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INDIA-BASED NEUTRINO OBSERVATORY

INDIA-BASED NEUTRINO OBSERVATORY. I N O. Naba K Mondal TIFR. 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. KGF Continued.

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INDIA-BASED NEUTRINO OBSERVATORY

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  1. INDIA-BASED NEUTRINO OBSERVATORY I N O Naba K Mondal TIFR

  2. 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

  3. KGF Continued KGF Proton Decay Experiment KGF collaboration contributed immensely to the cosmic ray and particle physics. The KGF mine was closed in early 90’s

  4. 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

  5. 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

  6. Physics with Neutrino beam from NUFACT – Phase II • Determination of q13 • Sign of d32 • Probing CP violation in leptonic sector • Matter effect in nm ntoscillation

  7. 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 ( <= 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

  8. INO Detector Concept

  9. The Magnet

  10. 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

  11. ICAL Detector Specifications

  12. RPC R & D • Built RPCs of different sizes • 30 cm X 30 cm : 25 • 120 cm X 90 cm : 2

  13. RPC Test facilities Cosmic Muon test setup at TIFR Gas mixing unit developed at SINP

  14. RPC Efficiencies and Timing RPC working in Streamer mode

  15. 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

  16. Performance in Avalanche mode Efficiency plots of RPCs in Avalanche mode Noise Rates of RPCs operating in Avalanche mode

  17. Magnet R & D • Two independent Studies: • Using Poisson Code at VECC • with solenoidal coil • Using MagNet 6.0 at BARC/TIFR • with Helmholtz coil

  18. Magnet Simulation

  19. Magnet Prototype

  20. Electronics for ICAL

  21. 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.

  22. Results using NUANCE n m

  23. Matter effects: Sign of D32 Preliminary With 500 kton yr exposure

  24. 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.

  25. Possible tunnel alignments at PUSHEP 4 possible alignments of INO tunnel at PUSHEP

  26. Underground Cavern Experimental Hall Layout of the Underground Cavern Size of the experimental hall 150 m X 22 m X 30 m Parking & Storage Access tunnel Experimental Hall Electronics

  27. 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

  28. Cost breakup

  29. 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

  30. 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

  31. Documentation produced so far

  32. 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.

  33. 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.

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