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NeSS2002 workshop, Sep.2002, Washington DC Takaaki Kajita, ICRR, U.Tokyo Outline Introduction Status and plans in Europe in Canada in Asia Summary Many thanks to: A.Bettini, L.Mosca, N.Spooner, A.Morales, D.Sinclair, S.K. Kim, K.Kuroda, T.Kishimoto Apology: Some underground labs (especially those related to geosciences, dark matter, double beta decay or cosmic ray experiments) may not be mentioned. Introduction History of particle/astroparticle physics discoveries by underground experiments year 1950’s Discovery of neutrinos (12 m underground) 1965 Observation of atmospheric neutrinos 1968 Solar neutrino problem 1987 Observation of neutrinos from SN1987A 1988 Atmospheric neutrino anomaly 1989-92 Confirmation of solar neutrino problem 1998 Discovery of neutrino oscillations 2001,2 Solar neutrino oscillation Important scientific results from underground experiments! Much more (neutrinos, p-decay, double beta decay, dark matter…) ! Why underground? : Background However, importance is experiment dependent: VERY important for ) 1 - Solar neutrino exp, year 2 Canfranc (lab3) ｵ flux: - ｷ GNOｵBG = 4% of the signal Boulby 1 106 / ｷ SNO ｵ induced n capture BG (after cuts) = 9% of the signal intensity (m Deeper is better for Atmospheric neutrino exp. Muon p-decay exp. supernova neutrino exp. ﾟﾟ exp. Depth (m.w.e.) Dark Matter exp. Status and Pyhasalmi Lab. plans in Europe Boulby mine Baksan Canfranc Frejus Gran Sasso INFN Gran Sasso National Laboratory •1400 m rock overburden •Flat cross-section •Underground area 18 000 m2 •Support facilities on the surface Scientific programme(1): Neutrino oscillations Neutrinos from CERN (CNGS) Neutrinos from the Sun OPERA GNO Low energy solar neutrino Observe exp with 30ton -decay t Ga. Em: 36tons, Pb: 2ktons ICARUS (600ton ? 3000ton) BOREXINO Real time measurement of 7Be ?. It will start m stop and decay in e soon. (data taken at the surface) Neutrinos from the atmosphere LENS proposal MONOLITH not approved Scientific programme(2) Neutrinos from Supernovae Search for non baryonic dark matter LVD Several complementary 1kton liq experiments scintillator detector Example: DAMA 100kg NaI detector Double beta decay experiments Enriched Ge (Heidelberg-Moscow) Cryogenic techniques (Cuorecino, Nuclear reactions (two accelerators, 40 TeO2) and 400keV) Fusion reactions in the Sun Anomalous screening in metals (LUNA-2) The lab is also used for studies of geology and biology. Occupancy HALL C HALL B MI R&D ICARUS Borexino & HALL A OPERA assembly OPERA LVD DAMA LUNA2 GENIUS? LENS? CUORE(?) CREST2 GNO MIBETA (CUORICINO) HMﾟﾟ HDMS Expansion of the Laboratory 1990. The Italian Parliament approved to build 1. An independent access and exit tunnel(safety) 2. Two new halls 2002. Final approval to proceed with the construction of the safety tunnel. Time for construction: 2 years. Further studies of the Gran Sasso aquifer will be conducted during the excavation of the tunnel in order to finalize the design of new underground halls Canfranc underground lab. (LSC) Many experiments on dark matter and ﾟﾟ 675 m.w.e. 2x10 m2 Program finished 5 m 20 m 2 27 m 2450 m.w.e. 1380 m.w.e 118 m2 Program IGEX finished COSME 2 ROSEBUD ANAIS Canfranc. Pyrenees, 175km from Zaragoza. LSC. Science Programme Double Beta Decay IGEX-2b Enriched 76Ge (6.3 kg). Exposure = 8.87 kg y Mee < (0.3 - 1.1) eV Dark Matter experiments ANAIS Search for annual modulations NaI scintillators (107 kg) Built a prototype: background = 1.2 c/(keV kg d) from ~4 keV to 10 keV ROSEBUD Measure heat and light 3 different bolometers of Ge (67 g), Al2O3 (50 g) and CaWO4 (54 g) in the same radioactive environment IGEX-DM one enriched Ge detector (2.1 kg) Exposure = 80 kg day New facilities under construction (expected completion : 2004) Main objective: Identification of Dark Matter Road tunnel @ 2450 m.w.e. Main hall 15 m Service area 45 m Railway tunnel Possible new experiments: GEDEON (Germanium Detectors in ONe cryostat), NURSE (NUclear Recoil Sensitive Experiment), …. Workshop will be held to discuss experiments in the new lab. (Spring, 2003). The Frejus Underground lab. 1985 1990 In the Fréjus Tunnel at about 6.5 km from both entrances Depth: 1760 m (4800mwe) One main hall: about 30x10x11m3 + 3 secondary:70 m2,18 m2 and 21 m2. Users (including technicians) 100 2002 New support structures on surface approved Science @Frejus underground lab. (Present) Double-beta decay search NEMO-3 100Mo (10 kg) inside a large tracking calorimeter Expected sensitivity Mee < 250 - 700 meV TGV Measurement of the 2n 2b-decay of 48Ca (20 g) Dark matter search EDELWEISS Measure heat & ionisation 3x320g Ge bolometers 11.7 kgｷ d exposure No evidence. Very sensitive limits published Future plans 20 (then 100) bolometers Low background facility : 14 Ge detetors for various measurements. A Megaton UNO-like detector @Frejus ? A long baseline experiment between CERN and Frejus is considered. 