snolab and its programme - ppd · snolab and its programme nigel smith ... eureca @ lsm...
TRANSCRIPT
N.J.T.Smith STFC RAL 2010 July 2010
SNOLAB and its programmeNigel Smith (plus many others)
N.J.T.Smith STFC RAL 2010 July 2010
OutlineScope of talk:
Focus from the deep underground facilities perspectiveEspecially new/planned expansions to u/ground facilities
Why go underground?BackgroundsBackground suppression
Science questionsStatus update on underground facilities
Europe - Asia - North America SNOLAB
Infrastructure developmentScience programme
N.J.T.Smith STFC RAL 2010 July 2010
Why go underground?
Studies for rare events, either decays (eg proton or 0νββ), low σ measurements or weak interactions (dark matter, natural or generated neutrino), require very radio-quiet environments to undertake searchesDeep underground facilities provide significant rock overburden and commensurate reduction in c.r. flux, and c.r.-spallation induced neutronsReduction in gamma backgrounds from reduction in c.r.s and neutrons
Additional science programmes possible with such infrastructure - extreme biosystems, geology, geophysics, gravitational waves...
10-20
10-18
10-16
10-14
10-12
10-10
10-8
10-6
10-4
1011 1013 1015 1017 1019 1021
Cosmic Ray Energy Spectrum
Proton-4Tien ShenAkenoHaverah ParkYakutskSydney
Inte
nsity
(cm
-2s-1
sr-1)
Cosmic Ray Energy (eV)
Experiment:
1 per square metre per second
1 per square metre per day
1 per square metre per year
1 per square kilometre per year
1 per square metre per century
1 per square kilometre per century
N.J.T.Smith STFC RAL 2010 July 2010
Muon backgrounds
2km rock overburden(6000mwe)
UndergroundLaboratory
SurfaceFacility
Muon Flux = 0.27/m2/day
N.J.T.Smith STFC RAL 2010 July 2010
Neutron backgrounds
Neutron production fromc.r. muon spallationU/Th fissionα, n reactions
Spectrum in laboratory depends on local geology (rock composition)
both for fast and thermal neutronsU/Th + moderatorsmuons + moderatorssmall levels of high neutron cross-section make a big difference
Persiani / Selvi
Kudryavtsev
N.J.T.Smith STFC RAL 2010 July 2010
Gamma Backgrounds
Reduction in gamma background at higher energies from c.r. and neutron reductionBelow 3.5MeV dependent on local geology and rock material
Boulby (red)Gran Sasso (blue)surface (black)
N.J.T.Smith STFC RAL 2010 July 2010
Background Suppressionc.r. µ and n spallation (depth, µ veto, self veto)γ,β (traditional gamma shielding or gamma blind)radon (clean room operations, atmospheric and material selection and radon suppression)U/Th (α,n) in rock and detector materials (shield, veto)Cosmogenics (underground fabrication)gravitational gradient (massive rock bed, away from surface)
SNO+ @ SNOLAB γ in Pb @ Boulby (Carson) EURECA @ LSM (Kudryavtsev)
N.J.T.Smith STFC RAL 2010 July 2010
Dark matter searches
Nuclear astrophysics
Sola
r/SN
neu
trino
Geo/reactor neutrinos
Gravity wave searches
Double beta decay
neutrino
Extrem
e biosphere
s
Geo
logy
, ge
ophy
sics
Long baseline
neutrino oscillation
Prot
on d
ecay
Science questions...
Low neutron background
Low gamma background
FacilityEnvironment
How do stars burn?
What constitutes most of the mass of the Universe?
How do fault slips develop?
Where does the matter-antimatter asymmetry in the Universe come from?
Where does the heat of the Earth
come from?
What is the physics beyond
the standard model?
What is the nature of the
neutrino?
What is the mass, and
mixing parameters, of the neutrino?
How do the most extreme astronomical
events evolve?
How do they explode?
How does life evolve in extreme
environments?
N.J.T.Smith STFC RAL 2010 July 2010
LNGS
1400 m rock overburden (3.2 km w.e.)Flat cross-sectionNeutron flux = 3.8±0.3 10–2 m–2s–1
µ flux = 3 x 10–4 m–2s–1 (angular depend. measured) γ flux= 1 104 m–2s–1
Volume 180 000 m3, area 17 300 m2
Ventilation: 1 lab volume/3.5 hRadon in air 50-120 Bq/m3 (less @ experiments)Support facilities on the surfaceDrive in to the experimentsThe largest international scientific communityPermanent staff = 80 permanent +23
Broad neutrino/NA programme:ν beam from CERN: ICARUS, OPERA, Solar νs: BOREXINO, SuperNOVA νs: LVD,
0νββ: CUORICINO, CUORE, GERDA
Centre for Underground Physics in Pyhäsalmi CUPP. Finland
Neutron flux being measuredPersonnel: 3 on site + 3 @ OuluOffices, labs and guest rooms on surfaceAccess via lifts or inclined road tunnel
Old mine - Operational 1962-2001Cavities available at several levels from 95 m to 980 mLab facilities may be excavated @ 1440 m, 4 km w.e.
