XAX The Ultimate Multi-Purpose Detector for Dark Matter, Double Beta Decay and Solar Neutrino

Transcription

1 2008/5/14 Katsushi Arisaka 1 XAX (Xenon-Argon-Xenon) on) XAX 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

2 2008/5/14 Katsushi Arisaka, UCLA 2 Outline Status of Dark Matter Search Scientific Motivation Experimental Status CDMS, XENON10, DAMA/LIBRA DUSEL XAX Detector Concept Why three targets? QUPID (Quartz Photon Intensifying Detector) Physics Sensitivity WIMP Double Beta Decay Solar Neutrino

3 Status of Dark Matter Search 2008/5/14 Katsushi Arisaka 3

4 2008/5/14 Katsushi Arisaka,UCLA 4 Unification of Forces Planck Epoch 100 GeV GeV GeV

5 2008/5/14 Katsushi Arisaka,UCLA 5 Hubble Deep Field Physicists View of Early Universe Fiat lux Let there be light

6 2008/5/14 Katsushi Arisaka,UCLA 6 Hubble Deep Field Physicists View of Early Universe Lorentz Invariance Local Gauge Invariance

7 Brain Universe 100 Billions Neurons 100 Billions Galaxies New York Times 8/21/ /5/14 Katsushi Arisaka,UCLA 7

8 2008/5/14 Katsushi Arisaka,UCLA 8 Symmetry Breaking Time 0 1B years Simple Symmetry Break Down Complex d b s µ - W + γ d ν c e τ+ Z o τ - ν e u e+ e u ν - µ b ν + µ W + s c

9 The Five Largest Mysteries in Nature Time 0 1B years Big Bang! First Galaxy formed Solar System formed First life on the Earth Eukaryotic Cell Plants, Fish Homo sapiens We were born. LHC (CMS) Origin of Universe Origin of Particles Origin of Structure Dark Matter (Pierre-Auger, XAX) Origin of Life High-speed Microscope Human Brain 2008/5/14 Katsushi Arisaka 9

10 Installing muon Detectors CMS Endcap Muon Chambers 2008/5/14 Katsushi Arisaka,UCLA 10

11 Ultra High-speed Movie of Single Neutron 2008/5/14 Katsushi Arisaka,UCLA 11

12 Fossils from the Earliest Universe Time (sec) Temp. ( sec o K) sec 1 year year 1 Energy (GeV) PeV 1TeV 1GeV 1MeV 1KeV 1eV 10-3 ev Planck GUT EW Now The Big Bang! Gravitational Wave GUT Particle (Super Heavy Dark Matter) Decoupling of Fossils Neutralino (Cold Dark Matter) Relic Neutrino (Hot Dark Matter) 2008/5/14 Katsushi Arisaka,UCLA 12

13 2008/5/14 Katsushi Arisaka 13 What is Dark Matter?

14 12/05/2007 Katsushi Arisaka, UCLA 14 Pierre-Auger Photon Limit Fraction Limit Flux Limit Super Heavy Dark Matter New Limit by Pierre-Auger

15 2008/5/14 Katsushi Arisaka 15 Future WIMP Searches XAX

16 Detection Technique 2008/5/14 Katsushi Arisaka 16

17 2008/5/14 Katsushi Arisaka,UCLA 17 Double-Phase Noble Liquids

18 2008/5/14 Katsushi Arisaka 18 XENON10 Detector

19 2008/5/14 Katsushi Arisaka 19 XENON10 Detector

20 XENON10 Final Cuts 2008/5/14 Katsushi Arisaka 20

21 2008/5/14 Katsushi Arisaka, UCLA 21 CDMS-II 5 Towers in Soudan x 136 days

22 CDMS-II New Results 2008/5/14 Katsushi Arisaka, UCLA 22

23 XENON100 Expected Sensitivity 2008/5/14 Katsushi Arisaka, UCLA 23 CDMS II XENON10

24 2008/5/14 24 DAMA/LIBRA 25 x 9.7 kg NaI(Tl) ~ 250 kg total in a 5x5 matrix

25 DAMA/LIBRA New Results 2008/5/14 Katsushi Arisaka, UCLA 25

26 XENON100 Expected Sensitivity 2008/5/14 Katsushi Arisaka, UCLA 26 DAMA CDMS II XENON10

27 2008/5/14 Katsushi Arisaka, UCLA 27 DUSEL (Deep Underground Science and Engineering Laboratory)

