INDIABASED NEUTRINO OBSERVATORY

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INDIA-BASED NEUTRINO OBSERVATORY
I N O
Naba K Mondal TIFR
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Neutrino Physics in India
Physics Letters 18, (1965) 196, dated 15th Aug
1965
Atmospheric neutrino detector at Kolar Gold
Field 1965
PRL 15, (1965), 429, dated 30th Aug. 1965
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KGF Continued
KGF Proton Decay Experiment
KGF collaboration contributed immensely to the
cosmic ray and particle physics. The KGF mine
was closed in early 90s
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INO initiative

• Multi Institutional Collaborative approach from
  beginning
• MOU Signed by Directors of 7 institutes under DAE
  in a meeting attended by Chairman, AEC on August
  30th 2002
• Two phase approach

R D and Construction Phase I Detector R
D, Physics studies, Site survey, Human resource
development Phase II Construction of the
detector
Operation of the Detector Phase I Physics with
Atmospheric Neutrinos Phase II Physics with
Neutrino beam from a factory
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Physics using atmospheric neutrinos during Phase I

• Reconfirm atmospheric neutrino oscillation
• Improved measurement of oscillation parameters
• Octant degeneracy for q23
• Search for potential matter effect in neutrino
  oscillation
• Determining the sign of Dm23 using matter effect
• Discrimination between nm ? nt and nm ? ns
  oscillation
• Probing CP and CPT violations
• Constraining long range leptonic forces
• Ultra high energy neutrinos and muons
• Kolar events

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Physics with Neutrino beam from NUFACT Phase II

• Determination of q13
• Sign of d32
• Probing CP violation in leptonic sector
• Matter effect in nm ? nt oscillation

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Choice of Neutrino Source and Detector

• Neutrino Source
• Need to cover a large L/E range
• Large L range
• Large En range
• Use Atmospheric neutrinos as source
• Detector Choice
• Should have large target mass ( 50-100 KT)
• Good tracking and Energy resolution ( tracking
  calorimeter)
• Good directionality ( lt 1 nsec time resolution
  )
• Ease of construction
• Modularity
• Complimentarity with other existing and proposed
  detectors
• Use magnetised iron as target mass and RPC as
  active detector medium

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INO Detector Concept
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The Magnet
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Construction of RPC
Two 2 mm thick float Glass Separated by 2 mm
spacer
2 mm thick spacer
Pickup strips
Glass plates
Graphite coating on the outer surfaces of glass
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ICAL Detector Specifications
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RPC R D

• Built RPCs of different sizes
• 30 cm X 30 cm 25
• 120 cm X 90 cm 2

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RPC Test facilities
Cosmic Muon test setup at TIFR
Gas mixing unit developed at SINP
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RPC Efficiencies and Timing
RPC working in Streamer mode
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RPC in Avalanche mode
CMS bakelite RPC 73 cm X 42.5 cm
120 cm X 90 cm Glass RPC Built at TIFR
CMS RPC on test stand
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Performance in Avalanche mode
Efficiency plots of RPCs in Avalanche mode
Noise Rates of RPCs operating in Avalanche mode
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Magnet R D

• Two independent Studies
• Using Poisson Code at VECC
• with solenoidal coil
• Using MagNet 6.0 at BARC/TIFR
• with Helmholtz coil

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Magnet Simulation
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Magnet Prototype
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Electronics for ICAL
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Detector Simulation

• Used NUANCE Neutrino Event Generator
• Generate atmospheric neutrino events inside INO
  detector
• Used Atmospheric Neutrino Flux of Honda et. al.
• GEANT3 detector simulation package
• Simulate the detector response for the neutrino
  event
• Generated 5 years of simulated data equivalent to
  5 years of running the experiment.
• Analysed oscillation data at two levels
• Using NUANCE output and kinematic resolution
  function
• Using full detector simulation
• Obtained preliminary results so far. Detailed
  simulation is underway.

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Results using NUANCE
n
m
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Matter effects Sign of D32
Preliminary With 500 kton yr exposure
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Location of the Underground Laboratory

• Studies were performed on two potential sites.
• Pykara Ultimate Stage Hydro Electric Project
  (PUSHEP) at Masinagudi, Tamilnadu
• Rammam Hydro Electric Project Site at Darjeeling
  District in West Bengal
• INO Site Selection Committee after thorough
  evaluation have now recommended PUSHEP at
  Tamilnadu as the preferred site for the
  underground lab.

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Possible tunnel alignments at PUSHEP
4 possible alignments of INO tunnel at PUSHEP
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Underground Cavern
Layout of the Underground Cavern
Experimental Hall
Size of the experimental hall 150 m X 22 m X 30 m
Parking Storage
Access tunnel
Experimental Hall
Electronics
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Preliminary Cost Estimate

• Three components
• Cost of building the facility
• Underground Tunnel
• Cavern
• Surface laboratory and INO Center
• Cost of Iron
• Cost of the Active Detector Modules
• RPCs
• Gas System
• Electronics
• Magnetisation

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Cost breakup
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Time Scale

• Phase 1 12-18 months
• Draw up detailed design report for tunnel and
  cavern
• Detailed design report on detector structure,
  RPCs, pickup electrodes, electronics power
  supply system
• Phase II 22-40 months
• Tunnel cavern construction
• RPC construction
• Tendering and procurement of iron, magnet coil
• Electronics and gas mixing unit procurement and
  fabrication
• Phase III 12-18 months
• Laboratory outfitting
• Transporting of materials
• Assembly
• Data taking of first module start early while
  assembly of other modules continue

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INO as a Facility for the Future

• Low Energy neutrinos
• Reactor neutrinos
• Supernova neutrinos
• Global radioactivity in the earth
• Double beta decay
• Nucleon decay
• Neutrino astronomy
• Low energy accelerator for nuclear astrophysics

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Documentation produced so far
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Status of the project

• Recent Important Steps
• Presentation to Funding agencies in May, 2005
• Presentation to SAC, PM in October, 2005
• Site Selection complete
• Task force for DPR report on site is being
  constituted now
• A committee setup jointly by DAE DST to discuss
  the future projects on HEP in india to meet soon.

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Summary

• Neutrino physics is key to our understanding of
  physics beyond standard model.
• A large magnetised detector of 50-100 Kton is
  needed to achieve some of the very exciting
  physics goals using atmospheric neutrinos.
• Physics case for such a detector is strong as
  evident from recent publications.
• It will complement the existing and planned
  water cherenkov detectors.
• Can be used as a far detector during neutrino
  factory era.
• We have started a very active R D work towards
  building such a detector.
• Looking for participation from international
  neutrino community.