Katsushi Arisaka, UCLA
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XAX (Xenon-Argon-Xenon) The Ultimate Multi-Purpose Detector for Dark Matter, Double Beta Decay and Solar Neutrino Katsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu 2008/5/14 Katsushi Arisaka 1 Outline ¾ Status of Dark Matter Search Scientific Motivation Experimental Status – CDMS, XENON10, DAMA/LIBRA DUSEL ¾ XAX Detector Concept Why three targets? QUPID (Quartz Photon Intensifying Detector) ¾ Physics Sensitivity WIMP Double Beta Decay Solar Neutrino 2008/5/14 Katsushi Arisaka, UCLA 2 Status of Dark Matter Search 2008/5/14 Katsushi Arisaka 3 Unification of Forces Planck Epoch 100 GeV 1016 GeV 1029 2008/5/14 Katsushi Arisaka,UCLA 1019 GeV 1032 4 Hubble Deep Field Physicists’ View of Early Universe Fiat lux Let there be light 2008/5/14 Katsushi Arisaka,UCLA 5 Hubble Deep Field Physicists’ View of Early Universe Lorentz Invariance Local Gauge Invariance 2008/5/14 Katsushi Arisaka,UCLA 6 Brain 100 Billions Neurons 2008/5/14 Universe 100 Billions Galaxies Katsushi Arisaka,UCLA New York Times 8/21/2006 7 Symmetry Breaking Time 0 1B years Simple 2 3 5 6 7 8 Symmetry Break Down 9 b + s µ- W γ νe τ+ o d -cν d e+ Z τe- e u u νµ b νµ W+µ+c s 4 10 11 12 13 14 2008/5/14 Complex Katsushi Arisaka,UCLA 8 The Five Largest Mysteries in Nature Time 0 1B years 2 3 Origin of Universe Big Bang! First Galaxy formed LHC (CMS) Origin of Particles Origin of Structure 4 Dark Matter (Pierre-Auger, XAX) 5 6 7 8 9 10 11 12 13 14 2008/5/14 Solar System formed First life on the Earth Eukaryotic Cell Plants, Fish… Homo sapiens Origin of Life High-speed Microscope We were born. Katsushi Arisaka Human Brain 9 Installing muon Detectors CMS Endcap Muon Chambers 2008/5/14 Katsushi Arisaka,UCLA 10 Ultra High-speed Movie of Single Neutron 2008/5/14 Katsushi Arisaka,UCLA 11 “Fossils” from the Earliest Universe Time (sec) Temp. Energy oK) (GeV) ( 10-45sec 18 1030 10 10-40 1015 10-35 10-30 1025 10-25 10-20 Planck GUT The Big Bang! Gravitational Wave GUT Particle (Super Heavy Dark Matter) 1012 109 1020 Decoupling of “Fossils” 1PeV 10-15 10-10 1015 1TeV 1GeV 10-5 1010 1MeV 105 sec 1 year 105 103 106 109 year 1 1KeV 1 2008/5/14 EW Neutralino (Cold Dark Matter) Relic Neutrino (Hot Dark Matter) 1eV 10-3eV Now Katsushi Arisaka,UCLA 12 What is Dark Matter? 2008/5/14 Katsushi Arisaka 13 Pierre-Auger Photon Limit Fraction Limit Flux Limit Super Heavy Dark Matter New Limit by Pierre-Auger 12/05/2007 Katsushi Arisaka, UCLA 14 Future WIMP Searches XAX 2008/5/14 Katsushi Arisaka 15 Detection Technique 2008/5/14 Katsushi Arisaka 16 Double-Phase Noble Liquids 2008/5/14 Katsushi Arisaka,UCLA 17 XENON10 Detector 2008/5/14 Katsushi Arisaka 18 XENON10 Detector 2008/5/14 Katsushi Arisaka 19 XENON10 Final Cuts 2008/5/14 Katsushi Arisaka 20 CDMS-II 5 Towers in Soudan x 136 days 2008/5/14 Katsushi Arisaka, UCLA 21 CDMS-II New Results 2008/5/14 Katsushi Arisaka, UCLA 22 XENON100 Expected Sensitivity CDMS II XENON10 2008/5/14 Katsushi