28 DUSEL: US DEEP LAB 2008/5/14 28

29 2008/5/14 29

30 2008/5/14 Katsushi Arisaka, UCLA 30 XAX Detector Concepts

31 2008/5/14 Katsushi Arisaka 31 XAX (Xenon-Argon-Xenon) Water Tank Veto WIMP (Spin odd) Solar Neutrino WIMP (Spin even) WIMP (Spin even) Double Beta Decay 10 m 129/131 Xe 19 ton (10 ton) 40 Ar 70 ton (50 ton) 132/134/136 Xe 19 ton (10 ton) 2 m 4 m 2 m 10 m 14 m

32 Properties of Noble Liqud Unit Neon Argon Xenon Z A ~132 Liquid Density g/cc Energy Loss (de/dx) MeV/cm Radiation Length cm Collision Length cm Boiling Temperature o K Scintillation Wavelength nm Scintillation photon/kev Ionization e-/kev Decay time (Fast Component) nsec Decay time (Slow Component) nsec Isotope No 39 Ar (1 Bq/kg) Price $ /ton $90k $2k $2-3M Single Phase Experiments CLEAN DEAP, CLEAN XMASS 136 Xe Double Phase Experiments WARP, ArDM, XAX ZEPLIN, LUX, XENON, XAX 2008/5/14 Katsushi Arisaka, UCLA 32

33 Target Mass Dependence of WIMP Cross Section 2008/5/14 Katsushi Arisaka, UCLA cm 2 Xe-132 Ar-40 Ge-73 Si-28 Ne-20

34 Separation of Odd and Even Spin Xenon 2008/5/14 Katsushi Arisaka 34

35 2008/5/14 Katsushi Arisaka, UCLA 35 Why Multiple Targets? Systematic Study of Dark Matter Interaction Target mass dependence of Cross section and Energy spectrum Xenon vs. Argon Spin dependence of Cross section 129/131 Xe (Spin odd) vs. 132/134/136 Xe (Spin even) Precise determination of Mass and Cross section Neutrino-less Double Beda Decay τ > years by 136 Xe Solar Neutrino 1% measurement of pp chain flux by 129/131 Xe.

36 XMASS (Single Phase Xenon) 10 ton detector 100kg Prototype 800kg detector With light guide ~30cm R&D ~80cm Dark matter search ~2.5m Multipurpose detector (solar neutrino, bb ) 2008/5/14 Katsushi Arisaka 36

37 2008/5/14 Katsushi Arisaka, UCLA 37 DEAP/CLEAN (Single Phase Ar/Ne) 360 kg Mini-CLEAN 3.6 ton DEAP/CLEAN

38 LUX 300 kg (Double phase Xenon) 2008/5/14 Katsushi Arisaka cm

39 WARP 150 kg (Double Phase Argon) 2008/5/14 Katsushi Arisaka, UCLA 39 60cm

40 2008/5/14 Katsushi Arisaka, UCLA 40 XAX (Double Phase Xe/Ar) Liquid Xe (19 ton) or Ar (9 ton) TPB + Resistive Coating (ATO) + Acrylic Vessel 2 m Radiation- free Photon Detector (3 QUPID, Total 3950) OFHC (Oxygen-Free High Conductivity Copper) Vacuum Vessel

41 2008/5/14 Katsushi Arisaka, UCLA 41 Concept of XAX Gas Xe/Ar 0 V -10 kv kv Electron Trajectories Acrylic Sheet + ITO Coating + TPB Coating TPB Coating +ATO Coating + Acrylic Sheet +ITO Coating 2 m 20 cm 175 nm 125 nm -10 kv Radiation-free Photon Detectors (QUPID) Liquid Xe (19 ton), Ar (9 ton) Fiducial Volume (Xe 10 ton, Ar 5 ton) 430 nm 2 m -200 kv -10 kv TPB Coating + ITO Coating Acrylic Sheet + ITO Coating

