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Katsushi Arisaka, UCLA 1 University of California, Los Angeles Department of Physics and Astronomy Katsushi Arisaka 2/24/2012.

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Presentation on theme: "Katsushi Arisaka, UCLA 1 University of California, Los Angeles Department of Physics and Astronomy Katsushi Arisaka 2/24/2012."— Presentation transcript:

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

2 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

3 4m Katsushi Arisaka, UCLA 3 MAX G3 Detector (at DUSEL) 2 m Xe 20 ton (10 ton) 40 Ar 70 ton (50 ton) Katsushi Arisaka, UCLA 3 2/24/2012

4 Roadmap to MAX Katsushi Arisaka, UCLA XENON100 G1 DarkSide50 Gran SassoDUSEL 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

5 Katsushi Arisaka, UCLA 5 G1 CMSSM F-SU(5)

6 2/24/2012Katsushi Arisaka, UCLA 6 G2 G1 CMSSM F-SU(5)

7 2/24/2012Katsushi Arisaka, UCLA 7 G2 G3 G1 Xenon 10 ton-year Argon 50 ton-year CMSSM F-SU(5)

8 (SI) WIMP Energy Spectrum for LXe (Cross Section = cm 2 ) 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

9 (SI) WIMP Energy Spectrum for LAr (Cross Section = cm 2 ) Katsushi Arisaka, UCLA 9 20 GeV 200 GeV 50 GeV 100 GeV 1000 GeV 500 GeV 200 keVr40 keVr Argon (w/ pulse shaping) Katsushi Arisaka, UCLA 9 2/24/2012

10 1-σ Error of WIMP Mass vs SI Cross Section (10 ton*year Xe and 50 ton*year Ar) Katsushi Arisaka, UCLA GeV100 GeV200 GeV500 GeV cm 2 Argon Xenon Katsushi Arisaka, UCLA 10 2/24/2012

11 1-σ Error of WIMP Mass vs SI Cross Section (10 ton*year Xe and 50 ton*year Ar) Katsushi Arisaka, UCLA GeV100 GeV200 GeV500 GeV Argon Xenon cm 2 Katsushi Arisaka, UCLA 11 2/24/2012

12 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 cm 2 Katsushi Arisaka, UCLA 12 2/24/2012

13 1-σ Error of WIMP Mass vs SI Cross Section (10 ton*year Xe and 50 ton*year Ar) Katsushi Arisaka, UCLA GeV Argon (4.2 events) Xenon (5.6 events) cm Katsushi Arisaka, UCLA 13 2/24/2012

14 (SI) WIMP Energy Spectrum for LXe (Cross Section = cm 2 ) Katsushi Arisaka, UCLA 14 Xenon 8 keVr45 keVr 20 GeV 200 GeV 50 GeV 100 GeV 1000 GeV 500 GeV Katsushi Arisaka, UCLA 14 2/24/2012 Summer Winter

15 (SI) WIMP Energy Spectrum for LAr (Cross Section = cm 2 ) 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

16 ±1σ Error of Annual Modulation Amplitude vs WIMP Mass (10 ton*year Xe and 50 ton*year Ar, Cross Section = cm 2 ) Katsushi Arisaka, UCLA 16 Argon Xenon cm 2 ±1σ Katsushi Arisaka, UCLA 16 2/24/

17 ±1σ Error of Annual Modulation Amplitude vs WIMP Mass (10 ton*year Xe and 50 ton*year Ar, Cross Section = cm 2 ) Katsushi Arisaka, UCLA 17 Argon Xenon cm 2 Katsushi Arisaka, UCLA 17 2/24/

18 ±1σ Error of Annual Modulation Amplitude for various WIMP velocities (50 ton*year Ar, Cross Section = cm 2 ) 2/24/2012Katsushi Arisaka, UCLA cm 2 Argon 170 km/s 220 km/s 270 km/s V 0 = 195 km/s 245 km/s

19 Technological Challenges  External Backgrounds  Deep underground– DUSEL 4850 ft  > 5 m water shielding– Water Tank (15 m)  Detector Materials  Photon Detectors – QUPID  Cryostat – Titanium  Others – Copper, PTFE…  Purity of Liquid Xe/Ar  Radon(< 0.3 mBq / ton)  39 Ar(> 100 depletion) – Depleted Ar  85 K(< 0.2 ppt in Xe) – 1 event / 10 ton-year  Physics Backgrounds in Xe  pp-chain solar neutrinos – 1 event / 10 ton-year  2v Double beta decays from 136 Xe– 1 event / 10 ton-year  Neutron Active Veto  Boron doped Liquid Scintillator Katsushi Arisaka, UCLA 19 Katsushi Arisaka, UCLA 19 2/24/2012