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EMMA experiment at 75m depthComposition of atmospheric µ @ kneeDrift chamber and plastic scintillators
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Romanian underground laboratory in Unirea salt mine,
Slanic Prahova-ROMANIA
View of underground laboratory view from Unirea salt mine
The Underground Laboratory for Measurement in Ultra-low Radiation Background is situated in Unirea salt mine, in Slanic Prahova town, in Prahova County, Romania. Slanic town, Prahova County is situated in sub-Carpathians hills, about 100 km N from Bucharest and 150 km SE from Brasov. The town is placed in Slanic River valley, tributary of Varbilau River. In this environment, we have constructed the Low Background Radiation Laboratory situated at a depth of 208 m beneath the surface at water equivalent thickness of ~600 m. This mine consists of a hivelike structure composed of more galleries 32 or 36 meters wide, 52 to 57 m height and hundreds of meter long. Also it must be pointed out the remarkable stability of the microenvironment characterized by a constant temperature all over the years of 120 C and relative humidity of 60 to 65 %.
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The Polkowice-Sieroszowice mine in Poland - one of the sites proposed for LAGUNA and ArDM
The Sieroszowice mine (178 km2 of underground excavation area), belongs to the KGHM holding of copper mines and metallurgic plants - 6th position in the world’s copper production and 2nd position for silver.
Near Wrocław, south-west of Poland - easily accessible from the Wroclaw airport and from the A4 motor-way, 950 km from CERN
Geological cutoff – layers of anhydrite, dolomite and salt rocks at depths from 600 till >1400 m below the surface
Boulby Science Facility• Boulby is a working potash mine in the North East
of England. Operated by Cleveland Potash Ltd – a major local employer.
• 1100m deep (2805 mwe giving ~106 reduction in CR muons).
• Surrounding rock-salt = low activity giving low gamma and radon backgrounds.
Middlesborough
Whitby
Staithes
York
JIF facilities - 2003 .> 1000 m2, fully equipped underground ‘Palmer lab’> Surface support facility.
Boulby Mine
June 2009: New facility manager & science
coordinator Sean Paling
A. Bettini.
600 m2 (40x15x12)
Depth: 800 m
Muons: 0.47 µ x 10-2 m m-2 s-1
Ventilation: 11.000 m3/h
Hall A
Hall B
Hall C
150 m2 (15x10x7)
Experimental halls A, B and C
Operative budget: ≈1600 k€/yr
Completion of the reinstallation of the infrastructure. June 2010
LSM Extension project
Fréjus tunnel
Safety gallery
Present LSM
Extension project
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Univ. of TohokuKamLANDKamLAND
Ge
Super-Kamiokande
Ge!"## $% &'(')(')*!"## $% &'(')(')*++
!"## ,% ''(-(''*!"## ,% ''(-(''*++
New Experimental Hall
Clean roomICP-MSXMASS R&D
HallXMASS, CANDLES
XMASS R&D
N AGE(D k M tt )IPMU Labo.API-MS, Ge
To Atotsuentrance
CLIO (Grav. Wave) 100m Lazer Strain Meter
NewAGE(Dark Matter)Super conductive
Gravity meter
API MS, Ge
Proprietaryarea
17
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=89:(=89:(=+*"& *+)> '? @/(%,"*"0 ') 122A=+*"& *+)> '? @/(%,"*"0 ') 122A
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Korea Middleland Power Co.Yangyang Pumped Storage Power Plant
Yangyang Underground Laboratory
Minimum depth : 700 m / Access to the lab by car (~2km)
Kim
IWD
D09
19
!"
#$"
Kim
IWD
D09
• Jinping Mountain Peak:4193m
• Maximum rock overburden: ~2500m• Length of Jinping transportation tunnel: 17.5km• Rock cover larger than 1500m:>70%
Layout of CJPL and its Phase-I space (red square)
6.5m*6.5m*40m main hall A
The construction of infrastructure of CJPL Phase-1 will be finished in April,2010.The Low background measurement facility will be established in Sept. 2010.
2009, Hall-A cavity OK!
