LArTPC and Dark Matter Cristiano Galbiati Princeton University Gran Sasso Science Institute ~ Module of Opportunity for DUNE Workshop Brookhaven National Laboratory November 13, 2019 10−37 XENON1T Migdal ] 2 10−38 S2-only 2019 CRESST-III 2019 −39 10 DarkSide-50 2018 [cm −40 SI 10 σ 10−41 CDMSLite 2017 10−42 DEAP-3600 2017 43 10− DEAP-3600 2019 LUX 2017 −44 10 DarkSide-50 2018 PANDAX-II 2017 10−45 XENON1T 2018 XENON1T Ionization Signals 2019 10−46 10−47 10−48 −49 Dark Matter-Nucleon 10 Neutrino floor on xenon −50 10 −3 −2 −1 2 10 10 10 2 1 10 10 Mχ [TeV/c ] DarkSide-20k at LNGS 20-tonnes fiducial dark matter detector start of operations at LNGS within 2023 200 tonne×year search for dark matter free of instrumental background 20- 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 DS-20kURANIA ARGO Argo at SNOLAB 300-tonnes depleted argon detector start of operations within 2030 3,000 tonne×year search for dark matter free of instrumental background precision measurement of solar neutrinos 10−37 XENON1T Migdal ] 2 10−38 S2-only 2019 CRESST-III 2019 −39 10 DarkSide-50 2018 [cm −40 SI 10 σ 10−41 CDMSLite 2017 10−42 DEAP-3600 2017 43 10− DEAP-3600 2019 SuperCDMS proj. LUX 2017 −44 10 DarkSide-50 2018 PANDAX-II 2017 DarkSide-LM proj. DEAP-3600 proj. 10−45 XENON1T 2018 LZ proj. XENON1T Ionization Signals 2019 10−46 proj. −47 XENONnTt× yr proj. 10 proj. t× yr −48 DarkSide-20kyr 200proj. 10 DARWIN 200t× Argo 3000 −49 Dark Matter-Nucleon 10 Neutrino floor on xenon −50 10 −3 −2 −1 2 10 10 10 2 1 10 10 Mχ [TeV/c ] THE GADMC PROGRAM FOR DARK MATTER SEARCHES • Explore heavy dark matter through the neutrino floor and beyond • Zero instrumental background • Exposure of O(1000 tonne × year) • Solar neutrinos become background: rejection of minimum ionizing background must reach at least one part in 105 • Exploration of directional signal TECHNOLOGICAL ENABLERS • Custom SiPM-based cryogenic photodetectors • Custom 39Ar-depleted liquid argon • ProtoDUNE-like cryostat for hosting detector and active veto LZ backgrounds summary 5.6 tonnes, 1000 days Gamma backgrounds Radon dominates (PMTs, cryostat) are ER backgrounds negligible. pp solar neutrinos, elastic scattering on atomic electrons Coherent neutrino scattering on xenon nuclei Physical Review Letters 121, 111302 (2018) +r<10 cm && 50% loss S2/S1 cut (70d) 14 1 Entries 16213 70 0.9 Integral 1.619e+04 0.8 60 0.7 50 0.6 40 90 0.5 f 0.4 30 0.3 20 0.2 10 0.1 Physical Review D 98, 102006 (2018) 0 0 0 50 100 150 200 250 300 350 400 450 500 S1 [PE] Enter the Age of Urania Renshaw, PNNL LRUA Workshop 2018 10 Gain: 52.68 σb: 2.19 1200 SNR: 24.1 Entries 1000 800 600 400 200 0 0 50 100 150 200 250 300 Amplitude [Arb.Units] 4 m 12 m ArDM The Global DS-20k DarkSide Argon Dark DS-LM DEAP⎬ Matter ⎬Argo MiniCLEAN DarkNoon Collaboration 350 COLLABORATORS ITALY, US, CANADA, BRAZIL, CHINA, FRANCE, GERMANY, POLAND, RUSSIA, SPAIN, UNITED KINGDOM R. Heastie and C. Lefebvre, Proc. Phys. Soc. 76, 180 (1960) Detector Configuration • TPC as of DarkSide-20k, Veto as DUNE cryostat • AAr in veto, UAr+Xe in TPC 6 m • Fiducial mass of 50 t of 136Xe, Xe 20% molar fraction, 136Xe enriched to 90% via Aria technology • 4π SiPM coverage, 0.1ns timing resolution, 0.8% σ resolution • 222Rn reduction and SiPMs’ single photon counting by operation at 87 K, Cherenkov-based discrimination of single and multiple electrons 20 m 4 10 50 cm cut 103 all 238U (Acrylic) keV] 232 × 102 Th (Acrylic) 238U (SiPM) 10 232Th (SiPM) 136 year Xe (2νββ) × 1 222Rn (internal) 137 −1 Xe (cosmgenics) iso 10 38Cl, 40Cl (cosmogenics) 10−2 8B (ν-e scattering) 10−3 10−4 10−5 Events / [tonne −6 10 1000 1500 2000 2500 3000 3500 E [keV] 7 10 DarkNoon DARWIN 6 CUORE-0 10 10 30 GERDA (phase-II, coaxial) yr 5 GERDA (phase-II, BeGe) 10 KamLand-Zen (phase-II, period 1) KamLand-Zen (phase-II, period 2) 10 29 4 yr 10 EXO-200 nEXO (w/o Ba-tagging) 3 JUNO Xe-LS (5 tons) 10 10 28 year / keV] JUNO Xe-LS (50 tons) yr × 102 10 25 10 26 10 27 10 yr yr yr M [mol 1 −1 1010−1 10−2 10−3 10−4 10−5 10−6 10−7 10−8 10−9 B [Events/(keV × mol × year)] THE END.