M. Pallavicini _{22,

23} , L. Pandola ₆₅ , E. Pantic ₅₀ , E. Paoloni _{17,

18} , G. Paternoster _{58,

59} , P.A. Pegoraro _{21,

32} , K. Pelczar ₃₇ , L.A. Pellegrini ₄₅ , C. Pellegrino _{7,

31} , F. Perotti _{38,

76} , V. Pesudo ₁₄ , E. Picciau _{21,

28} , F. Pietropaolo ₂₅ , C. Pira ₁₁ , A. Pocar ₄₉ , D.M. Poehlmann ₅₀ , S. Pordes ₆₈ , S.S. Poudel ₁ , P. Pralavorio ₁₅ , D. Price ₇₇ , F. Raffaelli ₁₇ , F. Ragusa _{38,

78} , A. Ramirez ₁ , M. Razeti ₂₁ , A. Razeto ₂₉ , A.L. Renshaw ₁ , S. Rescia ₇₉ , M. Rescigno ₄₁ , F. Resnati ₂₅ , F. Retiere ₉ , L.P. Rignanese _{6,

7} , C. Ripoli _{43,

44} , A. Rivetti ₃₉ , J. Rode _{40,

52} , L. Romero ₁₄ , M. Rossi _{22,

23} , A. Rubbia ₅₄ , P. Salatino _{16,

80} , O. Samoylov ₆₂ , E. SnchezGarca ₁₄ , E. Sandford ₇₇ , S. Sanfilippo _{26,

27} , D. Santone ₁₂ , R. Santorelli ₁₄ , C. Savarese ₅₃ , E. Scapparone ₇ , B. Schlitzer ₅₀ , G. Scioli _{6,

7} , D.A. Semenov ₄₆ , B. Shaw ₉ , A. Shchagin ₇₂ , A. Sheshukov ₆₂ , M. Simeone _{16,

80} , P. Skensved ₃₆ , M.D. Skorokhvatov _{47,

61} , O. Smirnov ₆₂ , B. Smith ₉ , A. Sokolov _{19,

20} , A. Steri ₂₁ , S. Stracka ₁₇ , V. Strickland ₂₄ , M. Stringer ₃₆ , S. Sulis _{21,

32} , Y. Suvorov _{16,

33,

47} , A.M. Szelc ₇₇ , R. Tartaglia ₂₉ , G. Testera ₂₃ , T.N. Thorpe _{29,

30} , A. Tonazzo ₅₂ , S. Torres-Lara ₁ , A. Tricomi _{2,

3} , E.V. Unzhakov ₄₆ , G. Usai _{21,

28} , T. VallivilayilJohn _{29,

30} , T. Viant ₅₄ , S. Viel ₂₄ , A. Vishneva ₆₂ , R.B. Vogelaar ₈₁ , M. Wada ₆₇ , H. Wang ₈₂ , Y. Wang ₈₂ , S. Westerdale ₂₁ , R.J. Wheadon ₃₉ , L. Williams ₈₃ , Ma.M. Wojcik ₃₇ , Ma. Wojcik ₈₄ , X. Xiao ₈₂ , C. Yang ₆₃ , Z. Ye ₁ , A. Zani ₂₅ , A. Zichichi _{6,

