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Katsushi Arisaka, UCLA 1 University of California, Los Angeles Department of Physics and Astronomy [email protected] Katsushi Arisaka 2/24/2012

Katsushi Arisaka - University of California, Los Angelesarisaka/Talks/2012/Arisaka_120224... · 2012. 11. 16. · Katsushi Arisaka, UCLA 1 University of California, Los Angeles Department

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  • Katsushi Arisaka, UCLA 1

    University of California, Los Angeles Department of Physics and Astronomy

    [email protected]

    Katsushi Arisaka

    2/24/2012

  • MAX - Multi-ton Argon & Xenon

    UMass Amherst, Arizona State University, Augustana College, Black Hills State University,

    Coimbra University, Columbia University, Fermilab, University of Houston, INAF, LNG, MIT, University of Münster,

    University of Notre Dame, Princeton University, Rice University, Temple University, UCLA, University of Virginia,

    University of Zürich

    Katsushi Arisaka, UCLA 2 2/24/2012

  • 4m

    Katsushi Arisaka, UCLA 3

    MAX G3 Detector (at DUSEL)

    2 m Xe

    20 ton (10 ton)

    40Ar 70 ton

    (50 ton)

    Katsushi Arisaka, UCLA 3 2/24/2012

  • Roadmap to MAX

    Katsushi Arisaka, UCLA 4

    2012 2013 2014 2015 2016 2017 2018 2019 2020

    XENON100

    G1

    DarkSide50

    Gran Sasso DUSEL

    G3

    Xe 10T

    Ar 50T

    MAX

    (Paul Scovell)

    XENON 1T

    G2

    DarkSide 5T

    (Elena Aprile)

    (Luca Grandi, Frank Calaprice)

    Katsushi Arisaka, UCLA 4 2/24/2012

  • 2/24/2012 Katsushi Arisaka, UCLA 5

    G1 CMSSM

    F-SU(5)

  • 2/24/2012 Katsushi Arisaka, UCLA 6

    G2

    G1 CMSSM

    F-SU(5)

  • 2/24/2012 Katsushi Arisaka, UCLA 7

    G2

    G3

    G1

    Xenon 10 ton-year

    Argon 50 ton-year

    CMSSM

    F-SU(5)

  • (SI) WIMP Energy Spectrum for LXe (Cross Section = 10-45cm2)

    Katsushi Arisaka, UCLA 8

    8 keVr 45 keVr Xenon

    200 GeV

    50 GeV

    100 GeV

    1000 GeV

    500 GeV

    20 GeV

    Katsushi Arisaka, UCLA 8 2/24/2012

  • (SI) WIMP Energy Spectrum for LAr (Cross Section = 10-45cm2)

    Katsushi Arisaka, UCLA 9

    20 GeV

    200 GeV

    50 GeV

    100 GeV

    1000 GeV

    500 GeV

    200 keVr 40 keVr Argon

    (w/ pulse shaping)

    Katsushi Arisaka, UCLA 9 2/24/2012

  • 1-σ Error of WIMP Mass vs SI Cross Section (10 ton*year Xe and 50 ton*year Ar)

    Katsushi Arisaka, UCLA 10

    50 GeV 100 GeV 200 GeV 500 GeV

    10-45 cm2 Argon

    Xenon

    Katsushi Arisaka, UCLA 10 2/24/2012

  • 1-σ Error of WIMP Mass vs SI Cross Section (10 ton*year Xe and 50 ton*year Ar)

    Katsushi Arisaka, UCLA 11

    50 GeV 100 GeV 200 GeV 500 GeV

    10-45

    10-46

    10-47

    10

    50

    10 50

    Argon

    Xenon

    10-46 cm2

    Katsushi Arisaka, UCLA 11 2/24/2012

  • 1-σ Error of WIMP Mass vs SI Cross Section (10 ton*year Xe and 50 ton*year Ar)

    Katsushi Arisaka, UCLA 12

    Argon (42 events)

    Xenon (56 events)

    100 GeV

    10-45

    10-46

    10-47

    10

    50

    10 50

    10-46 cm2

    Katsushi Arisaka, UCLA 12 2/24/2012

  • 1-σ Error of WIMP Mass vs SI Cross Section (10 ton*year Xe and 50 ton*year Ar)