Arisaka, UCLA 23 DAMA/LIBRA •25 x 9.7 kg NaI(Tl) ~ 250 kg total in a 5x5 matrix 2008/5/14 24 DAMA/LIBRA New Results 2008/5/14 Katsushi Arisaka, UCLA 25 XENON100 Expected Sensitivity DAMA CDMS II XENON10 2008/5/14 Katsushi Arisaka, UCLA 26 DUSEL (Deep Underground Science and Engineering Laboratory) 2008/5/14 Katsushi Arisaka, UCLA 27 DUSEL: US DEEP LAB 2008/5/14 28 2008/5/14 29 XAX Detector Concepts 2008/5/14 Katsushi Arisaka, UCLA 30 XAX (Xenon-Argon-Xenon) Water Tank Veto WIMP (Spin odd) Solar Neutrino 129/131Xe 19 ton (10 ton) 2m WIMP (Spin even) 40Ar 70 ton (50 ton) 4m 10 m WIMP (Spin even) Double Beta Decay 132/134/136Xe 19 ton (10 ton) 2m 10 m 14 m 2008/5/14 Katsushi Arisaka 31 Properties of Noble Liqud Z A Liquid Density Energy Loss (dE/dX) Radiation Length Collision Length Boiling Temperature Scintillation Wavelength Scintillation Ionization Decay time (Fast Component) Decay time (Slow Component) Isotope Price Single Phase Experiments Unit Neon Argon Xenon g/cc MeV/cm cm cm o K nm photon/keV e-/keV nsec nsec 10 20 1.21 1.4 24 80 27.1 85 30 46 19 1500 No $90k 18 40 1.4 2.1 14 80 87.3 125 40 42 7 1600 39 Ar (1 Bq/kg) $2k 54 ~132 3.06 3.8 2.8 34 165 175 46 64 4 22 136 Xe $2-3M CLEAN DEAP, CLEAN XMASS WARP, ArDM, XAX ZEPLIN, LUX, XENON, XAX $ /ton Double Phase Experiments 2008/5/14 Katsushi Arisaka, UCLA 32 Target Mass Dependence of WIMP Cross Section 10-44 cm2 Xe-132 Ar-40 Ge-73 Si-28 Ne-20 2008/5/14 Katsushi Arisaka, UCLA 33 Separation of Odd and Even Spin Xenon 2008/5/14 Katsushi Arisaka 34 Why Multiple Targets? ¾ Systematic Study of Dark Matter Interaction Target mass dependence of Cross section and Energy spectrum • Xenon vs. Argon Spin dependence of Cross section • 129/131Xe (Spin odd) vs. 132/134/136Xe (Spin even) Precise determination of Mass and Cross section ¾ Neutrino-less Double Beda Decay τ > 1028 years by 136Xe ¾ Solar Neutrino 1% measurement of pp chain flux by 129/131Xe. 2008/5/14 Katsushi Arisaka, UCLA 35 XMASS (Single Phase Xenon) 10 ton detector 100kg Prototype 800kg detector With light guide ～30cm ～80cm ～2.5m R&D Dark matter search Multipurpose detector (solar neutrino, bb …) 2008/5/14 Katsushi Arisaka 36 DEAP/CLEAN (Single Phase Ar/Ne) 360 kg Mini-CLEAN 3.6 ton DEAP/CLEAN 2008/5/14 Katsushi Arisaka, UCLA 37 LUX 300 kg (Double phase Xenon) 60 cm 2008/5/14 Katsushi Arisaka 38 WARP 150 kg (Double Phase Argon) 60cm 2008/5/14 Katsushi Arisaka, UCLA 39 XAX (Double Phase Xe/Ar) Liquid Xe (19 ton) or Ar (9 ton) TPB + Resistive Coating (ATO) + Acrylic Vessel Radiation- free Photon Detector (3” QUPID, Total 3950) 2m OFHC (Oxygen-Free High Conductivity Copper) Vacuum Vessel 2008/5/14 Katsushi Arisaka, UCLA 40 Concept of XAX Acrylic Sheet + ITO Coating + TPB Coating 0V -10 kV Gas Xe/Ar -17.5 kV TPB Coating +ATO Coating + Acrylic Sheet +ITO Coating -10 kV Electron Trajectories 2m 20 cm Radiation-free Photon Detectors (QUPID) 175 nm 125 nm Liquid Xe (19 ton), Ar (9 ton) 430 nm Fiducial Volume (Xe 10 ton, Ar 5 ton) -200 kV -10 kV 2m 2008/5/14 