The XMASS Experiment to search for Dark Matter at the Kamioka Observatory. Status and Results. Kai Martens Kavli IPMU The University of Tokyo
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1 The XMASS Experiment to search for Dark Matter at the Kamioka Observatory Status and Results Kai Martens Kavli IPMU The University of Tokyo
2 Outline - Kavli IPMU: introducing the institute - Dark Matter: setting the stage - Kamioka Observatory: the preeminent underground science laboratory in Japan - XMASS Experiment: - design - status - first results - future plans (if time allows: - Liquid noble gas cleanup... ) 2
3 Kavli IPMU one of the 5 original WPI centers: - founded Oct. 1, first institute in Todias Jan. 11, first Kavli institute in Japan May 10, 2012 best evaluations among WPI centers... 3
4 The Kamioka Observatory: new: KAGRA Super-Kamiokande, (T2K) KamLAND (Xe) Tokyo CANDLES Nagoya XMASS Mo zu mi IPMU Lab 3k m to IPMU Lab: U, Th HP-Ge few 100ppt ICP-MS 1ppq* Kr API-MS 1ppt* * after concentration EGADS NEWAGE CLIO Legend: DM,,, GW4
5 The XMASS Collaboration Kamioka Observatory, ICRR, University of Tokyo: Y. Suzuki, 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 IPMU, University of Tokyo: K. Martens, J.Liu Kobe University: Y. Takeuchi, K. Miuchi, K. Hosokawa, A. Murata, Y.Ohnishi Tokai University: K. Nishijima, F. Kusaba Gifu University: S. Tasaka Yokohama National University: S. Nakamura, I. Murayama, K. Fujii Miyagi University of Education: Y. Fukuda STEL, Nagoya University: Y. Itow, K. Masuda, H. Uchida, H. Takiya Sejong University: Y.D. Kim, N.Y. Kim KRISS: Y.H. Kim, M.K. Lee, K.B. Lee, J.S. Lee 42 collaborators, 10 institutions, 2 countries 5
6 Early Observations: Oort & Zwicky 1932: Jan Oort (Leiden, Netherlands): measures matter in galactic disk near sun from 3 motion of nearby stars: 1M /375ly > 2mstars dark matter Vera Carnegie Institution of Washington: rotation curves of galaxies 1975 AAS meeting 1980 paper 1933: Fritz Zwicky (Caltech, USA): virial theorem: ΣT = ½ ΣU galaxies in Coma cluster too fast for cluster's gravitational potential dark matter 6
7 Galactic Rotation Curves: Vera Rubin apod/ap html: inner part of NGC 2841 by HST vf A: expected curve given luminous matter B: observed Carnegie Institution of Washington: 1975 AAS meeting 1980 paper measured 60 galaxies via gas clouds (H, He) [not stars!] New Scientist (2005/03/19): Michael Brooks: 13 things that do not make sense: Maybe we can't work out what dark matter is because it doesn't actually exist. That's certainly the way Rubin would like it to turn out. "If I could have my pick, I would like to learn that Newton's laws must be modified in order to correctly describe gravitational interactions at large distances," she says. "That's more appealing than a universe filled with a new kind of sub-nuclear particle." 7
8 Dark Matter: It's out there blue: DM, red: hot gas 8
9 So What Are We Looking For? - gravitating: the only thing we know for sure... - cold: massive if particle (cold DM...) - collisionless: no E/M interaction no strong interaction at most: weakly interacting??? New Scientist (2005/03/19): Michael Brooks: 13 things that do not make sense: Maybe we can't work out what dark matter is because it doesn't actually exist. That's certainly the way Rubin would like it to turn out. "If I could have my pick, I would like to learn that Newton's laws must be modified in order to correctly describe gravitational interactions at large distances," she says. "That's more appealing than a universe filled with a new kind of sub-nuclear particle." (Rubin as in: Vera Rubin) favorites are: neutralino, axion, Kaluza-Klein, gravitino 9
10 Dark Matter and the WIMP Miracle WIMP denomination weak interaction... WIMP decoupling after BB: velocity averaged annihilation cross-section for GeV-TeV mass WIMPs: <σv> = cm3/s correct DM density TeV ~ SUSY partners?!? miracle 10
11 WIMP Dark Matter Searches: Direct Detection CDM massive nuclear recoil (NR) 50keVNR ~10keVee calibration sources are γ-sources...(ee) from proceedings Tev06: Search for WIMPs with CDMS and XENON important for verification: different target materials consistency! two types of interaction: - spin dependent (odd isotopes), smaller cross section - spin independent; σ ~ A2 (coherent: whole nucleus) 11