7} , G. Zuzel ₃₇ , M.P. Zykova ₁₀

Affiliation

Department of Physics, University of Houston, Houston, TX 77204, U.S.A.
INFN Catania, Catania 95121, Italy
Universit of Catania, Catania 95124, Italy
Instituto de Fsica, Universidade de So Paulo, So Paulo 05508-090, Brazil
Pacific Northwest National Laboratory, Richland, WA 99352, U.S.A.
Physics Department, Universit degli Studi di Bologna, Bologna 40126, Italy
INFN Bologna, Bologna 40126, Italy
Physics Department, Augustana University, Sioux Falls, SD 57197, U.S.A.
TRIUMF, 4004 Wesbrook Mall, Vancouver, BC V6T 2A3, Canada
Mendeleev University of Chemical Technology, Moscow 125047, Russia
INFN Laboratori Nazionali di Legnaro, Legnaro (Padova) 35020, Italy
Department of Physics, Royal Holloway University of London, Egham TW20 0EX, U.K.
Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow 119234, Russia
CIEMAT, Centro de Investigaciones Energticas, Medioambientales y Tecnolgicas, Madrid 28040, Spain
Centre de Physique des Particules de Marseille, Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France
INFN Napoli, Napoli 80126, Italy
INFN Pisa, Pisa 56127, Italy
Physics Department, Universit degli Studi di Pisa, Pisa 56127, Italy
Budker Institute of Nuclear Physics, Novosibirsk 630090, Russia
Novosibirsk State University, Novosibirsk 630090, Russia
INFN Cagliari, Cagliari 09042, Italy
Physics Department, Universit degli Studi di Genova, Genova 16146, Italy
INFN Genova, Genova 16146, Italy
Department of Physics, Carleton University, Ottawa, ON K1S 5B6, Canada
, European Organization for Nuclear Research 1211 Geneve 23, Switzerland, CERN
INFN Roma Tre, Roma 00146, Italy
Mathematics and Physics Department, Universit degli Studi Roma Tre, Roma 00146, Italy
Physics Department, Universit degli Studi di Cagliari, Cagliari 09042, Italy
INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
Gran Sasso Science Institute, L'Aquila 67100, Italy
Museo della fisica e Centro studi e Ricerche Enrico Fermi, Roma 00184, Italy
Department of Electrical and Electronic Engineering, Universit degli Studi di Cagliari, Cagliari 09123, Italy
Physics Department, Universit degli Studi “Federico II” di Napoli, Napoli 80126, Italy
INAF Osservatorio Astronomico di Capodimonte, 80131 Napoli, Italy
Centro de Astropartculas y Fsica de Altas Energas, Universidad de Zaragoza, Zaragoza 50009, Spain
Department of Physics, Engineering Physics and Astronomy, Queen's University, Kingston, ON K7L 3N6, Canada
M.Smoluchowski Institute of Physics, Jagiellonian University, 30-348 Krakow, Poland
INFN Milano, Milano 20133, Italy
INFN Torino, Torino 10125, Italy
LPNHE, CNRS/IN2P3, Sorbonne Universit, Universit Paris Diderot, Paris 75252, France
INFN Sezione di Roma, Roma 00185, Italy
Physics Department, Sapienza Universit di Roma, Roma 00185, Italy
Physics Department, Universit degli Studi di Salerno, Salerno 84084, Italy
INFN Salerno, Salerno 84084, Italy
Chemistry, Materials and Chemical Engineering Department “G.Natta”, Politecnico di Milano, Milano 20133, Italy
Saint Petersburg Nuclear Physics Institute, Gatchina 188350, Russia
National Research Centre Kurchatov Institute, Moscow 123182, Russia
Institut fr Kernphysik, Johannes Gutenberg-Universitt Mainz, D-55099 Mainz, Germany
Amherst Center for Fundamental Interactions and Physics Department, University of Massachusetts, Amherst, MA 01003, U.S.A.
Department of Physics, University of California, Davis, CA 95616, U.S.A.
INFN Laboratori Nazionali di Frascati, Frascati 00044, Italy
APC, Universit de Paris, CNRS, Astroparticule et Cosmologie, Paris F-75013, France
Physics Department, Princeton University, Princeton, NJ 08544, U.S.A.
Institute for Particle Physics, ETH Zrich, Zrich 8093, Switzerland
Department of Electronics and Communications, Politecnico di Torino, Torino 10129, Italy
Williams College, Physics Department, Williamstown, MA 01267 U.S.A.
Department of Physics and Astronomy, University of Hawai'i, Honolulu, HI 96822, U.S.A.
Fondazione Bruno Kessler, Povo 38123, Italy
Trento Institute for Fundamental Physics and Applications, Povo 38123, Italy
Universiatat de Barcelona, Barcelona E-08028, Catalonia, Spain
National Research Nuclear University MEPhI, Moscow 115409, Russia
Joint Institute for Nuclear Research, Dubna 141980, Russia
Institute of High Energy Physics, Beijing 100049, China
Engineering and Architecture Faculty, Universit di Enna Kore, Enna 94100, Italy
INFN Laboratori Nazionali del Sud, Catania 95123, Italy
Department of Physics, University of Alberta, Edmonton, AB T6G 2R3, Canada
AstroCeNT, Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences, 00-614 Warsaw, Poland
Fermi National Accelerator Laboratory, Batavia, IL 60510, U.S.A.
SNOLAB, Lively, ON P3Y 1N2, Canada
Department of Physics and Astronomy, Laurentian University, Sudbury, ON P3E 2C6, Canada
Physics Department, Temple University, Philadelphia, PA 19122, U.S.A.
Radiation Physics Laboratory, Belgorod National Research University, Belgorod 308007, Russia
Pharmacy Department, Universit degli Studi “Federico II” di Napoli, Napoli 80131, Italy
Fundacin ARAID, Universidad de Zaragoza, Zaragoza 50009, Spain
Physics Department, Lancaster University, Lancaster LA1 4YB, U.K.
Civil and Environmental Engineering Department, Politecnico di Milano, Milano 20133, Italy
Department of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, U.K.
Physics Department, Universit degli Studi di Milano, Milano 20133, Italy
Brookhaven National Laboratory, Upton, NY 11973, U.S.A.
Chemical, Materials, and Industrial Production Engineering Department, Universit degli Studi “Federico II” di Napoli, Napoli 80126, Italy
Virginia Tech, Blacksburg, VA 24061, U.S.A.
Physics and Astronomy Department, University of California, Los Angeles, CA 90095, U.S.A.
Department of Physics and Engineering, Fort Lewis College, Durango, CO 81301, U.S.A.
Institute of Applied Radiation Chemistry, Lodz University of Technology, 93-590 Lodz, Poland