Katsushi Arisaka, UCLA TPB Coating + ITO Coating Acrylic Sheet + ITO Coating 41 Equipotential lines and Electron Trajectories ITO (Indium Tin Oxide) Transparent Conductive Coating (~1 kΩ⁄ ) ATO (Antimony Tin Oxide) Transparent Resistive Coating (~ 1 GΩ⁄ ) Electron Trajectories ITO (Indium Tin Oxide) Transparent Conductive Coating (~1 kΩ⁄ ) 2008/5/14 Katsushi Arisaka, UCLA 42 Structure and S2 Detection at the Top 0V QUPID Ultra Bialkali (UBA) Photocathode Thin Platinum Quartz Window -10 kV Acrylic Light Guide 430 nm 5 cm Acrylic Light Guide -10 kV 1 cm 10 kV/cm 5 kV/cm 175 nm / 125 nm Gas Xenon / Argon -17.5kV Field Shaping Wire (-17.5 kV) 1 kV/cm -22.5kV 2008/5/14 ITO (Indium Tin Oxide) (-10 kV) TPB (Tetra-Phenyl- Butadiene) Electron Trajectories Liquid Xenon / Argon Katsushi Arisaka, UCLA 43 Efficiency (%) Emission/Absorption/QE Synthetic Silica (Quartz) (Transmittance) ITO (Indium Tin Oxide) (Transmittance) Acrylic Sheet Plexiglas G-UVT (Transmittance) Argon TPB (Emission) Xenon TPB (Absorption) Ultra Bialkali (QE) Wavelength (nm) 2008/5/14 Katsushi Arisaka 44 Expected No. of Photoelectrons per keV (Abs. Length = 10 m, Scat. Length = 50 cm) PTFE on Side Wall (Reflectivity = 98%) Photon Detectors on Side Wall ~ 1.5 pe/keV 2008/5/14 ~ 3 pe/keV Katsushi Arisaka, UCLA 45 Evolution from XENON10 to XAX 2008/5/14 Katsushi Arisaka, UCLA 46 Beauty of XAX Concept ¾ XAX is ideal as “the flag-ship experiment” at DUSEL. It addresses three major science topics: WIMP, Double Beta Decay and Solar Neutrino Largest detector: > 10 ton Cost is the right scale: ~ $100M ¾ It combines all existing/proposed noble liquid experiments into a unified superior experiment. Both Xenon and Argon. Single-phase-like geometry with double-phase TPC. 2008/5/14 Katsushi Arisaka, UCLA 47 Comparison of Detector Size XAX 19 ton (10 ton) XENON1ton 2.7 ton (1 ton) LUX XENON10 XENON100 ZEPLIN-II 15 cm 14cm 170 kg (50 kg) 14 kg (5.4 kg) 31 kg (7.2 kg) 30 cm 2008/5/14 20 cm 300 kg (100 kg) 2m 1m 65 cm 30 cm 30 cm 43 cm 1m Katsushi Arisaka, UCLA 2m 48 XENON100/1Ton Collaboration DOE + NSF NSF NSF Switzerland Katsushi Arisaka David Cline Hanguo Wang UCLA 2008/5/14 Portugal Italy h Katsushi Arisaka, UCLA 49 XENON100 Detector 2008/5/14 Katsushi Arisaka,UCLA 50 XENON100 Detector 2008/5/14 Katsushi Arisaka,UCLA 51 XENON100 Expected Sensitivity DAMA CDMS II XENON10 XENON100 2008/5/14 Katsushi Arisaka, UCLA 52 Dark Matter Experiments XENON10 XENON100 XENON 1ton 2008/5/14 XAX (10 ton) 53 XENON 1ton Radiation- free Photon Detector (3” QUPID, Total 968) 1m PTFE Spacer OFHC (Oxygen-Free High Conductivity Copper) Vacuum Vessel 2008/5/14 Katsushi Arisaka, UCLA 54 QUPID (Quartz Photon Intensifying Detector) 2008/5/14 Katsushi Arisaka, UCLA 55 QUPID (Quartz Photon Intensifying Detector) Photo Cathode (-10 kV) Quartz APD (0 V) 3 inch diameter 2008/5/14 Katsushi Arisaka, UCLA 56 13 inch HAPD and PE Distribution Developed by Hamamatsu for T2K and other neutrino experiments. 