XMASS Projects. Hiroyuki Sekiya. ICRR & Kavli-IPMU, University of Tokyo. for the XMASS Collaboration
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1 XMASS Projects Hiroyuki Sekiya ICRR & Kavli-IPMU, University of Tokyo for the XMASS Collaboration Aug st International Conference on Supersymmetry and Unification of Fundamental Interactions (SUSY2013)
2 Introduction Recent physics results From 2012 commissioning run Light WIMP search Phys. Lett. B719 (2013) 78 Solar axion search Phys. Lett. B724 (2013) 46 Current status Detector refurbishment Future prospects XMASS-1.5 Contents SUSY2013 8/29/2013 H. Sekiya 2
3 XMASS Projects Multipurpose low BG experiment with single phase (liquid) Xe Xenon MASSive detector for Solar neutrino (pp/ 7 Be) Xenon neutrino MASS detector (double beta decay) Xenon detector for Weakly Interacting MASSive Particles(DM) neutrinos, axions dark matters, neutrinos The ultimate XMASS Y. Suzuki, hep-ph/ Xe 24t (10t fiducial) Ø 2.5m SUSY2013 8/29/2013 H. Sekiya 3
4 XMASS-1 835kg LXe detector for Dark Matter search 80cm SUSY2013 8/29/2013 H. Sekiya 4
5 Why Single Phase Xe? Simple and Clean for Large Scalability Simplicity Single phase LXe scintillator Simple structure like Super-K Cleanliness Made of pure materials Development of low BG PMTs Xe purification technologies distillation system Xe has the advantage for Spin Independent interacting WIMPs Counts/day/kg/keV Expected WIMP spectrum SUSY2013 8/29/2013 H. Sekiya 5
6 Kamioka Observatory Located underground in Mozumi zinc mine at a 2700 m.w.e. depth. 2km horizontal access by cars Kamioka Tokyo Kyoto Mt. Ikenoyama (1369m) Surface Lab. 1000m Entrance 1800m Underground Lab.s TPC Paris /19/2012 H. Sekiya 6
7 XMASS-1 Detector 10m x φ10m water shield for external BG 1050 kg Liquid Xe within the chamber. Largest mass among DM detectors 642 hexagonal PMTs on 80cm pentakisdodecahedron Construction was completed in Oct 2010 SUSY2013 8/29/2013 H. Sekiya 7
8 Inside of the pentakisdodecahedron Photo coverage is 62.4% SUSY2013 8/29/2013 H. Sekiya 8
9 Clean PMT XMASS PMT HISTORY YEAR Model Prototype R8778 R10789 Material:Body glass Kovar Kovar QE 25% 25% 27-39% RI: w/ PMT base U [mbq/pmt] 50 18±2 0.70±0.28 Th [mbq/pmt] ± ± K [mbq/pmt] ± ± Co [mbq/pmt] < ± ±1.61 Clean PMT Base has also been developed. SUSY2013 8/29/2013 H. Sekiya 9
10 Xe Distillation System Commercial pure Xe contains ~0.1ppm Kr 85 K / K = τ =10.8 year, Q β = 687keV 5 order reduction was indispensable. Astoparticle Physics 31, (2009) 290 Xe Kr Boiling point (@0.2MPa) 178K 140K~150K 4m We established Xe purifiaction by distillation 1 ton LXe = 170 m 3 gas Xe Process speed: 4.7kg/hr 10 days Confirmed Kr < 2.7ppt by API-MS SUSY2013 8/29/2013 H. Sekiya 10
11 Detector Response Top PMT manipulator real data 57 Co simulation Calibration spectrum 59.3keV of W 122keV ~4% rms 136keV Reconstructed vertex real data simulation total photoelectrons Trigger efficiency energy kevee SUSY2013 8/29/2013 Highest LXe scintillation yields: 14.7p.e./keVee Lowest threshold: 4hits 0.3keVee H. Sekiya 11