4MW, 2.2GeV SPL (Superconducting Proton Linac) @CERN 130 km UNO-like detector @Frejus UNO (0.6Mton total mass) Physics: Long baseline exp (CP phase meas.) Proton decay Supernova, Solar and Atmospheric neutrino… Boulby Mine Dark Matter Facility The Facility is Operated by the UK Dark Matter Collaboration (UKDMC) 1100m Low activity salt rock (low U & Th) Pure water tank Boulby Mine Dark Matter Facility: Present Three WIMP dark matter search experiments • NAIAD: 46 kg multi- • ZEPLIN 1: 4 kg Liquid • DRIFT 1: Low pressure module NaI scintillation Xe scintillation detector. gas negative ion drift TPC. detector. Operational since Operational since 2001. Installed Aug 2001 - now 2000. running. Boulby Mine Dark Matter Facility: Future Expanding Surface & Underground Facilities • New (2002) dedicated surface building with workshop, laboratory computing & staging facilities. • New (2002) 1500m2 fully More DM Experiments Planned equipped experimental area with • DRIFT II, DRIFT III >500m2 available to new • ZEPLIN II, ZEPLIN III experiments. • ZEPLIN-MAX Other projects proposed or under consideration • OMNIS (Observatory for Multi flavor Neutrino Interactions from Supernovae) • SIREN (Solar neutrino Interactions by Real-time Excitation of Nuclei) • NUMAG (NeUtrino MAGnetic moment) • CASPER DM exp. (Cocktail of Alkali halide Scattering PARticles) CUPP (Center for Underground Physics in Pyhasalmi) Old mining hut Future plan Present room for surface laboratory and offices 95 m 210 m 1440 m 400 m proposed new 660 m underground facility 980 m available underground spaces in the old mine Possible new experiments On going exp: Cosmic ray muon •Neutrino factory far station Proposals: Double beta decay (2288 km from CERN) Multi-muon experiment •Various other exp’s Baksan Neutrino Observatory Experimental facility of INR Experiments BUST (Baksan Underground Scintillator Telescope) @ 850 m.w.e.. atmospheric neutrinos neutrinos from SN Cosmic Ray physics SAGE SAGE @ 4700 m.w.e. Gallium solar neutrino experiment mass = 55 t Future: Experiments on neutrinos, double beta decay, and DM …? Status and plans in Canada SNO-lab. Present SNO-lab. •2000 m rock overburden •Almost flat surface •Support facilities on the surface •Vertical access •Main cavity ~10,000m3 Solar neutrino oscillation ! Future SNO-lab. New exp. Hall (Approved, (15mﾗ60mﾗ15mh) expected completion: 2005) Two major exp’s + … One exp could be: PICASSO DM exp. Low B.G. counting facility (8mﾗ8mﾗ4mh, general purpose facility) Chem. Lab. Future clean SNO cavity boundaries Future: SNO upgrade or completely new exp. + surface facilities (under consideration) Status and plans in Asia Kamioka observatory Cheongpyung undergound lab. Oto Cosmo Obs Kamioka Observatory KamLAND (operated by 100m Tohoku Univ.) Super- Kamiokande XMASS R&D To mine entrance (1.8km from SK) Tokyo Dark Matter exp Plot type GW detectors •1000 m rock overburden •The mine is no more active 20mﾗ20m •Support facilities on the surface 100mﾗ100m (Cryogenic) Scientific programme(1) Aug.2002 ICRR Interuniversity programme: (1),Super-Kamiokande m 42 Reconstruction work going well. SK collab. would like to thank all the supports from the community. Restart experiment with full water by the 39m end of 2002. Scientific programme(2) ICRR Interuniversity programme(2) ?Tokyo Dark Matter experiment ?XMASS R&D Cryogenic Dark Matter XMASS: 10ton exp. (LiF, 8ﾗ20g) fiducial mass liq. Xe detector. Solar neutrino, dark matter, and ﾟﾟ. ? Plot type gravitational wave detectors 20mﾗ20m (program finished) CLIO 100mﾗ100m cryogenic (under construction) Scientific programme(3) ?KamLAND (Operated by Tohoku Univ.) ? KamLAND uses the Kamiokande site. ? The site transferred from ICRR to Tohoku univ. ? However, the old Kamiokande cavity was a little too small. ? Additional excavation (5m deeper). (1kton Liq. Scintillator detector) Long baseline reactor neutrino experiment. Direct test of the LMA solution of the solar neutrino problem Future plan (1) LCGT Large scale Cryogenic Gragitational wave Telescope. LCGT site Kamioka Observatory surface building sensitivity KamLAND 3km Super-K LCGT arms (tunnels) 3km Mine entrance Future plan (2) (or dream?) Hyper-Kamiokande Super-K (Depth: 2700mwe) 8 km Hyper-K (Depth: 1400 – 1900mwe, Not decided yet ) (Tochibora-mine of the Kamioka mining company) Physics: North-south Long baseline exp (CP phase meas.) Candidate About 500 - 600m. place Proton decay Supernova Atmospheric neutrino …… Oto Cosmo Observatory ?Operated by Osaka Univ. (100 km south of Osaka.) 500m ?Relatively low Rn concentration due to the inclined tunnel. Future: Just discussing MOON: CANDLES: CaF2 crystal Multi-ton Multi-ton 100
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