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Laboratorio Subterráneo de Canfranc

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Presentation on theme: "Laboratorio Subterráneo de Canfranc"— Presentation transcript:

1 Laboratorio Subterráneo de Canfranc
IN2P3 - MICINN meeting Madrid, 12 January 2009

2 Map of LSC

3 Experimental halls A, B and C
600 m2 (40x15x12) Hall A 150 m2 (15x10x7) Hall B Depth: m Muons: 0.47 m x 10-2 m m-2 s-1 Hall C Ventilation: m3/h

4 Status of the reparation works
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

5 Objectives 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) 23/03/2017 A. Bettini. LSC 5

6 External building Headquarters & Administration
Safety and Quality Assurance 16 offices for scientific users 7 offices for LSC personnel 4 specialised laboratories Mechanical workshop & storage room Meeting room Library Conference room Exhibitions room 2 apartments Surface: m2 (2.115 m2 built) Project completed: December 2008 Building completed: Autumn 2010 Cost of the building: ,27 €

7 Structures Managed by 14 staff

8 Scientific Programme Physics
- Approved experiments on proposal of the International Scientific Committee. 3 years running. Milestones defined. Two referees appointed to each exp EXP (ANAIS) Dark Matter (NaI, Annual modulation) Direct check of DAMA/LIBRA result EXP (ROSEBUD) Dark Matter (Scintillating bolometers) Integrated in the European EURECA project EXP (BiPo) 0 decay (extra-low surface background meas.) Ancillary to Super-NEMO EXP (ULTIMA) Super-fluid 3He physics To be screened by muon background EXP (NEXT) 0 decay (Enriched 136Xe TPC) Majorana vs Dirac neutrinos CUP Consolider approved EoI (ArDM) EoI on Dark Matter (Liquid Argon TPC) In risk analysis phase

9 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 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

10 EXP-01-2008 ANAIS Search for the annual modulation
Confirm/refute DAMA evidence 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 1410.7 kg NaI crystals stored underground since 1988 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

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

12 EoI-02-2005 ArDM Ar two-phase TPC
Tests on 1 t prototype going on at CERN Preliminary LSC risk analysis stage

13 Neutrino-less Double beta decay
Unlike 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 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) 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

14 EXP-03-2008 BiPo 232Th 238U EFWHM/E @ 1MeV NEMO3 =14-17%
Best prototype so far = 8% Design figure = MeV a (300 ns) 232Th 212Bi (60.5 mn) 208Tl (3.1 mn) 212Po 208Pb (stable) 36% 64% Contamination of the (large) source foil BiPo detectors for requested sensitivity 208Tl < 20 µBq/kg  <2 µBq/kg 214Bi < 300 µBq/kg  <10 µBq/kg a (164 ms) 238U 214Bi (19.9 mn) 210Tl (1.3 mn) 214Po 210Pb 22.3 y 0.021%

15 The ultimate background: 2bn
Case of 136Xe assuming T1/2()1021 (measured lower limit) Expos.=0.5 t y Mee=60 meV FWHM= 3.5% FWHM= 1% Expos.=5 t y Mee=20 meV High pressure TPC Strong R&D effort needed EXO achieved

16 EXP 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

17 EXP-04-2008 ULTIMA 100 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

18 Possible location of the experiments
Laboratory space is almost full

19 Strategic Plan 2010-2013 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 To be presented tomorrow

20 Scientific Programme Geodynamics, Environment
- 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 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

21 The astrophysical S-factor
? S(E) = E·(E)·exp(2) (E) = S(E)·exp(-2)/E 2 = Z1 Z2 (/E)0.5 Extrapolations by orders of magnitude not always safe (resonances)

22 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

23 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

24 GIGS. Fast and slow quakes
Local normal quakes 1.5 µm Michelson interferometer with asymmetric arms. Longer one is 90 m Quake at Giava superposed to a slow local quake Slow (aseismic) quake 0.5 µm

25 Dark Life No proposal yet 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? No proposal yet

26 Thank you

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