42 Equipotential lines and Electron Trajectories 2008/5/14 Katsushi Arisaka, UCLA 42 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 )

43 Structure and S2 Detection at the Top 0 V QUPID -10 kv Ultra Bialkali (UBA) Photocathode Thin Platinum Quartz Window 430 nm Acrylic Light Guide 5 cm Acrylic Light Guide -10 kv 1 cm -17.5kV 10 kv/cm 5 kv/cm 175 nm / 125 nm Gas Xenon / Argon ITO (Indium Tin Oxide) (-10 kv) TPB (Tetra-Phenyl- Butadiene) Field Shaping Wire (-17.5 kv) -22.5kV 1 kv/cm Electron Trajectories Liquid Xenon / Argon 2008/5/14 Katsushi Arisaka, UCLA 43

44 Emission/Absorption/QE Efficiency (%) Argon Synthetic Silica (Quartz) (Transmittance) Xenon Acrylic Sheet Plexiglas G-UVT (Transmittance) ITO (Indium Tin Oxide) (Transmittance) TPB (Emission) TPB (Absorption) Ultra Bialkali (QE) Wavelength (nm) 2008/5/14 Katsushi Arisaka 44

45 Expected No. of Photoelectrons per kev (Abs. Length = 10 m, Scat. Length = 50 cm) 2008/5/14 Katsushi Arisaka, UCLA 45 PTFE on Side Wall (Reflectivity = 98%) Photon Detectors on Side Wall ~ 1.5 pe/kev ~ 3 pe/kev

46 2008/5/14 Katsushi Arisaka, UCLA 46 Evolution from XENON10 to XAX

47 2008/5/14 Katsushi Arisaka, UCLA 47 Beauty of XAX Concept 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 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.

48 2008/5/14 Katsushi Arisaka, UCLA 48 Comparison of Detector Size XAX 19 ton (10 ton) ZEPLIN-II 31 kg (7.2 kg) 14cm XENON10 14 kg (5.4 kg) 15 cm 30 cm XENON kg (50 kg) 65 cm LUX 300 kg (100 kg) 1 m XENON1ton 2.7 ton (1 ton) 2 m 30 cm 20 cm 30 cm 43 cm 1 m 2 m

49 2008/5/14 XENON100/1Ton Collaboration Katsushi Arisaka, UCLA 49 DOE + NSF NSF NSF Switzerland Portugal Italy Katsushi Arisaka David Cline Hanguo Wang UCLA h

50 XENON100 Detector 2008/5/14 Katsushi Arisaka,UCLA 50

51 XENON100 Detector 2008/5/14 Katsushi Arisaka,UCLA 51

52 XENON100 Expected Sensitivity 2008/5/14 Katsushi Arisaka, UCLA 52 DAMA CDMS II XENON10 XENON100

53 Dark Matter Experiments XENON10 XENON100 XENON 1ton XAX (10 ton) 2008/5/14 53

54 XENON 1ton 2008/5/14 Katsushi Arisaka, UCLA 54 Radiation- free Photon Detector (3 QUPID, Total 968) 1 m PTFE Spacer OFHC (Oxygen-Free High Conductivity Copper) Vacuum Vessel

55 2008/5/14 Katsushi Arisaka, UCLA 55 QUPID (Quartz Photon Intensifying Detector)

56 2008/5/14 Katsushi Arisaka, UCLA 56 QUPID (Quartz Photon Intensifying Detector) Photo Cathode (-10 kv) Quartz APD (0 V) 3 inch diameter

57 2008/5/14 Katsushi Arisaka, UCLA inch HAPD and PE Distribution Developed by Hamamatsu for T2K and other neutrino experiments. 1 pe 2 pe 3 pe 4 pe 5 pe