12 Unexpected BG BG is 2 order higher than that had been expected. counts/day/p.e. Data BG simulation 238U & 210Pb of PMT Al seal expected BG (PMT & components) ~1MeV(60Co peak) total photoelectrons GORE-TEX? ~5keV SUSY2013 8/29/2013 Major origin of BG was considered to be γ from PMTs, but the observed data seemed to have additional surface contamination. Aluminum sealing parts for the PMT (btw metal body and quartz glass) contains 238U and 210Pb (>5keV) GORE-TEX between PMT and holder is suspicious below 5keV. H. Sekiya 12
13 XMASS Full Volume: Low BG w/o PID Although extra BG sources were found, XMASS BG level is still competitive w/o rejecting electronic events. XMASS has a competitive sensitivity to Light WIMPs & Axions Evens/kg/day/keV XMASS full volume kg days Fiducial volume analyses are on-going and will be released. E. Aprile, 2010 Princeton SUSY2013 8/29/2013 H. Sekiya 13
14 Phys. Lett. B719 (2013) 78 Light WIMPs Set an upper limit on the WIMP-nucleon cross section for WIMPs with masses below 20GeV w/o PID and excludes part of the parameter space allowed by DAMA PRL 109, (2012) /kg/kevee/day data σ WIMP-n cm CoGeNT DAMA 5σ 90%CL XMASS Band:Q.F uncertainty CDMS 1 7GeV 12GeV 18GeV [kevee] 2 SUSY2013 8/29/ WIMP mass [GeV/c 2 ] H. Sekiya 14
15 Solar Axions JETP Lett., 95, 379 (2012) A. V. Derbin et al., arxiv: XMASS has also sensitivity to solar axions that would be produced by Bremsstrahlung and Compton effects (g aee ) in the Sun through the axio-electric effect in Xe N.B. Not g aγγ through Primakoff effect Expected flux g aee = SUSY2013 8/29/2013 H. Sekiya 15
16 Phys. Lett. B724 (2013) 46 Solar Axions Same data set as Light WIMP search No indication of signals. Bound in gaee vs. mass. Better than any other constraint in 10-40keV. Better than any other experimental constraint Data Signal MC SUSY2013 8/29/2013 H. Sekiya 16
17 Countermeasures XMASS-1 Refurbishment for Background reduction PMT+Cu surface cleanup Remove GORE-TEX Cover PMT Aluminum seal Cu ring around aluminum seal Electropolished Cu cover above Cu rings SUSY2013 8/29/2013 H. Sekiya 17
18 After Cu ring attachment SUSY2013 8/29/2013 H. Sekiya 18
19 After thin Cu plate attachment SUSY2013 8/29/2013 H. Sekiya 19
20 Almost finished Will resume data taking in this autumn. SUSY2013 8/29/2013 H. Sekiya 20
21 Next step: XMASS-1.5 Inner Ø: 1.5 m contains 5 tons of LXe fiducial mass 1 ton Lessons from XMASS-1 Still Dark matter detector New PMT Flat photocathode cannot catch Plano-concave photocathode can catch SUSY2013 8/29/2013 H. Sekiya 21
22 XMASS-1.5 Actively being developed w/ Hamamatsu Effectiveness is verified by MC SUSY2013 8/29/2013 H. Sekiya 22
23 XMASS projects and timeline XMASS-1-RFB XMASS-1.5 x10 x10 XMASS-2 The ultimatum H. Sekiya 23
24 Conclusion XMASS-1 obtained light WIMP and solar axion result by using 835kg of LXe with very low threshold (0.3keVee) Phys. Lett B 719(2013)78, Phys. Lett B 724 (2013) 46 Initial contamination problems are understood and being addressed. The refurbishment of XMASS-1 is on-going and data taking will resume soon. XMASS-1.5 is planned and the projects move on. SUSY2013 8/29/2013 H. Sekiya 24
25 Extra slides SUSY2013 8/29/2013 H. Sekiya 25
