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Laboratorio Subterráneo de Canfranc

IN2P3 - MICINN meeting

Madrid, 12 January 2009

http://www.lsc-canfranc.es/

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Map of LSC

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600 m2 (40x15x12)

Depth: 800 m

Muons: 0.47x 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

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• January 2007: Signs of rocks instability

• March 2007: Rock fall in hall A

• August 2007: End of short range consolidation works (UZ)

• January 2008: Agreement on the project for safety improvement works

• February 2008: UZ sends project to GA for supervision

• July 2008: LSC Director requests to UZ, including

•Report on the status of the reparation works “as done”, and convergence measurements

•Programme of the future works including organisation, milestones and times

• December 2008: GA sends final supervision to UZ

Status of the reparation works

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Create a world-class underground multi-disciplinary laboratory with experiments and observatories leading in:

•Dark matter searches

•Neutrino nature (Majorana vs. Dirac) and mass

•Nuclear astrophysics

•Physics of system near absolute zero

•Extreme low background techniques

•Sub-surface geo-dynamics

•Environmental ultra-low background studies

•Life under extreme conditions

Consider options for long range development (LAGUNA)

Objectives

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Headquarters & AdministrationSafety and Quality Assurance16 offices for scientific users7 offices for LSC personnel4 specialised laboratoriesMechanical workshop & storage roomMeeting roomLibraryConference roomExhibitions room 2 apartments

Surface: 1.821 m2 (2.115 m2 built)Project completed: December 2008Building completed: Autumn 2010Cost of the building: 2.830.403,27 €

External building

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Managed by 14 staff

Structures

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- Approved experiments on proposal of the International Scientific Committee.

3 years running. Milestones defined. Two referees appointed to each exp

EXP-01-2008 (ANAIS) Dark Matter (NaI, Annual modulation) Direct check of DAMA/LIBRA result

EXP-02-2008 (ROSEBUD) Dark Matter (Scintillating bolometers)Integrated in the European EURECA project

EXP-03-2008 (BiPo) 0 decay (extra-low surface background meas.)

Ancillary to Super-NEMO

EXP-04-2008 (ULTIMA) Super-fluid 3He physicsTo be screened by muon background

EXP-05-2008 (NEXT) 0 decay (Enriched 136Xe TPC)Majorana vs Dirac neutrinosCUP Consolider approved

EoI-02-2005 (ArDM) EoI on Dark Matter (Liquid Argon TPC) In risk analysis phase

Scientific ProgrammePhysics

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Dark Matter

95% of the Universe mass-energy is “dark” •Status of the art. Calorimetric approach: target of dark particles = detector

• sensitive detector mass M= several kg

• best background b=O(10–3 kg–1keV–1 d–1)

•To explore theoretical range need M=O(1t) and b=O (10–5 kg–1keV–1 d–1)

•This levels may be reached in the next few years by noble liquids

•10-100 kg Xe and Ar modules operational / under construction at LNGS

•Xe and Ar complementary, both in physics and technique. Both should be done

•Do not forget other techniques. Hunting for dark matter is extremely difficult

•Strong competition world wide

•DAMA positive evidence can be confirmed/rejected only by an annual modulation sensitive experiment with Iodine nuclei

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EXP-01-2008 ANAIS

•Contribution to background of internal contamination at 2-6 keV

•U&Th < 1/ (keV kg d) OK•40K several/(keV kg d) too large

•New crystals required•Funded about 100 kg by MCINN Program•Additional NaI procurementwith LSC funding under examination

Active vetos

PVC box

40 cm neutron shielding

2 mm Cd

10 cm Roman lead 20 cm lead

Work on a series of prototype performed in the old LSC using 1410.7 kg NaI crystals stored underground since 1988

Search for the annual modulationConfirm/refute DAMA evidence

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EXP-02-2008 ROSEBUDDevelop cryogenic temperatures bolometers with heat and scintillation light readout, focussing on prototypes for EURECA (next-generation European project for DM search with bolometers)

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EoI-02-2005 ArDMAr two-phase TPCTests on 1 t prototype going on at CERNPreliminary LSC risk analysis stage

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Neutrino-less Double beta decayUnlike the other particles neutrinos may be matter and antimatter at the same time•Two approaches: calorimetric and tracking

•Status of the art of calorimetric approach (two experiments @ LNGS)

•Exposure: O (100 kg yr)

•Background: b=O(10–2 kg–1keV–1 y–1)

•Complementary tracking approach necessary, on different isotopes, with similar sensitive masses

•Due to limited overburden of LSC tracking approach (calorimetry already covered by CUORE and GERDA)

•SuperNEMO @ 100 kg does not fit in LSC

•Extrapolates NEMO3 technology. However, much R&D needed

•First steps: BiPo and its prototypes

•Liquid Xe TPC. EXO 200 kg in the US

•Gas TPC with novel R&D techniques

• Much R&D needed. NEXT

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EXP-03-2008 BiPo

(300 ns)

232Th

212Bi(60.5 mn)

208Tl(3.1 mn)

212Po

208Pb(stable)36

%

64%

(164 s)