58 2008/5/14 Katsushi Arisaka 58 Gain of HAPD Total Gain = 2000 x 10 = 20,000

59 Comparison of Low-radioactive Photon Detectors from Hamamatsu R inch R inch QUPID 3 inch XENON10 XENON100 XMASS LUX XENON1T XAX 2008/5/14 Katsushi Arisaka, UCLA 59

60 2008/5/14 Katsushi Arisaka 60 Dimension Comparison Unit R8520 R8778 QUPID QUPID/R8778 Size 1 inch 2 inch 3 inch Shape Square Round Round Outer Size mm 25.7 mm square 57 mm diameter 70 mm diameter Photo Cathode mm 21.8 mm square 45 mm diameter 65 mm diameter Total Area cm Photocathode Area cm Filling factor % 72.0% 62.3% 86.2% 1.38 Price Price $ $1,100 $2,700 $3, Price per potocathode area $/cm 2 $231 $170 $ Performance QE at 175 nm (Typical) % 25% 25% 30% 1.20 QE at 175 nm (Best) % 35% 35% 35% 1.00 Peak to Vally Ratio ENF DQE = QE/ENF (Typical) % 16% 23% 30% 1.32 Radioactivity Total (Typical) mbq Total (Best) mbq Per area (Typical) mbq/cm Per area (Best) mbq/cm

61 2008/5/14 Katsushi Arisaka, UCLA 61 Expected Performance of QUPID Large diameter: 3 inch Existing largest PMT with low radioactivity is 2 inch (R8778) Extremely low radioactivity: << 1 mbq To be compared with Hamamatsu R8778 (2 inch) for XMASS: ~10 mbq Hamamatsu R8520 (1 inch) for XENON100: ~1 mbq True photon counting 1, 2 5 photo-electron peaks are clearly visible. Collection efficiency is ~100% Simple HV supply HV supply can be common for all HAPD No tube to tube variation of gains Resister chain not necessary

62 Systematic Diagram of XAX Readout 2008/5/14 Katsushi Arisaka, UCLA 62 XENON1T Detector VME board (6U) Dark Matter ( < 100 kev) Amp X 40 FADC 500 MHz 12 Bits QUPID G=20,000 Amp X 5 FPGA FADC 500 MHz 12 Bits HV = -10kV LV = 350 V Double Beta Decay ( < 4 MeV) Total 968 QUPIDs 8 channel per board Total 242 boards

63 2008/5/14 Katsushi Arisaka, UCLA 63 Physics Sensitivity Xenon, 2 m Detector (19 ton) WIMP Double Beta Decay Solar Neutrino

64 2008/5/14 Katsushi Arisaka, UCLA 64 XAX (Double Phase Xe) Liquid Xe (19 ton) TPB + Resistive Coating (ATO) + Acrylic Vessel 2 m Radiation- free Photon Detector (3 QUPID, Total 3950) OFHC (Oxygen-Free High Conductivity Copper) Vacuum Vessel

65 Energy Spectrum (Natural Xe) 2008/5/14 Katsushi Arisaka, UCLA GeV WIMP (10-44 cm 2 ) 2ν DBD (10 22 yrs) pp Solar Be7 Solar 0ν DBD (10 27 yrs) B8 Solar

66 Energy Spectrum (Natural Xe) 2008/5/14 Katsushi Arisaka, UCLA GeV WIMP (10-44 cm 2 ) pp Solar 2ν DBD (10 22 yrs) 0 cm 5 cm 10 cm 20 cm 30 cm Be7 Solar 0ν DBD (10 27 yrs) B8 Solar

67 WIMP Energy Spectrum and Sensitivity 2008/5/14 Katsushi Arisaka, UCLA 67

68 Gamma Backgrounds after S2/S1 cut (1 mbq / QUPID, 2m Xenon Detector) 2008/5/14 Katsushi Arisaka, UCLA GeV WIMP (10-44 cm 2 ) γ BG (0 cm shield) γ BG (5 cm shield) 1 TeV 2ν DBD (10 22 yrs) 10 TeV pp Solar Neutrino γ BG (10 cm shield) Be7 Solar Neutrino

