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Atmospheric Neutrinos

Atmospheric Neutrinos. Atmospheric neutrino detector at Kolar Gold Field –1965. More on KGF. KGF Proton Decay Experiment. INO Collaboration.

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Atmospheric Neutrinos

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  1. Atmospheric Neutrinos Atmospheric neutrino detector at Kolar Gold Field –1965

  2. More on KGF KGF Proton Decay Experiment

  3. INO Collaboration B.S.Acharya, Sudeshna Banerjee, P.N.Bhat, S.R.Dugad, P.Ghosh, K.S.Gothe, S.K.Gupta, S.D.Kalmani, N. Krishnan, N. K Mondal, B.K.Nagesh , P.Nagaraj, Biswajit Paul, A.K.Ray, Probir Roy, B.Satyanarayana, S.Upadhaya, P.Verma Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai V.M.Datar, M.S.Bhatia, S.K.Kataria Bhabha Atomic Research Centre, Mumbai P. Bhattacharya, S.Bhattacharya, S. Chattopadhyay, A.Ghoshal, A.Goswami K. Kar, D.Majumdar, P.B.Pal, S. Saha, M. Sharan, S.Sarkar, S.Sen Saha Institute of Nuclear Physics, Kolkata S. Chattopadhyay, M.R.Datta Mazumdar, P.Ghosh, G.S.N.Murthy, T.Nayak, Y.P.Viyogi Variable Energy Cyclotron Centre, Kolkata  Amitava Raychaudhuri Calcutta University, Kolkata M.V.N.Murthy, D.Indumathi Institute of Mathematical Sciences, Chennai A. Datta, R.Gandhi, S.Goswami, S. Rakshit, P.Mehta Harish Chandra Research Institute, Allahabad S.C.Phatak, D.P.Mahapatra IOP, Bhubaneswar Amit Roy Nuclear Science Centre, New Delhi J.B.Singh, M.M.Gupta, V.Bhatnagar Panjab University, Chandigarh   S.D.Sharma Himachal Pradesh University, Simla A.Joshipura, S.Rindani P.R.L., Ahmedabad A.Bhadra,B.Ghosh,A.Mukherjee,S.K.Sarkar North Bengal University S.Umasankar IIT, Mumbai S.K.Singh AMU Scientific Advisors: G.Rajasekaran, Bikash Sinha, Ramnath Cowsik,V.S.Narasimham, H.S.Mani, Amit Roy 41 Experimentalists + Engineers 22 Theorists

  4. Current Initiative • Two phase approach: • Phase I ~ 2 Yrs. • Detector R & D • Site survey • Human resource development through training and workshops • Phase II • Construction of the detector • Detector Possibilities: • Magnetised iron with RPCs or glass spark chambers. • Alternate detector design. • Should be an international facility

  5. Neutrino Oscillations For neutrinos, weak eigenstates may be different from mass eigenstates. In a weak decay one produces a definite weak eigenstate Then at a later time t

  6. 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 • Use magnetised iron as target mass and RPC as active detector medium

  7. N up(L/E) N down(L’/E) = P(nm nm; L/E) Disappearance of Vs. L/E The disappearance probability can be measured with a single detector and two equal sources: L’ q L = 1 - sin2 (2Q) sin2 (1.27 Dm2L/E) q

  8. Current Activities • Detector Development. • Detector Simulation. • Physics Studies. • Data Acquisition System. • Site Survey. • International Collaboration.

  9. INO Detector Concept INO IRON CALORIMETER RPC Trays

  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 Complete RPC

  11. RPC Principles of Operation Signal pickup(x) Graphite Glass Plates Spacers 8 KV Signal pickup (y) Graphite A passing charged particle induces an avalanche, which develops into a spark. The discharge is quenched when all of the locally ( ) available charge is consumed. Before After ++++++ ++++++ ++++++++++++++++++++ ---------- ------- ------------------------- The discharged area recharges slowly through the high-resistivity glass plates.

  12. Principles of Operation: Rate Capability After the passage of a charge particle a part of the detector around the track will be dead. The recovery time is approximately +++++++ +++++++ ------------ -------- If we assume the area of dead space to be , then rates of upto can be handled with 1% deadtime or less. This is well below what is expected in our application.

  13. Pulse Height from RPC In streamer mode of operation, pulses are large (~100 mV into 50 ohms) and fast (FWHM ~ 15ns)

  14. Test of RPC

  15. Glass Spark Chamber R & D Schematic of the RPC test setup at TIFR P3 Glass RPC under test P1 P2 P6 P4 P5 Muon Trigger =

  16. Gas Mixing Unit

  17. Bubble Counter as flow rate monitor

  18. RPC Efficiency and Time resolution Freon 134a : 62% Argon : 30% Isobutane : 8% Fermi Lab measurement

  19. RPC Efficiency Studies

  20. RPC Timing Studies

  21. RPC Charge distribution

  22. RPC Mean Charge Vs. Voltage

  23. RPC Noise Pulse rate

  24. RPC Cross talk

  25. Magnet Model at VECC • A model of the INO magnet has been fabricated at VECC to understand – If the measured field agrees with calculation. Whether 2D calculation is OK To understand magnet energizing time Expected field inside iron 14 KG

  26. Detector and Physics Simulation • NUANCE Event Generator: • Generate atmospheric neutrino events inside INO detector • GEANT Monte Carlo Package: • Simulate the detector response for the neutrino event • Event Reconstruction: • Fits the raw data to extract neutrino energy and direction • Physics Performance of the baseline INO detector. • Analysis of reconstructed events to extract physics. These studies are going on at all the collaborating institutes

  27. Physics Performance

  28. Other Physics potential • Cosmic ray studies using multiple muon + air shower on surface • Search for magnetic monopoles • Search for WIMPs • Additional studies on Kolar Events, Double core events, anomalous cascades • Neutrinos from factories

  29. Possible INO sites • PUSHEP (Pykara Ultimate Stage Hydro Electric Project) in South India or • RAMMAM Hydro Electric Project Site

  30. Possible tunnel alignments at PUSHEP 4 possible allignments of INO tunnel at PUSHEP

  31. PUSHEP • Action Items: • Stress measurement at depths of 1000m • Permissions to conduct tests and approval • for locating INO at PUSHEP • Possibility of building exploratory tunnel

  32. Location of Rammam

  33. Possible tunnel alignment at Rammam

  34. International Collaboration • Such a facility has to be an international effort. • A small beginning in detector collaboration with Gran Sasso Laboratory and Fermilab. • Discussing with JHF proponents on a possible very long base line beam towards INO. Ultimate Long base line neutrino experiment should have a beam from USA to India. • US has long term commitment towards neutrino physics. India has started R & D effort in this direction. There are lot of scope for collaboration. • There are lot more to achieve • Detector R & D • Associated Electronics • Simulation software and event reconstruction

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