STATUS OF INDIA-BASED NEUTRINO OBSERVATORY (INO)

1. STATUS OF INDIA-BASED NEUTRINO OBSERVATORY (INO) Naba K Mondal Tata Institute of Fundamental Research Mumbai, India NuHorizons-09

2. Atmospheric neutrino detection in 1965 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 NuHorizons-09

3. KGF NuHorizons-09

4. India-based Neutrino Observatory Project • India-based Neutrino observatory is a Mega Science Project funded by Dept. of Science & Technology and Dept. of Atomic Energy, Govt. of India . The project will lead to: • Creation of a world class underground laboratory in the country for carrying out research in the emerging field of neutrino physics. Will develop into a full fledged underground laboratory over the years for other studies in physics, biology & geology. • Involvement of Universities in a big way for carrying out large basic science projects- healthy development of University-Research lab partnership. • A Centre for particle physics and detector technology and its varied applications in areas like medical imaging. • INO graduate training program will lead to Ph.D. in particle physics and more importantly creating highly skilled scientific manpower for experimental high energy and nuclear physics. Hands on training on all aspect of experiments with strong emphasis on detector development. NuHorizons-09

5. INO Initiative • In early 2002, a document was presented to the Dept. of Atomic Energy (DAE), Govt of India with a request for fund to carry out feasibility study for setting up an underground neutrino laboratory in India. • In August 2002, an MoU was signed by the directors of seven participating DAE institutes towards working together on the feasibility study for such a laboratory. • A neutrino collaboration group was established with members mostly from Indian Institutes and Universities. • A sum of 50 million INR ( 1 M USD) was allotted by DAE to carry out the feasibility study. • Considering the physics possibilities and given the past experience at Kolar, it was agreed to carry out the feasibility study for a large mass magnetised iron calorimeter which will compliment the already existing water cherenkov based Super-K experiment in Japan. NuHorizons-09

6. INO Collaboration • University of Jammu • Jamia Millia Islamia University • University of Kashmir • University of Mysore • Panjab University • Physical Research Laboratory • Saha Institute of Nuclear Physics • Sambalpur University • Sikkim Manipal Institute of Technology • Tata Institute of Fundamental Research • Variable Energy Cyclotron Centre • Aligarh Muslim University • Banaras Hindu University • Bhabha Atomic Research Centre • Calcutta University • Delhi University • Harish Chandra Research Institute • University of Hawaii • Himachal Pradesh University • Indian Institute of Technology, Chennai • Indian Institute of Technology, Guwahati • Indian Institute of Technology, Mumbai • Indira Gandhi Center for Atomic Research, • The Institute of Mathematical Sciences • Institute of Physics 25 institutions currently in INO collaboration NuHorizons-09

7. INO activities during feasibility study period • Detector R & D: • Choice of active detector • Design of the magnet • Prototyping • Electronics front end and DAQ system • Gas recirculation system • Cost estimate for various components • Site Survey: • History of the site. • Cost factors. • Risk factors and safety issues. • Ownership & site sharing. • Depth • Outreach potential • Local support & awareness NuHorizons-09

8. INO activities during feasibility study period • Numerical simulation: • Development of GEANT3 & GEANT4 based codes for proposed detector geometry • Neutrino generator • Analysis to evaluate physics potential. • Human Resource development: • INO training school • Joint universities training program • Direct recruitment • INO positions/ INO fellowships at various institutions • Ph. D. degree for instrument building NuHorizons-09

9. India-based Neutrino Observatory Proposal Goal:A large mass detector with charge identification capability • Two phase approach: • R & D and Construction • Phase I • Physics studies, • Detector R & D, • 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 NuHorizons-09

10. Neutrino Physics using INO NuHorizons-09

11. Physics using atmospheric neutrinos during Phase I • Reconfirm atmospheric neutrino oscillation • Improved measurement of oscillation parameters • Search for potential matter effect in neutrino oscillation • Determining the sign of Dm223 using matter effect • Measuring deviation from maximal mixing for q23 • Probing CP and CPT violation • Constraining long range leptonic forces • Ultra high energy neutrinos and muons NuHorizons-09

12. 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: = 1 - sin2 (2Q) sin2 (1.27 Dm2 L/E) NuHorizons-09