69 Expected Background from Gammas (1 mbq / QUPID, 1 year, Multi Hit Cut, No S2/S1 cut) 2008/5/14 Katsushi Arisaka, UCLA 69 Xenon (2m) 0.01 γ /10ton-year after S2/S1 cut < 10 8 DRU 10 ton

70 Neutron Backgrounds after Multi-hit Cut (1 n/year/qupid, 2m Xenon Detector) 2008/5/14 Katsushi Arisaka, UCLA 70 1 TeV 100 GeV WIMP (10-44 cm 2 ) 10 TeV 0 cm 20 cm 10 cm 30 cm

71 Expected Background from Neutrons (1 n/year/qupid, 10 year, No Multi Hit Cut) 2008/5/14 Katsushi Arisaka 71 Xenon (2m) 10 ton

72 Expected Background from Neutrons (1 n/year/qupid, 10 year, Multi Hit Cut) 2008/5/14 Katsushi Arisaka, UCLA 72 Xenon (2m) 0.4 n /10ton-year < 10 8 DRU 10 ton

73 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 cm 2 Gamma (no cut) cm 2 Gamma (S2/S1 cut) cm 2 pp-chain Solar (S2/S1 cut) Neutron (no cut) Neutron (multi-hit cut) cm cm 2 2-Neutrino DBD (S2/S1 cut) 19.2 ton 14.0 ton 9.8 ton Self Shielding Cut (cm from wall) WIMP Mass (GeV) 2008/5/14 Katsushi Arisaka, UCLA 73

74 90% CL Sensitivity to the Cross Section (one year, background free) 2008/5/14 Katsushi Arisaka, UCLA kevr kevr XENON10 Ar(500 kg) Ar(5 ton) Ar(50 ton) Xe(100 kg) Xe(1 ton) Xe(10 ton)

75 2008/5/14 Katsushi Arisaka 75 Sensitivity to CMSSM (cm 2 ) XENON XENON10 XENON100 XENON1t XAX XENON100 XENON1t XAX

76 1-CL of WIMP Cross Section and Mass by 100 kg-year of Xenon (10-44 cm 2 = 10-8 pb) 2008/5/14 Katsushi Arisaka, UCLA 76 Cross Section (cm 2 ) GeV 50 GeV 100 GeV 200 GeV 500 GeV 1-CL Blue region: 90% CL

77 1-CL of WIMP Cross Section and Mass by 1 ton-year of Xenon (10-44 cm 2 = 10-8 pb) 2008/5/14 Katsushi Arisaka, UCLA 77 Cross Section (cm 2 ) GeV 50 GeV 100 GeV 200 GeV 500 GeV 1-CL Blue region: 90% CL

78 2008/5/14 1-CL of WIMP Cross Section and Mass by 10 ton-year of Xenon (10-44 cm 2 = 10-8 pb) Katsushi Arisaka, UCLA CL Cross Section (cm 2 ) GeV 50 GeV 100 GeV 200 GeV 500 GeV Blue region: 90% CL

79 Neutrino-less Double Beta Decay 2008/5/14 Katsushi Arisaka, UCLA 79

80 Double Beta ββ(0ν) Decay 2008/5/14 Katsushi Arisaka 80 ββ(0ν) : 2n 2p+2e - p ΔL = 2 Process Majorana Neutrino ν = ν Right-handed current in weak interaction Majoron emission SUSY particle exchange n e ν M n W e p (Q ββ ~ MeV)

81 Neutrino Mass Differences 2008/5/14 Katsushi Arisaka 81 Normal Scheme Inverted Scheme (50 mev) 2 (9 mev) 2 Laurent SIMARD, LAL - Orsay

82 Sensitivity of Neutrinoless Double Beta Decay to Neutrino Mass 2008/5/14 Katsushi Arisaka, UCLA 82 Normal Scheme DBD Life Time Inverted Scheme yr yr Cosmology yr Cosmology Laurent SIMARD, LAL - Orsay (Figure from C. Giunti)