26 Kamioka Observatory, ICRR, Univ. of Tokyo: Y. Suzuki (Spokesperson), M. Nakahata, S. Moriyama, M. Yamashita, Y. Kishimoto, A. Takeda, K. Abe, H. Sekiya, H. Ogawa, K. Kobayashi, K. Hiraide, B. Yang, A. Shinozaki, k. Hieda, O. Takachio, D. Umemoto, N. Oka, K. Nakagawa Kavli-IPMU, University of Tokyo: K. Martens, J.Liu Tokai University: K. Nishijima,F. Kusaba Gifu University: S. Tasaka XMASS Collaboration Yokohama National University: S. Nakamura,I. Murayama,K. Fujii Miyagi University of Education: Y. Fukuda STEL, Nagoya University: Y. Itow, K. Masuda, H. Uchida, Y. Nishitani, H. Takiya Kobe University: Y. Takeuchi, K. Miuchi, O. Yosuke, K. Hosokawa, A. Murata Sejong University: Y.D. Kim, N.Y.Kim Korea Research Institute of Standards and Science (KRISS): Y. H. Kim, M. K. Lee, K. B. Lee, J. S. Lee 42 researchers form 10 institutes SUSY2013 8/29/2013 H. Sekiya 26
27 Pure components More than 250 components RIs of all the components were measured with HPGe and low RI materials were selected. PMT(R10789) 3 HPGe detectors in Kamioka C1020(OFHC) RI: /one PMT Sum of other components RI: Compared w/ SUS304 screws 642 PMTs U 0.70±0.28 mbq Th 1.51±0.31 mbq 40K 9.10±2.15 mbq 60Co 2.92±1.61 mbq SUSY2013 8/29/2013 LEDs H. Sekiya U Th 40K 60Co <35% <35% <20% <20% 27
28 Dark Matter Axion DAMA signal can be explained by electromagnetic interactions of non-relativistic Axions and NaI. [J. Collar, arxiv: ] XMASS has sensitivity to dark matter Axion through Axio-electric effect. g aee /kg/kev/day data g aee Limits on g aee 90%CL XMASS DAMA allowed CoGeNT 2011 CDMS 2009 m a =3keV [kevee] H. Sekiya 28
29 Rn H. Sekiya 29
30 Quenching Factor/Leff uncertainty H. Sekiya 30
31 Energy scale calibration 31
32 Self-shielding for detector material BG High density Xe itself is the shield for γ,n from PMT/OFHC/ 20cm Xe is used for shields Fiducail Volume is 100kg Thicker shield makes lower BG region in center H. Sekiya 32
33 Ex.) Most dirty component : PMT 238 U Chain 1.8mBq/PMT 5cm Original expectation 10cm 20cm Full MC, assuming abs. 100cm, scat. 30cm for photon tracking Counts/day/kg/keV 20cm Xe is used for shield Fiducail Volume is 100kg (Full Volume is 857kg) kev gammas < 10-5 counts/day/kg/kev neutrons < 10-6 counts/day/kg/kev H. Sekiya 33
34 Cable line Calibration line Xe circulation system Gas circulation 30L/min filters gas pump 4 x 180W refrigerator PTR developed by KEK emergency gas pump 100L/min Water tank 800kg 1050kg Condenser 360W evaporator filters 10 m 3 x 2 Outer vacuum liquid pump Liquid circulation 5L/min 700L Liq. Storage gas storage H. Sekiya 34
35 Lab-C Xe Circulation system Water tank LXe tank Distillation Tower Gas Xe tank H. Sekiya 35
36 Water shields for external BG Active for µ, passive for γ,n 10m Ex.) Fast n mine: ( ) x10-5 /cm 2 /sec Assuming all neutron s energies are 10 MeV very conservatively 10 7 n generated 10m y [cm] with 70 PMTs (20 inch) to detect Cerenkov light Water purification system keeps Rn < 1mBq/m 3 water Liq. Xe < 10-4 count/day/kg X [cm] 5m tank is enough large to shield n and γ H. Sekiya 36
37 U chain Th chain GLA2010 3/29/2010 H. Sekiya 37
38 Calibration source rod Calibration System source+holder (Exchangeble) adopter (SUS304) OFHC (C1020) rod Source list Isotopes Energy [kev] intensity [Hz] diameter [mm] (1) Fe (2) Cd , 25, (3) Am (4) Co H. Sekiya 38
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