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