13. Precision measurement of Dm231 andq23 NuHorizons-09

14. Beyond Superbeam - Neutrino Factory 7000 km NuHorizons-09

15. NF: Golden channel optimisation sin22θ13:5σ sensitivity • Magic baseline (7500 km) good degeneracy solver • Stored muon energy > 20 GeV Patrick Huber: NUFACT06 NuHorizons-09

16. NF: Golden channel optimisation Mass hierarchy: 3σ sensitivity • Baseline: ~7500 km • Stored muon energy 20 – 50 GeV Patrick Huber- NUFACT06 NuHorizons-09

17. Beta Beam from CERN to INO S. Agarwalla et. al. NuHorizons-09

18. INO Detector Specifications NuHorizons-09

19. INO Phase 1 • 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 ) • Charge identification • Ease of construction • Modularity • Complimentarity with other existing and proposed detectors • Use magnetised iron as target mass and RPC as active detector medium NuHorizons-09

20. INO Detector Concept NuHorizons-09

21. Construction of RPC Two 2 mm thick float Glass Separated by 2 mm spacer 2 mm thick spacer Pickup strips Glass plates Resistive coating on the outer surfaces of glass NuHorizons-09

22. ICAL detector Structure NuHorizons-09

23. ICAL Detector Specifications NuHorizons-09

24. First RPC lab at TIFR NIM Gas dist unit Gas filter unit Gas mixing unit Telescope stand CAMAC Tools and jigs NuHorizons-09

25. RPC Test Stand NuHorizons-09

26. Early results NuHorizons-09

27. Cosmic Muon Test using small RPCs DAQ Gas unit Telescope • Streamer mode (R134a=62%, • Argon=30% and the rest Iso-Butane) • Recording hits, timing, noise rates etc Stack of 10 RPCs NuHorizons-09

28. Some interesting events tracked NuHorizons-09

29. Aging: Efficiency drop of a RPC NuHorizons-09

30. Long-term stability tests of RPCs • Two RPCs (J2 & J3) built using 2mm Japanese glass for electrodes • Readout by a common G-10 based signal pickup panel sandwiched between the RPCs • Operated in avalanche mode (R134a: 95.5% and the rest isobutene) at 9.3KV • Round the clock monitoring of RPC and ambient parameters – Temperature, Relative humidity and Barometric pressure • Under continuous operation for more than two years. • Chamber currents, noise rate, combined efficiencies etc are stable NuHorizons-09

31. Effect of SF6 on efficiency & cross talk NuHorizons-09

32. Painting with conductive paint on Glass • Paint developed by • KANSAI-NEROLAC • composition : • Binder (acrylic resin), • Pigments • (conductive black), • (iii) solvents (Aromatic • hydrocarbons and alcohols). NuHorizons-09

33. RPC building blocks NuHorizons-09

34. Making of RPC gap NuHorizons-09

35. RPC fabrication NuHorizons-09

36. RPC Fabrication NuHorizons-09

37. Prototype RPC Stack at TIFR tracking Muons NuHorizons-09

38. Some interesting cosmic ray tracks NuHorizons-09

39. Performances of RPCs NuHorizons-09

40. R & D on Bakelite RPC • With silicone coating • Efficiency plateau >96% obtained • Counting rate decreased • Current decreased NuHorizons-09 40

41. INO Prototype Magnet now at VECC • 12, 1m2 RPC layers • 13 layers of 5 cm thick magnetised iron plates • About 1000 readout channels • RPC and scintillation paddle triggers • Hit and timing information NuHorizons-09

42. Status of RPC R & D R & D for Large size glass RPC is in good shape. 1 m2 size RPCs are now made routinely in the lab. 100 % success rate. All the components needed are locally developed. Prototype electronics including FPGA based self trigger system is operational. A stack of 12 RPCs are continuously recording cosmic muon tracks ( ~ 90K/day). Trigger rate is currently limited by the DAQ band width. Data available on line on the Web. More web-based data monitoring tools will be available soon NuHorizons-09 42

43. INO Simulations NuHorizons-09

44. Detector Simulation • Used NUANCE Neutrino Event Generator • Generate atmospheric neutrino events inside INO detector • Used Atmospheric Neutrino Flux of Honda et. al. • GEANT detector simulation package • Simulate the detector response for the neutrino even • 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. NuHorizons-09

45. Some simulation results NuHorizons-09

46. Hadron Response NuHorizons-09

47. Track Resolution NuHorizons-09 47

48. INO Site NuHorizons-09

49. INO Underground Laboratory NuHorizons-09

50. Location of INO NuHorizons-09