20 Photo Cathode (-6 kV) APD (0 V) Quartz Al coating APD (0 V) Photo Cathode (-6 kV) QUPID (QUartz Photon Intensifying Detector) 20 Katsushi Arisaka, UCLA arXiv: Katsushi Arisaka, UCLA 20 2/24/2012

21 Comparison of Low-radioactive Photon Detectors from Hamamatsu QUPID 3 inch R inch R inch XENON10 XENON100 LUX (XMASS) DarkSide50 XENON1T MAX, XAX < 0.3 mBq ~ 10 mBq ~ 1 mBq 2/24/2012Katsushi Arisaka, UCLA 21

22 QE of two types of QUPID 22 Katsushi Arisaka, UCLA Xenon (178 nm)Argon + TPB (420 nm) Katsushi Arisaka, UCLA 22 2/24/2012

23 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

24 7 QUPID with Holder Tested in both Xe and Ar at UCLA Ready for DarkSide 10 2/24/2012Katsushi Arisaka, UCLA 24

25 Katsushi Arisaka, UCLA n / year Before Cuts 1/8 Multi Hit Cut 0.10 n / year 1/ n / year Liquid Scinti. Veto Xe 10 ton Neutron Background (100 Years) Xenon 10 ton arXiv: Katsushi Arisaka, UCLA 25 2/24/2012

26 Katsushi Arisaka, UCLA n / year 2.1 n / year0.39 n / year 1/20 1/6 Multi Hit CutLiquid Scinti. VetoBefore Cuts Argon 50 ton Ar 50 ton Neutron Background (100 Years) arXiv: Katsushi Arisaka, UCLA 26 2/24/2012

27 XAX (Xenon-Argon-Xenon) Katsushi Arisaka, UCLA 27 4 m 129/131 Xe 12 ton (6 ton) 40 Ar 70 ton (50 ton) WIMP (Spin odd) pp Solar Neutrino WIMP (Spin even) Double Beta Decay WIMP (Spin even) 2 m 136 Xe 7 ton (4 ton) 1.2 m arXiv: /24/2012

28 (10 22 yrs) 0 DBD (10 27 yrs) 0 cm 10 cm 30 cm 20 cm B8 Solar Neutrino 40 cm 50 cm 2 DBD (2 x yrs) 136 Xe Double Beta Decay and Gamma Background (1 mBq / QUPID, 2m Xenon Detector) Katsushi Arisaka, UCLA 28 2/24/2012

29 Double Beta Decay Experiments (with 0.1 mBq QUPID) Katsushi Arisaka, UCLA 29 EXO 1Ton EXO200 NEMO3 (Mo) NEMO3 (Se) Mass (kg) No. of Backgrounds (/year) Cuoricino GERDA I GERDA II GERDA III Super-NEMO (Se) CUORE I CUORE II CUORE III COBRA CANDLES III EXO 1Ton (Ba tag) yrs yrs yrs10 28 yrs XAX (Enriched) XAX (Natural) XENON1T 2/24/2012

30 Katsushi Arisaka, UCLA 30 Water Tank Liquid Scinti Water Tank Xe 20 ton (10 ton) 40 Ar 70 ton (50 ton) 15 m 6 m Liquid Scinti Xe Ar MAX G3 Detector (at DUSEL)

31 Katsushi Arisaka, UCLA 31 Xe 20 ton (10 ton) 40 Ar 70 ton (50 ton) 2/24/2012

32 Schedule at DUSEL Katsushi Arisaka, UCLA 32 Kevin Lesko 2/24/2012

33 US Dark Matter Programs Katsushi Arisaka, UCLA 33 G3 = Xe (10T) + Ar (50T) 2010 Xe Ar 2/24/2012

34 Conclusions  MAX  10 Ton Xe + 50 Ton Ar at DUSEL  Joint efforts by XENON and DarkSide collaborations (currently at LNGS towards G2)  Science cases  Sensitivity down to cm 2  Precision measurements if > cm 2  Possibility to combine with 0v Double Beta Decays  XAX Katsushi Arisaka, UCLA 34 2/24/2012


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