1 pe 2 pe 3 pe 4 pe 5 pe 2008/5/14 Katsushi Arisaka, UCLA 57 Gain of HAPD Total Gain = 2000 x 10 = 20,000 2008/5/14 Katsushi Arisaka 58 Comparison of Low-radioactive Photon Detectors from Hamamatsu R8520 1 inch XENON10 2008/5/14 XENON100 R8778 2 inch XMASS Katsushi LUXArisaka, UCLA QUPID 3 inch XENON1T XAX 59 Comparison Unit R8520 1 inch Square R8778 2 inch Round QUPID 3 inch Round mm mm cm2 cm2 % 25.7 mm square 21.8 mm square 6.60 4.75 72.0% 57 mm diameter 45 mm diameter 25.52 15.90 62.3% 70 mm diameter 65 mm diameter 38.48 33.18 86.2% 1.51 2.09 1.38 $1,100 $231 $2,700 $170 $3,000 $90 1.11 0.53 25% 35% 1.3 1.3 16% 25% 35% 2.5 1.1 23% 30% 35% 5 1 30% 1.20 1.00 2.00 0.91 1.32 1 0.2 0.2 0.03 50 10 3.1 0.4 1.000 0.100 0.030 0.003 0.020 0.010 0.010 0.008 Size Shape QUPID/R8778 Dimension Outer Size Photo Cathode Total Area Photocathode Area Filling factor Price Price $ Price per potocathode area $/cm2 Performance QE at 175 nm (Typical) % QE at 175 nm (Best) % Peak to Vally Ratio ENF DQE = QE/ENF (Typical) % Radioactivity Total (Typical) mBq Total (Best) mBq Per area (Typical) mBq/cm2 Per area (Best) mBq/cm2 2008/5/14 Katsushi Arisaka 60 Expected Performance of QUPID ¾ Large diameter: 3 inch Existing largest PMT with low radioactivity is 2 inch (R8778) ¾ Extremely low radioactivity: To be compared with << 1 mBq • Hamamatsu R8778 (2 inch) for XMASS: • Hamamatsu R8520 (1 inch) for XENON100: ~10 mBq ~1 mBq ¾ True photon counting 1, 2 … 5 photo-electron peaks are clearly visible. Collection efficiency is ~100% ¾ Simple HV supply HV supply can be common for all HAPD • No tube to tube variation of gains Resister chain not necessary 2008/5/14 Katsushi Arisaka, UCLA 61 Systematic Diagram of XAX Readout XENON1T Detector VME board (6U) Dark Matter ( < 100 keV) Amp X 40 QUPID G=20,000 FADC 500 MHz 12 Bits FPGA Amp X5 FADC 500 MHz 12 Bits HV = -10kV LV = 350 V Double Beta Decay ( < 4 MeV) 8 channel per board Total 242 boards Total 968 QUPIDs 2008/5/14 Katsushi Arisaka, UCLA 62 Physics Sensitivity ¾ Xenon, 2 m Detector (19 ton) WIMP Double Beta Decay Solar Neutrino 2008/5/14 Katsushi Arisaka, UCLA 63 XAX (Double Phase Xe) Liquid Xe (19 ton) TPB + Resistive Coating (ATO) + Acrylic Vessel Radiation- free Photon Detector (3” QUPID, Total 3950) 2m OFHC (Oxygen-Free High Conductivity Copper) Vacuum Vessel 2008/5/14 Katsushi Arisaka, UCLA 64 Energy Spectrum (Natural Xe) 100 GeV WIMP (10-44 cm2) 2ν DBD (1022 yrs) pp Solar Be7 Solar 0ν DBD (1027 yrs) B8 Solar 2008/5/14 Katsushi Arisaka, UCLA 65 Energy Spectrum (Natural Xe) 100 GeV WIMP (10-44 cm2) 0 cm 5 cm 2ν DBD (1022 yrs) 10 cm 20 cm pp Solar 30 cm Be7 Solar 0ν DBD (1027 yrs) B8 Solar 2008/5/14 Katsushi Arisaka, UCLA 66 WIMP Energy Spectrum and Sensitivity 2008/5/14 Katsushi Arisaka, UCLA 67 Gamma Backgrounds after S2/S1 cut (1 mBq / QUPID, 2m Xenon Detector) γ BG (0 cm shield) 100 GeV WIMP (10-44 cm2) γ BG (5 cm shield) 1 TeV 2ν DBD (1022 yrs) pp Solar Neutrino γ BG (10 cm shield) 10 TeV Be7 Solar Neutrino 2008/5/14 Katsushi Arisaka, UCLA 68 Expected Background