    Katsushi Arisaka, UCLA 13

    100 GeV

    Argon (4.2 events)

    Xenon (5.6 events)

    10-46

    10-47

    10-48

    10-47 cm2

    10

    50

    10 50

    Katsushi Arisaka, UCLA 13 2/24/2012

  • (SI) WIMP Energy Spectrum for LXe (Cross Section = 10-45cm2)

    Katsushi Arisaka, UCLA 14

    Xenon 8 keVr 45 keVr

    20 GeV

    200 GeV

    50 GeV

    100 GeV

    1000 GeV

    500 GeV

    Katsushi Arisaka, UCLA 14 2/24/2012

    Summer Winter

  • (SI) WIMP Energy Spectrum for LAr (Cross Section = 10-45cm2)

    Katsushi Arisaka, UCLA 15

    Argon

    45 keVr 200 keVr

    20 GeV

    200 GeV

    50 GeV

    100 GeV

    1000 GeV

    500 GeV

    Katsushi Arisaka, UCLA 15 2/24/2012

    Summer Winter

  • ±1σ Error of Annual Modulation Amplitude vs WIMP Mass (10 ton*year Xe and 50 ton*year Ar, Cross Section = 10-45cm2)

    Katsushi Arisaka, UCLA 16

    Argon Xenon

    10-45 cm2

    ±1σ

    ±1σ

    Katsushi Arisaka, UCLA 16 2/24/2012

    10

  • ±1σ Error of Annual Modulation Amplitude vs WIMP Mass (10 ton*year Xe and 50 ton*year Ar, Cross Section = 10-44cm2)

    Katsushi Arisaka, UCLA 17

    Argon Xenon

    10-44 cm2

    Katsushi Arisaka, UCLA 17 2/24/2012

    10

  • ±1σ Error of Annual Modulation Amplitude for various WIMP velocities (50 ton*year Ar, Cross Section = 10-44cm2)

    2/24/2012 Katsushi Arisaka, UCLA 18

    10-44 cm2

    Argon

    170 km/s

    220 km/s

    270 km/s

    V0 =

    195 km/s

    245 km/s

  • Technological Challenges Ø  External Backgrounds

    §  Deep underground – DUSEL 4850 ft §  > 5 m water shielding – Water Tank (15 m)

    Ø  Detector Materials §  Photon Detectors – QUPID §  Cryostat – Titanium §  Others – Copper, PTFE…

    Ø  Purity of Liquid Xe/Ar §  Radon (< 0.3 mBq / ton) §  39Ar (> 100 depletion) – Depleted Ar §  85K (< 0.2 ppt in Xe) – 1 event / 10 ton-year

    Ø  Physics Backgrounds in Xe §  pp-chain solar neutrinos – 1 event / 10 ton-year §  2v Double beta decays from 136Xe – 1 event / 10 ton-year

    Ø  Neutron Active Veto §  Boron doped Liquid Scintillator

    Katsushi Arisaka, UCLA 19 Katsushi Arisaka, UCLA 19 2/24/2012

  • Photo Cathode (-6 kV)

    APD (0 V)

    Quartz

    Quartz

    Al coating

    APD (0 V)

    Photo Cathode (-6 kV)

    QUPID (QUartz Photon Intensifying Detector)

    20 Katsushi Arisaka, UCLA

    arXiv:1103.3689

    Katsushi Arisaka, UCLA 20 2/24/2012

  • Comparison of Low-radioactive Photon Detectors from Hamamatsu

    QUPID 3 inch

    R8520 1 inch

    R8778 2 inch

    XENON10 XENON100

    LUX (XMASS)

    DarkSide50 XENON1T MAX, XAX

    < 0.3 mBq ~ 10 mBq ~ 1 mBq

    2/24/2012 Katsushi Arisaka, UCLA 21

  • QE of two types of QUPID

    22 Katsushi Arisaka, UCLA

    0

    10

    20

    30

    40

    150 200 250 300 350 400 450 500 550 600

    Qua

    ntum

    Effi

    cien

    cy [%

    ]

    Wavelength [nm]

    Xenon type

    Argon type

    Xenon (178 nm) Argon + TPB (420 nm)