Future liquid-argon DarkSide-20k and Argo detectors, designed for direct dark matter search, will be sensitive also to core-collapse supernova neutrinos, via coherent elastic neutrino-nucleus scattering. This interaction channel is flavor-insensitive with a high-cross section, enabling for a high-statistics neutrino detection with target masses of ∼50t and ∼360t for DarkSide-20k and Argo respectively. Thanks to the low-energy threshold of ∼0.5 keV_nr achievable by exploiting the ionization channel, DarkSide-20k and Argo have the potential to discover supernova bursts throughout our galaxy and up to the Small Magellanic Cloud, respectively, assuming a 11-M_☉ progenitor star. We report also on the sensitivity to the neutronization burst, whose electron neutrino flux is suppressed by oscillations when detected via charged current and elastic scattering. Finally, the accuracies in the reconstruction of the average and total neutrino energy in the different phases of the supernova burst, as well as its time profile, are also discussed, taking into account the expected background and the detectorresponse.

中文翻译：

未来液态氩暗物质搜索实验对核心坍缩超新星中微子的敏感性

未来的液氩 DarkSide-20k 和 Argo 探测器，专为直接暗物质搜索而设计，通过相干弹性中微子核散射，也将对核心坍缩超新星中微子敏感。该相互作用通道对味道不敏感，具有高横截面，可实现高统计中微子检测，DarkSide-20k 和 Argo 的目标质量分别为~50t 和~360t。由于利用电离通道可实现 ~0.5 keV _nr的低能量阈值，假设 11-M _☉始祖星。我们还报告了对中子化爆发的敏感性，其电子中微子通量在通过带电电流和弹性散射检测时受到振荡的抑制。最后，还讨论了超新星爆发不同阶段的平均和总中微子能量的重建精度及其时间分布，同时考虑了预期的背景和探测器响应。

更新日期：2021-03-15

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