238U

214Bi(19.9 mn)

210Tl(1.3 mn)

214Po

210Pb22.3 y

0.02

1%

Contamination of the (large) source foil BiPo detectors for requested sensitivity208Tl < 20 µBq/kg <2 µBq/kg214Bi < 300 µBq/kg <10 µBq/kg

EFWHM/E @ 1MeV

NEMO3 =14-17%Best prototype so far = 8%Design figure = 4% @3 MeV

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The ultimate background: 2

Expos.=0.5 t yMee=60 meVFWHM= 3.5%

Expos.=0.5 t yMee=60 meVFWHM= 1%

Expos.=5 t yMee=20 meVFWHM= 1%

Expos.=5 t yMee=20 meVFWHM= 3.5%

Case of 136Xe assuming T1/21021 (measured lower limit)

EXO achieved

High pressure TPC Strong R&D effort needed

S

B;meQ

5

7 E( )6T1/

T1/0

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EXP-05-2008 NEXT

High pressure gas TPC with enriched 136Xe Complementary to EXO

Status. Initial R&D phases. CUP Consolider (mainly NEXT) approved (5 M€)

•Avoid charged background from surfaces by eliminating surfaces, based on 100% active, completely closed virtual fiducial surface

• Obtain fine topological information (unlike EXO)

• Tag signal by topology: 2 balls at the end of the spaghetti

• Expected reduction of (dominant) gamma background > 100

•FWHM resolution O(1%) appears feasible with latest TPC R/O techniques

•Montecarlo evaluation of the tolerable radioactive contaminants in materials & screening starting now

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EXP-04-2008 ULTIMA100 µK superfluid 3He detector

Density of quasi-particles determined directly by measuring the damping of micro vibrating wire

Originally proposed for dark matter direct search via spin-dependent coupling

Detector sensitive mass very small (grams)

The super-fluid phase of the 3He-4He mixture might be observable at these temperatures

Signal is confused by cosmic muons interference on the surface

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Possible location of the experiments

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•Due by all the Spanish ICCs by 31/12/2008

•Built on the basis of the approved multi-annual LSC funding

•Invest in infrastructures residuals 2006-2008

•To be presented tomorrow

Strategic Plan 2010-2013

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- Presented at the Scientific Committee, preliminary stage of discussion

Canfranc Nuclear Astrophysics facility (CUNA) New dedicated hall & Accelerator (5 MeV, to be funded separately)

Develop synergic program with INFN LNGS

Dedicated scientific Workshop in Barcelona 19-20 Feb 2009

Geodynamic facility (GEODYN)

Integrate in the TOPO-IBERIA Consolider

Integrate with LSC rock stability monitors

Ultra-Low Level Lab for Environmental Radioactivity Monitoring (ULLERM)

Groundwater, rainwater, air (inside & outside) and soil characterisation

Integrate in the general purpose ultra-low-background service

Scientific ProgrammeGeodynamics, Environment

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The astrophysical S-factor

S(E) = E·(E)·exp(2)

(E) = S(E)·exp(-2)/E

2 = 31.29 Z1 Z2 (/E)0.5?Extrapolations by orders of magnitude not always safe (resonances)

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CUNA•First Laboratory for Nuclear Underground Astrophysics (LUNA) at INFN LNGS. 1995…..

•LUNA1: 50 kV + LUNA2: 400 kV

•Beautiful measurements of the cross sections of nuclear reactions relevant for the Sun and stars: d(p,)3He, 3He()7Be, 14N(p,)15O, 25Mg(p,)26Al

•Many other cross sections await for measurement:

• 12C()16O, 13C(n)16O, 22Ne(n)25Mg

• (n) on 15N, 14N, 18O…

•Next phase requires higher energy (3-5 MeV) accelerator

•Needs separate hall due to neutron production

•LUNA3 proposal at LNGS 3-4 MeV

•Develop European program with two complementary sources

•Build a dedicated hall and associated facilities at LSC

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GEODYN•LSC is located underground in one of the most seismically active areas in Europe

•Ideal position for an advanced geodynamic observatory with

•two perpendicular LASER strainmeters

•borad-band and strong motion seismometers

•CGPS stations on the surface

•Integrate in the TOPO-IBERIA Consolider project

•Local phenomena

•measure seismic phase velocity

•Slow earthquakes

•Strain seasonal changes (charging and discharging of the aquifer,..)

•Tectonic deformation

•Global phenomena

•Siesmic core modes

•Free oscillations of the Earth

•Free core nutation

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GIGS. Fast and slow quakes

Local normal quakes1.5 µm

0.5 µmSlow (aseismic) quake

Quake at Giava superposed to a slow local quake

Michelson interferometer with asymmetric arms. Longer one is 90 m

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Dark Life

•Microbiology•How deeply in the earth does life extend?•What makes life successful deep under the surface?•What can life underground teach us about how life evolved?

•Status of art. Studies made by Henderson DUSEL project in US•2 new Phyla discovered at Henderson

•Cross-disciplinary work between biologists and geologists•Do bacteria enter into the genesis of minerals and rocks?

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Thank you