Diapositiva 1

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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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Experimental halls A, B and C
600 m2 (40x15x12)
Hall A
150 m2 (15x10x7)
Hall B
Depth 800 m
Muons 0.47 m x 10-2 m m-2 s-1
Hall C
Ventilation 11.000 m3/h
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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

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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)
21/11/2009
A. Bettini. LSC
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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 1.821 m2 (2.115 m2 built) Project
completed December 2008 Building completed
Autumn 2010 Cost of the building
2.830.403,27
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Structures
Managed by 14 staff
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Scientific ProgrammePhysics

• - 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 physics
• To be screened by muon background
• EXP-05-2008 (NEXT) 0??? decay (Enriched 136Xe
  TPC)
• Majorana vs Dirac neutrinos
• CUP Consolider approved
• EoI-02-2005 (ArDM) EoI on Dark Matter (Liquid
  Argon TPC)
• In risk analysis phase

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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 bO(103 kg1keV1 d1)
• To explore theoretical range need MO(1t) and bO
  (105 kg1keV1 d1)
• 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
Search for the annual modulation Confirm/refute
DAMA evidence
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
• UTh lt 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

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EXP-02-2008 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)
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EoI-02-2005 ArDM
Ar two-phase TPC Tests on 1 t prototype going on
at CERN Preliminary LSC risk analysis stage
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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
  experiments _at_ LNGS)
• Exposure O (100 kg yr)
• Background bO(102 kg1keV1 y1)
• 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 _at_ 100 kg does not fit in LSC
• Extrapolates NEMO3 technology. However, much RD
  needed
• First steps BiPo and its prototypes
• Liquid Xe TPC. EXO 200 kg in the US
• Gas TPC with novel RD techniques
• Much RD needed. NEXT

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EXP-03-2008 BiPo
?EFWHM/E _at_ 1MeV NEMO3 14-17 Best prototype so
far 8 Design figure 4 _at_3 MeV
Contamination of the (large) source foil BiPo
detectors for requested sensitivity 208Tl lt 20
µBq/kg ? lt2 µBq/kg 214Bi lt 300 µBq/kg ? lt10
µBq/kg
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The ultimate background 2b?n
Case of 136Xe assuming T1/2(????)?1021 (measured
lower limit)
High pressure TPC Strong RD effort needed
EXO achieved
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EXP-05-2008 NEXT

• High pressure gas TPC with enriched 136Xe
  Complementary to EXO
• Status. Initial RD 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
  gt 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
Laboratory space is almost full
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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 2006-2008
• To be presented tomorrow

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Scientific ProgrammeGeodynamics, 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 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

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The astrophysical S-factor
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 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
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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?

No proposal yet
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Thank you