    Katsushi Arisaka, UCLA 22 2/24/2012

  • 1, 2 and 3 PE Distribution with 2 m cable

    Katsushi Arisaka, UCLA 23

    2 PE

    3 PE

    1 PE

    G = 800 × 200 = 160,000

    TTS = 160 ps (FWHM)

    Katsushi Arisaka, UCLA 23 2/24/2012

  • 7 QUPID with Holder

    Tested in both Xe and Ar at UCLA Ready for DarkSide 10 2/24/2012 Katsushi Arisaka, UCLA 24

  • Katsushi Arisaka, UCLA 25

    0.81 n / year

    Before Cuts 1/8

    Multi Hit Cut

    0.10 n / year

    1/4

    0.03 n / year

    Liquid Scinti. Veto

    Xe 10 ton Neutron Background (100 Years)

    Xenon 10 ton

    arXiv:1107.1295

    Katsushi Arisaka, UCLA 25 2/24/2012

  • Katsushi Arisaka, UCLA 26

    42 n / year 2.1 n / year 0.39 n / year

    1/20 1/6 Multi Hit Cut Liquid Scinti. Veto Before Cuts

    Argon 50 ton

    Ar 50 ton Neutron Background (100 Years) arXiv:1107.1295

    Katsushi Arisaka, UCLA 26 2/24/2012

  • XAX (Xenon-Argon-Xenon)

    Katsushi Arisaka, UCLA 27

    4 m

    129/131Xe 12 ton (6 ton)

    40Ar 70 ton

    (50 ton)

    WIMP (Spin odd) pp Solar Neutrino

    WIMP (Spin even) Double Beta Decay WIMP (Spin even)

    2 m

    136Xe 7 ton

    (4 ton)

    1.2 m

    arXiv:0808.3968

    2/24/2012

  • (1022 yrs)

    0ν DBD (1027 yrs)

    0 cm

    10 cm

    30 cm

    20 cm

    B8 Solar Neutrino

    40 cm 50 cm

    2ν DBD (2 x 1021 yrs)

    136Xe Double Beta Decay and Gamma Background (1 mBq / QUPID, 2m Xenon Detector)

    Katsushi Arisaka, UCLA 28 2/24/2012

  • Double Beta Decay Experiments (with 0.1 mBq QUPID)

    Katsushi Arisaka, UCLA 29

    EXO 1Ton

    EXO200

    NEMO3 (Mo)

    NEMO3 (Se)

    Mass (kg)

    No.

    of B

    ackg

    roun

    ds (/

    year

    )

    Cuoricino

    GERDA I

    GERDA II

    GERDA III Super-NEMO (Se)

    CUORE I

    CUORE II

    CUORE III

    COBRA

    CANDLES III

    EXO 1Ton (Ba tag)

    1025 yrs 1026 yrs 1027 yrs 1028 yrs

    XAX (Enriched)

    XAX (Natural)

    XENON1T

    2/24/2012

  • 2/24/2012 Katsushi Arisaka, UCLA 30

    Water Tank

    Liquid Scinti

    Water Tank

    Xe 20 ton (10 ton) 40Ar 70 ton (50 ton)

    15 m 6 m

    Liquid Scinti

    Xe Ar

    MAX G3 Detector (at DUSEL)

  • MAX G3 Detector (at DUSEL)

    Katsushi Arisaka, UCLA 31

    Xe 20 ton

    (10 ton)

    40Ar 70 ton

    (50 ton) 2/24/2012

  • Schedule at DUSEL

    Katsushi Arisaka, UCLA 32

    Kevin Lesko

    2/24/2012

  • US Dark Matter Programs

    Katsushi Arisaka, UCLA 33

    G3 = Xe (10T) + Ar (50T)

    2010

    Xe

    Xe

    Ar

    Ar

    2/24/2012

  • Conclusions

    Ø MAX § 10 Ton Xe + 50 Ton Ar at DUSEL § Joint efforts by XENON and DarkSide

    collaborations (currently at LNGS towards G2)

    Ø Science cases § Sensitivity down to 10-48 cm2 § Precision measurements if > 10-46 cm2 § Possibility to combine with 0v Double Beta

    Decays à XAX

    Katsushi Arisaka, UCLA 34 2/24/2012