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 Mo CaF2 ﾟﾟ solar detector and ﾟﾟ detector

Liq. scintillator 20 inch PMT Korea Underground Lab. at Cheongpyung

Homyung Mt.

Reservoir

Access tunnel (1.4km) 350m Laboratory (7m ﾗ 8m) KIMS Power plant dark matter experiment 220 cm Future: ~100 kg CsI(Tl) crystal start data taking this year. Workshop for the

cm 1 year data taking would future Underground

140 Confirm or reject the lab. In Korea (Oct. DAMA result 2002). Summary • Because of the variety of physics programme, there are various underground labs. • Many underground labs. have their own future program. This is good, because the requirements to the underground labs depend on the experiments (physics). • In general, deeper site is better as far as backgrounds are concerned. However, required depth depends of the experiment. • For DM and ﾟﾟ experiments, lower n, ? and radon are also important. • There are many factors that characterize the lab., but let me plot…. Summary of the present non-US underground labs. ) 3

Gran Sasso (3 halls)

Super-K

Volume (m Baksan Boulby SNO Kam Baksan LAND Frejus

Cheongpyung Canfranc Europe Oto Canada Asia Depth (m) Possible future non-US underground labs.

Hyper-K UNO-like @Frejus ) 3

Gran Sasso (2 more halls) Volume (m General lab. @SNO Canfranc

Near future ? Far future Depth (m)