12 The Current Situation: (WIMP hypothesis:) compatible: - spectra: CoGeNT/CRESST-II - modulations: DAMA/CoGeNT tension: - Xe/all of the above - modulation amplitude (halo assumptions...) two regions of experimental focus: - low threshold... - low background... 12
13 The XMASS Experiment Xe detector for weakly interacting MASSive particles Xe -MASS detector Xe MASSive -detector Exploiting Xenon: - high mass number SI cross section - no long-lived radioactive isotope - good scintillation yield: ~ 46ph/keV - high density (liquid): 3g/cm3-48% odd isotopes (natural) SD cross section - ββ candidate: 136Xe 136Ba+2e +2.48MeV Ultimately: 10t fiducial volume multi-purpose detector: - neutrino mass: ββ - Dark Matter: WIMP limited by: - solar neutrinos: pp, 7Be (the water tank in Hall C is designed to hold this...) 13
14 XMASS Progression: the far future: the current incarnation: Phase I 835kg WIMP detector (100kg fiducial), 80cm Ø 24t, + the PAST: 100kg prototype, (3kg fiducial), 30cm proof of principle 100kg reference: arxiv: (10t fiducial) 2.5m detector technology advantages: - simple - scalable - self-shielding the next step: ultimately: 24t (10t fid.) 2.5m Ø 5 ton total, > 1.5ton fiducial 14
15 XMASS Physics: low background speak: Phase II: dru Phase I: 10/25 t (differential rate unit): 100/835 kg multi purpose: sole purpose: DM direct detection: events / day / kg / kev DM direct detection χ + Xe χ + Xe χ + Xe χ + Xe pp and 7Be solar neutrinos: ν + e ν + e expected neutrinoless double-β decay: singal Xe Ba + 2e rates [dru]: 10 4 next proposal: XMASS 1.5 to compete in the next round of DM direct detection: ~1t 10 hep/ph Y. Suzuki 6 χ m=50gev χ m=100gev 2ν2e (2.38x1021y) pp 7 Be 15
16 Background Requirements: WIMPs: 10-4 dru cross sections down to a few times cm2 solar neutrinos: better than 10-5 dru expected rate in 10t: 14/d for pp + 6/d for 7Be important considerations: - go underground (shielding from cosmic rays) - carefully select and monitor your materials for radio isotopes - shield your detector... 16
17 gamma radiation: xenon self-shielding: inner pink circle: fiducial volume also: hall lining Rn retarding Rn- poor outside air supply Shielding Against External Radiation fast neutrons: water tank 11m high (10m water) 10m Ø active: -veto fast Neutron MC: Xe Watertank 17
18 Hall C in Kamioka: XMASS water in tank: 10m high 10m Ø Hall C: 15m,21m,15m (h,d,w) 18
19 XMASS from the Outside In: Inner Detector(ID): 642 PMTs calibration port 1100 kg LXe (total) 835 kg (inside PMTs) 100 kg (fiducial) Outer Detector (OD): 72 x 20inch PMTs (=SK) 19
20 Inner Detector Structure: F I L L E R nd 2 L A Y E R LXe in detector: 1100kg in sensitive volume: 835kg 20
21 Building the Inner Detector 1: 21
22 Building the Inner Detector 2: Feb
23 Low BG PMT Development: BG: biggest worry PMT great development: U < Th< K < Co = 4.47± hexagonal + 12 round) PMTs: Hamamatsu R10789: QE 28-39% + XMASS photocathode coverage: 62.4% 23
24 Electronics: Super-Kamiokande ATM: 12 bit ADC/TDC integration: -100ns +300ns 1.2 μs window new: FADCs CAEN V ch/board bandwidth 500MHz, sampling rate 1GS/s resolution 10bit 1.2 μs window 24
25 Xe Distillation: otherwise: (85) Kr Removal hall C distillation system: extensive materials validation before construction: (used before filling detector) IPMU Lab: U, Th HP-Ge few 100ppt ICP-MS 1ppq* Kr API-MS 1ppt* * after concentration experience: detector stable w/o: - routine getter operation - active Rn removal K.Abe et al, Astroparticle Physics 31(2009), p290 capacity of XMASS Xe distillation system: 6kg/h; did 1 ton in ~ 1 week (3.3±1.1)ppt 25
26 XMASS Calibration System: internal γ calibration for XMASS: - 57Co (122keV) main anchor of energy scale - 241Am (59.5keV), 109Cd (88keV), 55Fe (5.9keV) external (hose) - 60Co, 137Cs - 252Cf neutron calibration (needs FADC) source exchange gate valve 26
27 57 Co Calibration: reconstruction: data MC W (59.3 kev) Co (122 center: data vs. MC Co (136 kev) center position sets energy scale: 14.7 p.e./kevee energy resolution: 4% rms position resolution (rms): center: 1.4 cm ±20cm: 1.0 cm 27
28 Unexpected BG: The Likely Culprits: unexpected BG observed from surface between PMTs: α,β from local materials?! Al seal for PMT window: 238 U and 210Pb (not in secular equilibrium) Gore-Tex (light barrier) under PMT rim: may contain up to 6% modern carbon 28
