Occupancy

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• The Gran Sasso underground laboratory
• Eugenio Coccia
• coccia_at_lngs.infn.it

Erice 31 august 2007
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Underground Laboratories
Very high energy phenomena, such as proton decay
and neutrinoless double beta decay, happen
spontaneously, but at extremely low rates. The
study of neutrino properties from natural and
artificial sources and the detection of dark
matter candidates requires capability of
detecting extremely weak effects.
Thanks to the rock coverage and the corresponding
reduction in the cosmic ray flux, underground
laboratories provide the necessary low background
environment to investigate these processes.
These laboratories appear complementary to those
with accelerators in the basic research of the
elementary constituents of matter, of their
interactions and symmetries.
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1400 m rock coveragecosmic µ reduction 106 (1
/m2 h)underground area 18 000 m2external
facilitieseasy access 756 scientists from 24
countriesPermanent staff 70 positions
LABORATORI NAZIONALI DEL GRAN SASSO -
INFN Largest underground laboratory for
astroparticle physics

• Research lines
• Neutrino physics
• (mass, oscillations, stellar physics)
• Dark matter
• Nuclear reactions of astrophysics interest
• Geophysics
• Biology

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LNGS most significant results with past
experiments
Evidence of neutrino oscillation GALLEX / GNO -
solar n MACRO - atmospheric n Uniqu
e cosmic ray studies EAS-TOP with LVD
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Underground Laboratories
Boulby UK
Modane France
Canfranc Spain
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??beam from CERN OPERA ICARUS

Fundamental physics VIP
PRESENT EXPERIMENTS
Dark Matter DAMA/LIBRA CRESST WARP Xenon test
bb decay and rare events Cuoricino CUORE GERDA
n from Supernovae LVD Borexino ICARUS
Solar ?n Luna Borexino
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Occupancy
HALL C
HALL B
LISA
MI RD
XENON
Borexino
ICARUS
HALL A
BAM - OPERA
OPERA
LVD
WARP
DAMA/LIBRA
GERDA
LUNA2
VIP
CRESST CUORE CUORICINO
LOW ACTIVITY LAB
GENIUS-TF
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LVD Large Volume Detector
Collab. Italy, Brazil, Russia, USA, Japan
Running since 1992
1000 billions ? in 20s from the SN
core Measurement of neutrinos spectra and time
evolution provides important information on ?
physics and on SN evolution. Neutrino signal
detectable from SN in our Galaxy or Magellanic
Clouds
2 - 5 SN/century expected in our Galaxy. Plan
for multidecennial observations 1000 tons liquid
scintillator layers of streamer tubes 300 ?
from a SN in the center of Galaxy (8.5 kpc)
SN1987A
Early warning of neutrino burst important for
astronomical observations with different
messengers (photons, gravitational waves) SNEWS
Supernova Early Warning System LVD, SNO, SuperK
in future Kamland, BOREXINO
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Large Volume Detector
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Super-Kamiokande (104) Kamland (330)
SNO (800) MiniBooNE (190)
Tra parentesi il numero di eventi da una SN
al centro della Galassia
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LVD data history

• ??? rate of Galactic Gravitational Stellar
  Collapses lt 0.18 event/year 90 c.l.

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The first CNGS event OnE
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During the CNGS run LVD has collected 582 CNGS
events (578 expected).
Agreement between the observed events and the
expected from the beam intensity!
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BOREXINO
300 tons liquid scintillator in a nylon bag 2200
photomultipliers 2500 tons ultrapure water Energy
threshold 0.25 MeV Real time neutrino (all
flavours) detector Measure mono-energetic (0.86
MeV) 7Be neutrino flux through the detection of
?-e. 40 ev/d if SSM
Sphere 13.7 m diam. supports the PMs optical
concentrators Space inside the sphere contains
purified PC Purified water outside the sphere
18 m diam., 16.9 m height
Collab. Italy, France, USA, Germany, Hungary,
Russia, Belgium Poland, Canada
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Borexino
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March 2, 2007 1012 inside of the SSS
PCPPO
PCDMP
water
Laura Perasso -Venezia,XII Neutrino Telescope,
March 6, 2007
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Solar, atmospheric, reactor neutrino experiments
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Emerging picture
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Purpose of CNGS tau appareance Nobody has
observed unambiguously the appearance of new
flavours You cant do it at the solar scale (E
too small to produce muons) At the atmospheric
scale oscillations are very likely P(nm ? nt) ?
cos4 ?13 sin2 2?23 sin2 1.27 Dm223
L(km)/E(GeV) Hence, you must be able to identify
unambiguously ? leptons The CNGS experiments
have been designed for it
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1979
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Cern Neutrinos to Gran Sasso (CNGS)
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The 2 ways of detecting t appearance _at_GRAN SASSO
m- nt nm BR 18 h- nt npo 50
e- nt ne 18 p p- p- nt npo
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nm .. nt ? t- X
oscillation CC