from Gammas (1 mBq / QUPID, 1 year, Multi Hit Cut, No S2/S1 cut) Xenon (2m) 0.01 γ /10ton-year after S2/S1 cut < 10–8 DRU 10 ton 2008/5/14 Katsushi Arisaka, UCLA 69 Neutron Backgrounds after Multi-hit Cut (1 n/year/QUPID, 2m Xenon Detector) 100 GeV WIMP (10-44 cm2) 1 TeV 10 TeV 0 cm 20 cm 10 cm 30 cm 2008/5/14 Katsushi Arisaka, UCLA 70 Expected Background from Neutrons (1 n/year/QUPID, 10 year, No Multi Hit Cut) Xenon (2m) 10 ton 2008/5/14 Katsushi Arisaka 71 Expected Background from Neutrons (1 n/year/QUPID, 10 year, Multi Hit Cut) Xenon (2m) 0.4 n /10ton-year < 10–8 DRU 10 ton 2008/5/14 Katsushi Arisaka, UCLA 72 Expected No. of WIMP Signals and Backgrounds (10 ton-year of Liquid Xenon, Window = 3 – 15 keVee) No. of Background Events No. of WIMP Signals 10-44 cm2 Gamma (no cut) 10-45 cm2 Gamma (S2/S1 cut) 10-46 cm2 Neutron (no cut) 10-47 cm2 pp-chain Solar (S2/S1 cut) Neutron (multi-hit cut) 10-48 cm2 2-Neutrino DBD (S2/S1 cut) 19.2 ton 14.0 ton 9.8 ton Self Shielding Cut (cm from wall) 2008/5/14 Katsushi Arisaka, UCLA WIMP Mass (GeV) 73 90% CL Sensitivity to the Cross Section (one year, background free) 5-30 keVr 40-130 keVr XENON10 Ar(500 kg) Xe(100 kg) Ar(5 ton) Xe(1 ton) Ar(50 ton) Xe(10 ton) 2008/5/14 Katsushi Arisaka, UCLA 74 Sensitivity to CMSSM (cm2) 10-42 XENON10 10-43 XENON10 10-44 XENON100 10-45 2008/5/14 XENON100 XENON1t 10-46 XENON1t XAX 10-47 XAX Katsushi Arisaka 75 1-CL of WIMP Cross Section and Mass by 100 kg-year of Xenon (10-44 cm2 = 10-8 pb) 1-CL Cross Section (cm2) 10-43 20 GeV 50 GeV 100 GeV 200 GeV 500 GeV 10-44 Blue region: 90% CL 2008/5/14 Katsushi Arisaka, UCLA 76 1-CL of WIMP Cross Section and Mass by 1 ton-year of Xenon (10-44 cm2 = 10-8 pb) 1-CL Cross Section (cm2) 10-43 20 GeV 50 GeV 100 GeV 200 GeV 500 GeV 10-44 Blue region: 90% CL 2008/5/14 Katsushi Arisaka, UCLA 77 1-CL of WIMP Cross Section and Mass by 10 ton-year of Xenon (10-44 cm2 = 10-8 pb) 1-CL Cross Section (cm2) 10-43 20 GeV 50 GeV 100 GeV 200 GeV 500 GeV 10-44 Blue region: 90% CL 2008/5/14 Katsushi Arisaka, UCLA 78 Neutrino-less Double Beta Decay 2008/5/14 Katsushi Arisaka, UCLA 79 Double Beta ββ(0ν) Decay ββ(0ν) : 2n → 2p+2e- p n ΔL = 2 Process ¾ Majorana Neutrino ν = ν ¾ Right-handed current in weak interaction ¾ Majoron emission ¾ SUSY particle exchange e− νM n e− W− p (Qββ ~ MeV) 2008/5/14 Katsushi Arisaka 80 Neutrino Mass Differences Normal Scheme Inverted Scheme (50 meV)2 (9 meV)2 Laurent SIMARD, LAL - Orsay 2008/5/14 Katsushi Arisaka 81 Sensitivity of Neutrinoless Double Beta Decay to Neutrino Mass Normal Scheme DBD Life Time Inverted Scheme 1026 yr 1027 yr 2008/5/14 Cosmology Cosmology Laurent SIMARD, LAL - Orsay 1028 yr (Figure from C. Giunti) Katsushi Arisaka, UCLA 82 136Xe Double Beta Decay and Gamma Background (1 mBq / QUPID, 2m Xenon Detector) 0 cm 2ν DBD (1022 yrs) 10 cm γ BG ~ 10-7 dru FWHM = 50 keV → 5*10-4 /FWHM*kg*year 20 cm 30 cm 40 cm 50 cm 0ν DBD (1027 yrs) B8 Solar 2008/5/14 Katsushi Arisaka, UCLA 83 Expected Background from Gammas (1 