29 Background and Its Sources 1: higher energies (0.1-3MeV): understood: γ from PMTs consistent w/ge ~1MeV histogram: data MC: 210Pb on Al MC: PMT gammas mid energies (5keV-1MeV): understood: α,β on surface consistent w/ge ~100keV 29
30 Background < 5keV (XMASS design thres.) under study one hypothesis: some 14C in Gore-Tex??? modern carbon in MC: 7.5% next: what assumption about light propagation and generation INSIDE the Gore-Tex material??? shown: two assumptions: both: generation inside LXe filled pores top: 0.3mm att. length bot: 0.1mm att. length black histogram: data MC: 210Pb on Al MC: 14C in Gore-Tex modern carbon measurements: 0 or (6±3)% were measured... 30
31 The Good News: BG (Low), LY high (still optimizing: reduce leakage of surface events into FV) but: XMASS full volume!!! graph (- XMASS...) taken from: E. Aprile (Princton 2010) high light yield (LY) low threshold go for light WIMPs (heavy WIMPs large A large cross section to come) 31
32 Going after the Light WIMPs: cum grano salis: WIMP mass: light heavy 4 hit trigger efficiency: data: 6.75 days with 4 hit threshold full volume 835kg mχ = 7 GeV 0.25keV 0.30keV 32
33 Light WIMPs: Full Volume, Low Threshold our limit: maximally allowed = 835kg cross section: = 6.75 days MC prediction < data playing to our strength: full volume 4 hit threshold backgrounds considered: - no OD activity - no afterpulse activity - Cherenkov ( K in photocathode) - ringing, radioactivity 40 cuts applied: ID trigger only timing RMS < 100ns q(20ns)/q(total) < 0.6 ± Δt > 10ms systematics accounted for: Leff, energy resolution & scale, trigger efficiency, cuts 33
34 Cherenkov Cut Cherenkov light emission in PMT glass (40K, ) Cherenkov photons emitted immediately : timing structure by PMT timing resolution (~3.5ns) scintillation events: time constant τ ~ 25ns (low energy γ and nucl. recoil) cut parameter: charge(first 20ns) charge(total) keep < 0.6 efficiency varies with p.e. range: 40% 70% 34
35 XMASS Full Volume (835kg): Low Mass WIMPs data set: 6.75 days of low threshold data preliminary ID only trigger && RMS of tube timings < 100ns && event timing isolated (±10ms) && Cherenkov cut 35
36 XMASS Result 1: systematic contributions: (in order of importance) - Leff uncertainty * - energy resolution - trigger efficiency - energy scale preliminary - Cherenkov cut * following arxiv (Xe100) 36
37 Annual Modulation Analysis DAMA & DAMA/LIBRA modulation: energy range 2keV 6keV, ~ 1 druee XMASS event 2 kev: ~ 2druee two fits to our data: - straight line - DAMA modulation chi2/ndf
38 XMASS Full Volume (835kg): Pseudoscalar by Axioelectric Effect originally pursued to explain DAMA vs. nucl. recoil; rate: R[kg-1d-1] = A-1g2aēemapσpe photoelectric cross section σ pe ~ 1/v again: conservative limit (max. rate = BG) [simulation for ma = 3keV] preliminary (from astro-ph/ ) coupling constant gaēe dru but: dashed: DAMA (corrected: ) XMASS, CoGeNT, CDMS preliminary Ee [kevee] 38
39 Solar Axions through Axio-Electric: γ production in the sun: - gan: nuclear de-exitation (57Fe, 14.4keV) gaγγ - gaee: Bremsstrahlung, Compton e a gaee e - gaγγ: Primakoff effect γ indirect bound from solar ν flux x detection in XMASS: axio-electric a XMASS solar axion limit: gaee< 4.5x10-11 CoGeNT XMASS DM axion limit CDMS 39
40 Prospects with Fiducialization: solid line: Xenon100 CDMS II dashed: XMASS 5keVee, 100d XMASS 2keVee, 100d high light yield allows lower threshold early MC study: 1 year, 100kg fiducial w/bg ~ 10-4 dru 50 GeV WIMP w/σ χp = 10-44cm2 black: SG, red: BG still working on surface leakage 40
41 Refurbishment: in preparation: - latter half of this year lines of attack: 310mm - Cu surface cleanup electropolish to rm -r U* Th* - light barrier (Cu cover) for PMT Al seal MC study - remove Gore-Tex (presumed guilty until proven innocent ) 41
42 Conclusions XMASS 800kg completed first commissioning phase: - exceptional light yield: 14.7 PE/keVee - still analyzing data (stay tuned...) - backgrounds largely understood preparing for detector refurbishment: - surface cleaning - modification of inter-pmt spaces resume data taking with reduced surface BG & FADC - early next year. Results (so far): light WIMP limit, axio-electric cross section limit more to come stay tuned... also: Starting to plan for 5 ton version of XMASS: XMASS
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