Tunnnel to main hall
Main hall is ready! Electronics Layer and Crane
Painting Radon-proof Layer
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1 Homestake DUSEL
DUSEL Facility Design Advancing Following Interactions with Agencies and Collaborations
• World-Class Facility– Research Campuses
• Surface• 4850 (~4200 mwe)• 7400 (~7100 mwe)• Other Levels and Ramps
– Dual Access to Research Campuses– Best-practices Life Safety Systems
and Programs– Experimental Support Groups– Design Enabling Future Expansion – Project Enabling Participation by Other
Agencies• Suite of Transformational Experiments
– Diverse and Compelling Suite– Integral Education and Outreach Efforts
2 Homestake DUSEL
NSF and DOE Cooperation In Creating DUSEL and its Scientific Program
• Initial NSF Guidance - $750M to include:– DUSEL Facility (our goal is for FY13 construction start)– Diverse and Compelling Suite of Experiments
• Dark Matter Searches• Long Baseline Neutrinos• Proton Decay• Neutrinoless Double Beta Decay• Additional Physics Experiments such as:
– Nuclear Astrophysics– Solar Neutrinos
• Biology, Geology, Engineering Experiments including topics such as:– Geomicrobiology– Fault Rupture and geophysics– Coupled Processes
• DOE Established CD0 for Long Baseline Neutrinos Experiment January 2010– Range established $660 - $940M– Joint oversight group (JOG) meeting regularly (DOE OHEP ,DOE ONP, NSF PHY)
• We anticipate maintaining Sanford Lab science program through DUSEL construction– LUX dark matter and Majorana Demonstrator neutrinoless double beta decay
N.J.T.Smith STFC RAL 2010 July 2010
DUSEL Programme
Current status - Sanford LabExcavation of infrastructure for Majorana underwayLUX surface deployment underwayBeneficial occupancy expected 2011
MREFC Proposal in Dec 2010Decision by Spring 2011Construction starts (T0) by 2013/4Beneficial occupancy of full 4850 and 7400 levels would occur at T0+4 yearse.g. DUSEL DM Community focussed on several third generation target technologies (Ge, Ar, Xe, directional, ...)DIANA nuclear astrophysics, twin accelerators
N.J.T.Smith STFC RAL 2010 July 2010
Facility developments
Several expansions of deep underground facilities completed, in construction or well progressed in planning
Site Size Status Available
Kamioka + 5.5x103m3 Complete 2008
SNOLAB 3x104m3 Complete 2009
LSC 8x103m3 In Construction 2010
SUSEL >3x104m3 In Construction 2010
CJPL 1.7x103m3 In Construction 2011
Yangyang 1.6x104m3 In Construction 2011+
LSM 4x104m3 Planned 2013
DUSEL >105m3 Planned 2015
N.J.T.Smith STFC RAL 2010 July 2010
SNOLAB Overall StatusSurface Facility
Operational from 2005.Provides offices, conference room, dry, warehousing, IT servers, clean-room labs, detector construction labs, chemical + assay lab
Underground Construction (Cube Hall, Cryopit, Ladder Labs, Lab Entrance)
Excavation complete and outfitting began June 2007. All main infrastructure (Chiller, MPC, HVAC, waste water plant) commissionedGeneral outfitting in Phase I areas almost complete + Cryopit 5T crane/access.Ladder Labs final cleaning complete, first experiment going inFirst experimental infrastructure installation in Cube Hall, fully clean
Experimental ProgrammeContinued operation of DEAP-1 and PICASSO. Current allocations to: PICASSO-III, DEAP-I, SNO+, DEAP-3600, MiniCLEAN, SuperCDMS TF, SuperCDMS, COUPP, HALO. Anticipated and under discussion: EXO-gas, DarkSide, low background counters to measure 39Ar, future Cobra upgrade…
N.J.T.Smith STFC RAL 2010 July 2010
Laboratory Space
All clean spaces will be operated as Class2000 clean rooms (or better).
ExcavationExcavation Clean RoomClean Room LaboratoryLaboratoryArea (m2) Volume (m3) Area (m2) Volume (m3) Area (m2) Volume (m3)
Original SNO Areas
Phase I
Phase II
1860 16500 1130 13300 750 11700
6070 38750 3900 29750 2430 23700
7220 46650 4940 37250 3060 29550
N.J.T.Smith STFC RAL 2010 July 2010
Chiller
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Chiller
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Lab Entry
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LabEntrance
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PersonnelFacility
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LabEntry
SNO Access Drift
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Galley/Refuge
Facilities 3 Feb 2009
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Galley/Refuge
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MeetingRoom
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CryopitAccess
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Cryopit
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Cryopit
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CubeHall
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CubeHall
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CubeHall
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CubeHall
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The Cube Hall Goes CleanCubeHall
N.J.T.Smith STFC RAL 2010 July 2010Unsealing door to Ladder Labs 5th Aug
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LadderLabs
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Personnel facilities
SNOCavern
Ladder Labs
Cube Hall
Cryopit
SouthDrift
HaloStub
UtilityDrift
DEAP-3600MiniCLEAN
HALO
Current PICASSO-II, DEAP-I (Dark Matter)
PUPS (Seismicity)
2009+
DEAP-3600, MiniCLEAN,
PICASSO-III (Dark Matter)
SNO+, HALO,
(Neutrino)
2010+SuperCDMS,
COUPP, DarkSide (Dark Matter)
Exo-Gas (Neutrino)
PICASSO-II
DEAP-I PUPS
SNO+
SuperCDMS
PICASSO-III
DarkSide
COUPP-60
COUPP-4
N.J.T.Smith STFC RAL 2010 July 2010
Dark Matter at SNOLABNoble Liquids: Deap-I, MiniCLEAN, & DEAP-3600, DarkSide
Single Phase Liquid Argon uses pulse shape discrimination. Two-phase (DarkSide)
Prototype DEAP-I operational in SNOLAB now. Successful demonstration of PSD and test bench for DEAP/CLEAN design/operations.