83 136 Xe Double Beta Decay and Gamma Background (1 mbq / QUPID, 2m Xenon Detector) 2008/5/14 Katsushi Arisaka, UCLA 83 0 cm 2ν DBD (10 22 yrs) 10 cm 20 cm 30 cm γ BG ~ 10-7 dru FWHM = 50 kev 5*10-4 /FWHM*kg*year 40 cm 50 cm 0ν DBD (10 27 yrs) B8 Solar

84 Expected Background from Gammas (1 mbq / QUPID, 1 year, Multi Hit Cut) 2008/5/14 Katsushi Arisaka, UCLA 84 6 γ /year < 10 8 DRU 4.1 ton

85 Expected No. of DBD Signals and Backgrounds (10 ton-year of Liquid Xenon, Window = 2479 ± 25 kev) No. of Background Events No. of 0-Neutrino DBD Signals 19.2 ton 14.0 ton 9.8 ton 6.6 ton 4.1 ton Self Shielding Cut (cm from wall) Life Time (Year) 2008/5/14 Katsushi Arisaka, UCLA 85

86 2008/5/14 Katsushi Arisaka, UCLA 86 Double Beta Decay Sensitivities XAX (1 mbq) 136 Xe ~ XAX (0.1mBq) 136 Xe ~

87 Solar Neutrino Detection 2008/5/14 Katsushi Arisaka, UCLA 87

88 2008/5/14 Katsushi Arisaka 88 Solar Neutrino M. Nakahata

89 2008/5/14 Katsushi Arisaka 89 Sular Neutrino Detection M. Yamashita

90 Solar Neutrino Study by XMASS Group 2008/5/14 Katsushi Arisaka, UCLA 90 M. Nakahata

91 Solar Neutrino Energy Spectrum ( 136 Xe depleted) 2008/5/14 Katsushi Arisaka, UCLA GeV WIMP (10-44 cm 2 ) pp Solar γ BG (5 cm shield) γ BG (10 cm shield) Be7 Solar 2ν DBD (10 22 yrs) γ BG (20 cm shield) 1 TeV 10 TeV B8 Solar

92 Expected Background from Gammas (1 mbq / QUPID, 1 year, Multi Hit Cut) 2008/5/14 Katsushi Arisaka, UCLA 92 5 γ /10ton-year < 10 8 DRU 10 ton

93 Concept of Double Layer XAX Water Tank Veto WIMP (Spin odd) Solar Neutrino WIMP (Spin even) Double Beta Decay WIMP (Spin even) 8 m 129/131 Xe 10 ton 136 Xe 10 ton 40 Ar 10 ton 2 m 2 m 8 m 10 m 2008/5/14 Katsushi Arisaka 93

94 Summary 2008/5/14 Katsushi Arisaka, UCLA 94

95 2008/5/14 Katsushi Arisaka, UCLA 95 Cost (in $M) & Schedule Agency Total FY07 FY08 FY09 FY10 FY11 FY12 FY13 FY14 Gran Sasso XENON100 Total US(DOE) 0 US(NSF) Foreign XENON1Ton Total US(DOE) US(NSF) Foreign DUSEL (4850 ft) XAX Total US(DOE) DUSEL Foreign

96 Detection of Cosmic Radiation Larger Volume Lower Threshold Hyper-K Super-K IMB Kamiokande ICECUBE AMANDA Neutrino JEM-EUSO Pierre-Auger HiRes AGASA Cosmic Ray XAX XENON1t XENON100 XENON10 CDMS-II Dark Matter Future Ongoing Past

97 Conclusions 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) XAX can achieve three important scientific goals: Systematic study of WIMP properties Sensitivity below cm 2 at 100 GeV (< cm 2 at 1 TeV) Determination of Mass and Cross section Target mass (A) dependence of Cross section (Argon vs. Xenon) Spin dependence ( 129/131 Xe vs. 132/134/136 Xe) Neutrino-less Double Beta Decay (by 136 Xe) Sensitivity up to years pp-chain Solar Neutrino (by 129/131 Xe) Flux measurement with 1% statistical error 2008/5/14 Katsushi Arisaka, UCLA 97