interaction
OPERA Observation of the decay topology of ?
in photographic emulsion ( mm
granularity) ICARUS detailed TPC image in
liquid argon and kinematic criteria ( mm
granularity)
Decay kink
n
t-
nt
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1st CNGS run august 06
1.7x1013 pot/extraction (70 nom.)
SPS cycle 16.8 sec
Total 7.6 E17 pot Ext1 3.81 E17 pot Ext2 3.79
E17 pot
Wed 30 Aug. 2006 0500
1st Extraction
MD Monday CNGS smoke detection system problem
Fri 18 Aug. 2006 1340
2 days MD problems on Friday 25
CNGS eff. 65
2nd Extraction
Unix time (ns)
Unix time (ns)
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OPERA (Oscillation Project with Emulsion-tRacking
Apparatus Conceptual design

• Target
• Lead/emulsions bricks alternated to
  scintillator strips
• emulsion tracking resolution ?xlt 1µm?????1mrad
• 206336 bricks 1.8 kton

• Muon Spectrometer
• Vertical drift tubes for ? p measurement from
  deflection through 24 magnetized iron slabs.
• Magnet instrumented with 22 RPC plane for
• ?p/p25 up to 50 GeV, charge miss-IDlt0.3

1 brick 56 layers of pb emulsion
Collab. Italy, France, Germany, Belgium,
Turkey, Switzerland, Russia, Japan, Israel,
Croatia
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Search for ????? oscillationexpected number of
events
full mixing, 5 years run _at_ 4.5x1019 pot / year
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OPERA sensitivity to ?13
Simultaneous fit of Ee, missing pT and Evis
distributions
10 syst. in ?e contamination
Limits at 90 CL for ?m2 2.5x10-3 eV2
full mixing
M.Komatsu, P.Migliozzi, F.Terranova J.Phys. G29
(2003) 443.
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NEUTRINO EVENTS IN OPERA
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Beam Direction
OPERA
Zenith angle of muon track
y
qy gt0
z
qy lt0
August Run result lt?gt3.40.3 (statistically
dominated))
MC simulation from MACRO parametrization,
ABSOLUTE normalization

• OPERA collect 319 beam events
• 3/4 external events (rock)
• 1/4 internal (CC NC)

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ICARUS T600 General layout
Dewar LN2 (30 m3)

Dewar LAr (30 m3)
T600
Passive heaters
Installation in progress in Gran Sasso Hall B,
commissioning after summer 2007
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ICARUS technique
Uniform Imaging in large volume liquid Argon

• Readout of the ionization electrons using wire
  planes with different orientation
• 3D reconstruction
• pixel 3 x 3 x 3 mm3
• High resolution calorimetry
• imaging ionization
• Readout of the Argon scintillation light
• Event start time
• Very high purity argon i (lt 0.1 ppb O2 equiv.)
• drift gt 5 m - Large dimension uniform detector

PMT
Electric Field
Ionizing Track
UV Light
Drifting
e-
in LAr
E1
wire pitch
Induction Plane I
Induction wire Signal Waveform
E2
d
Induction Plane II
Charge
Amplifier
E3
Tpeak
Tdrift
d
T0
Collection Plane
Light
time
PMT Signal
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Neutrinoless bb Decay
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Neutrino masses and 0n2b decayHeidelberg Moscow
experiment
Claimed evidence of 0nbb _at_ 4s T1/2 (0.3 - 2.0)
x 1025 y
0.1lt mn lt0.6 eV
HV Klapdor et al, NIMA Data Acquisition and
Analysis of the 76-Ge Double Beta experiment in
Gran Sasso 1990-2003
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Cuoricino (low temperature bolometer for double
beta experiment)