Construction for DEAP-3600 and MiniCLEAN underway. Full DEAP-3600 capital funding granted (with SNO+)
Will measure Spin Independent cross-section.
Superheated Liquid / Bubble chamber: PICASSO, COUPPSuperheated droplet detectors and bubble chambers. Insensitive to MIPS radioactive background at operating temperature, threshold devices
PICASSO currently operational in SNOLAB, demonstration of alpha rejection and test bench for scale-up of detector volumes.
COUPP on its way...
Will measure Spin Dependent cross-section primarily, COUPP has SI sensitivity
Solid State: SuperCDMSState of the art Ge crystals with ionisation and phonon readout.
Currently operational in Soudan. Next phase will benefit from SNOLAB depth to reach desired sensitivity. Test facility in Ladder Labs under development.
Mostly sensitive to Spin Independent cross-section.
N.J.T.Smith STFC RAL 2010 July 2010
SuperCDMS
Brink DM2010
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DEAP3600/miniCLEAN
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CubeHall - DEAP/
miniCLEAN
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DEAP-3600 DirectorMark Boulay
standing at the location of theDEAP-3600 Shield tank.
N.J.T.Smith STFC RAL 2010 July 2010
Nigel Smith with DEAP-3600 DirectorMark Boulay standing at the location
of the DEAP-3600 experiment.
N.J.T.Smith STFC RAL 2010 July 2010
Acceptance testing of theMiniCLEAN Vacuum Vessel.
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Aligning the anchors for the
MiniCLEAN detector stand.
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The PICASSO detector
N.J.T.Smith STFC RAL 2010 July 2010
PICASSO Stages
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COUPP
‘Rapid deployment’ of COUPP-4kg anticipated this summerShielding design underwayRegulatory checks in progressSpace allocated and service delivery in progressCOUPP-60kg to follow later this year/early next
N.J.T.Smith STFC RAL 2010 July 2010
Double beta decay2νββ expected in SM
half life > 1019 years 0νββ forbidden in SM (ΔL=2)
allowed in BSM models half life > 1025 years
requires ν massrequires Majorana nature
Inverted hierarchy: m3 << m1 ≈ m2
Normal hierarchy: m1 << m2 ≈ m3
Degenerate hierarchy: m1 ≈ m2 ≈ m3
KKDC range
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0νββ at SNOLABSNO+ : 150Nd → 150Sm + e- + e-
Uses existing SNO detector. Heavy water replaced by scintillator loaded with 150Nd. Modest resolution compensated by high statistical accuracy.
EXO-gas : 136Xe → 136Ba++ + e- + e-Developing technique to tag Ba daughter with electron tracking.
Chen/Nakamura
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Measuring the SNO+ Acrylic Vessel
flange in preparation
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Measuring the SNO+ Acrylic Vessel
flange in preparation
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Excavating a larger space in the
SNO+ Utility room to
N.J.T.Smith STFC RAL 2010 July 2010
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Other systems
SNO+ : Will also measure solar neutrino pep, geo-neutrinos, supernovae bursts and reactor neutrinos.
HALO: Dedicated Supernova watch experimentCharged/neutral current interactions in leadMaterials prepared for underground installation (Pb, NCD, DAQ)Infrastructure design completedInstallation in 2010.
PUPS: Seismicity Deep UndergroundCompleted operational cycle and now decommissioningSeismic wave propagation at various levels deep underground
N.J.T.Smith STFC RAL 2010 July 2010
Status of SNOLAB
SNOLAB Phase I infrastructureSurface facility, Cube Hall, Ladder LabsFinal outfitting and cleaning underway
Facility is now in transition to experimental programmeDeployment of support systems for first experiments underway (SNO+, DEAP-3600, MiniCLEAN, HALO)Smaller scale experiments continue operations (DEAP-I, PICASSO)Infrastructure requirements for additional systems being developed (COUPP, CDMS, DarkSide)
Additional space available now, Phase II (Cryopit)SNOLAB is looking forwards to contributing to the world programme of underground research facilities