mBq / QUPID, 1 year, Multi Hit Cut) 6 γ /year < 10–8 DRU 4.1 ton 2008/5/14 Katsushi Arisaka, UCLA 84 Expected No. of DBD Signals and Backgrounds (10 ton-year of Liquid Xenon, Window = 2479 ± 25 keV) No. of Background Events 19.2 ton 14.0 ton 9.8 ton No. of 0-Neutrino DBD Signals 6.6 ton 4.1 ton Self Shielding Cut (cm from wall) 2008/5/14 Katsushi Arisaka, UCLA Life Time (Year) 85 Double Beta Decay Sensitivities XAX (1 mBq) XAX (0.1mBq) 2008/5/14 136Xe 136Xe 4000 4000 50 50 0.0005 0.00005 Katsushi Arisaka, UCLA ~1027 ~1028 15 – 95 10 – 60 86 Solar Neutrino Detection 2008/5/14 Katsushi Arisaka, UCLA 87 Solar Neutrino M. Nakahata 2008/5/14 Katsushi Arisaka 88 Sular Neutrino Detection M. Yamashita 2008/5/14 Katsushi Arisaka 89 Solar Neutrino Study by XMASS Group M. Nakahata 2008/5/14 Katsushi Arisaka, UCLA 90 Solar Neutrino Energy Spectrum (136 Xe depleted) 100 GeV WIMP (10-44 cm2) pp Solar γ BG (5 cm shield) γ BG (10 cm shield) Be7 Solar 2ν DBD (1022 yrs) 1 TeV γ BG (20 cm shield) 10 TeV 2008/5/14 B8 Solar Katsushi Arisaka, UCLA 91 Expected Background from Gammas (1 mBq / QUPID, 1 year, Multi Hit Cut) 5 γ /10ton-year < 10–8 DRU 10 ton 2008/5/14 Katsushi Arisaka, UCLA 92 Concept of Double Layer XAX Water Tank Veto WIMP (Spin odd) Solar Neutrino WIMP (Spin even) Double Beta Decay WIMP (Spin even) 8m 129/131Xe 10 ton 136Xe 40Ar 10 ton 10 ton 2m 2m 8m 10 m 2008/5/14 Katsushi Arisaka 93 Summary 2008/5/14 Katsushi Arisaka, UCLA 94 Cost (in $M) & Schedule Agency Total FY07 FY08 FY09 FY10 FY11 FY12 FY13 FY14 Gran Sasso XENON100 Total US(DOE) US(NSF) Foreign 1.3 0 1 0.3 0.4 0.9 0.3 0.1 0.7 0.2 XENON1Ton Total US(DOE) US(NSF) Foreign 15 5 5 5 6 2 2 2 6 2 2 2 3 1 1 1 100 30 40 30 1 1 1 0.5 0.5 0.5 0.5 0.5 0.5 DUSEL (4850 ft) XAX Total US(DOE) DUSEL Foreign 2008/5/14 Katsushi Arisaka, UCLA 37 12 15 10 37 12 15 10 23 6 8.5 8.5 95 Detection of Cosmic Radiation Larger Volume Lower Threshold ICECUBE AMANDA Hyper-K Super-K IMB Kamiokande 2010 2000 1990 JEM-EUSO Pierre-Auger HiRes AGASA Cosmic Ray Neutrino XAX XENON1t XENON100 XENON10 CDMS-II Future Dark Matter Ongoing Past Conclusions ¾ XAX incorporates several innovative concepts: Largest detector (> 10 ton) compatible with Argon and Xenon Background free • • • • Radiation-free photon detector: QUPID Thick (20 cm) self shielding Multi-hit cut and S2/S1 cut by double phase TPC Pulse shape discrimination (for Ar) with “reconstructed” S1 signal Best photon collection • 4π coverage of photon detectors (like single phase detectors) ¾ XAX can achieve three important scientific goals: Systematic study of WIMP properties • • • • Sensitivity below 10-47 cm2 at 100 GeV (< 10-46 cm2 at 1 TeV) Determination of Mass and Cross section Target mass (A) dependence of Cross section (Argon vs. Xenon) Spin dependence (129/131Xe vs. 132/134/136Xe) Neutrino-less Double Beta Decay (by 136Xe) • Sensitivity up to 1028 years pp-chain Solar Neutrino (by 129/131Xe) • Flux measurement with 1% statistical error 2008/5/14 Katsushi Arisaka, UCLA 97