• Search for the 2bon in 130Te (Q2529 keV) and
  other rare events
• At Hall A in the Laboratori Nazionali del Gran
  Sasso (LNGS)
• 18 crystals 3x3x6 cm3 44 crystals 5x5x5 cm3
  40.7 kg of TeO2
• Operation started in the beginning of 2003

11 modules, 4 detector each, crystal dimension
5x5x5 cm3 crystal mass 790 g 4 x 11 x 0.79
34.76 kg of TeO2
2 modules, 9 detector each, crystal dimension
3x3x6 cm3 crystal mass 330 g 9 x 2 x 0.33 8.38
kg of TeO2
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Cuoricino (double beta experiment)

• Background .18.01 c /kev/ kg/ a
• T 1/2 0n (130Te) gt 2.4 x 1024 y ltmngt .2
  -1.
• Klapdor 0.1 0.9

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The CUORE project (Italy,USA, Spain)) approved
by the S.C. of Gran Sasso Laboratory and by INFN)
CUORE is an array of 988 bolometers grouped in
19 colums with 13 flours of 4 crystals
Crystals are separated by a few mm, only, with
little material among them
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CUORE expected sensitivity
In 5 years
Strumia A. and Vissani F. hep-ph/0503246
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IONIZATION
GERDA (Germany-Italy-Russia)

• goal analise HM evidence in a short timeusing
  existing 76Ge enriched detectors (HM, Igex)
• approach similar to GENIUS but less LN2
• naked Ge crystals in LN2 or LAr
• more compact than GENIUS
• 1.5 m LN2(LAr) 10 cm Pb 2 m water
• 2-3 orders of magnitude better bkg thanpresent
  Status-of-the-Art
• active shielding with LAr scintillation
• 3 phases experiment
• Phase I 2008
• radioactivity tests
• 20 kg 76Ge from HM and Igex
• expected bkg 0.01 c/keV/kg/y (intrinsic)
• check at 5s HM evidence
• 15 kgy 61 bb events on 0.5 bkg events
• Phase II
• add new enriched segmented detectors with
  special care for activation
• expected background 0.001 c/keV/kg/y
• 21026 y with 100 kgy
• ltmgt 0.09 0.29 eV

• Approved by LNGS S.C.
• site Hall A northern wing
• funded 40 kg enriched 76Ge for
• phase II
• aggressive time schedule

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GERDA _at_ LNGS
Screening ultra-pure liquids LAr Active H2O
Phase 1 Exposure 15 kg y b 102 yDRU
Sensitivity Mee 300-900 meV KK signal should
give 6.01.4 ev. on 0.5 bkg
Phase 2 Exposure 100 kg y b 103 yDRU
Minimise cosmogenic in Ge SegmentationPSA Sensit
ivity Meelt 90-290 meV lt170 meV ROD05 matr. el)
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Gran Sasso 2nd generation neutrino experiments

• Mass scale / Dirac or Majorana?
• (CUORE, GERDA)
• Oscillation parameters (neutrino tau appearence,
  unitarity of the mixing matrix , matter effect)
• (OPERA, ICARUS, Borexino)
• How small q13 ? gt Improve limits (only if q13
  ?0 and d ?0 CP leptonic violation possible)
• (OPERA)

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Dark matter particles

• How many different types?
• Dark matter particles have gravitational
  interaction
• Other unknown interactions?
• From cosmology should have Weak Interactions
  WIMPs (generically)
• SUSY extensions have a good candidate
  neutralino, stable if R is conserved
• Many other candidates from theorists( sneutrino,
  right neutrino, pseudo-Goldstone,.)
• Neutralino predictions of counting rates strongly
  model-dependent

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Dark matter search DAMA100 kg NaI(Tl) high
purity- ended 7/02
Annual modulationgt evidence for WIMPS Final
analysis total 107731 kg?d (Riv. N. Cim. 26 n.
1 (2003) 1-73)
fitted (all parameters free) A (0.0200 ?
0.0032) cpd/kg/keV t0 (140 ? 22) d
T (1.00 ? 0.01) y
6s
(P(A0) 7?10-4)
... ora DAMA/LIBRA
New apparatus - installed 2002 - 2003 250 kg
more radiopure NaI(Tl)
(Large sodium Iodide Bulk for RAre processes)
it will offer unique radiopurity, increased mass
and deep control of the running parameters
NEW RD for ultimate NaI(Tl) radiopurification
started towards a possible 1 ton set-up DAMA
proposed since 1996
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Noble Liquids

• Noble liquids, Xe, Ar, and Ne look very
  promising for the WIMP detection, because
• can be easily assembled in large masses
• self-shielding structures can be built, with the
  central part shielded by a large contiguous mass
  (in the same container) of the same liquid ? no
  free surface, no surface contamination
• Shield can be instrumented to act as a veto

• Two-phase (Liquid Gas)
• discrimination between nuclear and
  electromagnetic recoils by
• detection of primary scintillation light and
  ionisation via proportional scintillation
  (Benetti et al. in 1993)
• difference in the time dependence of luminescence
  for light (slow component from 3S states) and
  heavy recoils (fast component from 1S states) (A.
  Hitachi et al. in 1983)

Projects being developed CLEAN, LNe, Xe L-phase
XMASS (_at_KAMIOKA) L-Gas Xe XENON (_at_LNGS), ZEPLIN
(_at_Boulby) and XMASS-2P L-Gas Ar WARP (_at_LNGS),
DEAP (RD_at_Los Alamos)
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WARP 140-kg Detector

• The WARP 140-kg detector to be installed and
  commissioned at LNGS- 140 kg active target, will
  possibly allow to reach into 10-45 cm2
• covers most critical part of SUSY parameter space
• Complete neutron shield!
• 4p active neutron veto (9 tons Liquid Argon, 300
  PMTs)
• 3D Event localization and definition of fiducial
  volume for surface background rejection
• Detector designed for positive confirmation of a
  possible WIMP discoveryActive control on
  nuclide-recoil background, owing to unique
  feature (LAr active veto)
• Cryostat designed to allocate a possible 1400 kg
  detector

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XENON10 Underground at LNGS

• March 2006 XENON10 is shipped from Nevis Labs
  (Columbia University) to LNGS and commissioning
  starts underground. Presently running inside the
  shield since August 2006.

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A new large European infrastructure for a
detector 105-106 ton scale ? Improved studies
on proton decay, on low-energy neutrinos from
astrophysical origin and possible detection of
future accelerator neutrino beams Three
detection techniques being studied
water-Cherenkov, liquid scintillator and liquid
argon Worldwide efforts
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LNGS
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Liquid Argon and CNGS2 off axis
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Liquid Argon and CNGS2 off axis
Cave for one 5 kton unit 11x20x60m
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Liquid Argon and CNGS2 off axis
20kTon liq Argon Dedicated beam
Ultimate limitation target/horn (for all
beams) CNGS now 4.5x 1019
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Gerda
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.. not only Science

• Safety
• Training
• Outreach

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2004 - 2005 - 2006 Important safety and
infrastructures upgrade of the Laboratory

• Floor waterproofing
• Realization of containment basins
• Safety measure for the drinkable water

• Upgrade of the ventilation system
• Upgrade of the cooling capability
• Upgrade of the electrical power

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Gran Sasso - Princeton Summer School
20 selected Abruzzo students 4 weeks stage in
the Princeton University Campus
1 week Review of classical physics 2 week
Introduction to special relativity 3 week
Introduction to quantum mechanics 4 week
Introduction to particle physics

• Sponsors
• INFN
• Abruzzo Region
• Micron
• NJ Italian-american associations

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Gran Sasso - Princeton Summer School
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Training
Outreach
17000 visitors/year
17000 visitors/year
Alta Formazione
2007 1.3 M Euro from Abruzzo region
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• The Gran Sasso Lab is ready to face the second
  phase of his scientific life with top class
  experiments in neutrino physics and dark matter
  direct searches.

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