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

2. 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 • Discrimination between nm nt and nm  ns oscillation • Probing CP and CPT violation • Constraining long range leptonic forces • Ultra high energy neutrinos and muons

3. Physics with Neutrino beam from NUFACT – Phase II • Determination of q13 • Sign of Dm223 • Probing CP violation in leptonic sector • Matter effect in nm ntoscillation

4. 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)

5. Confirmation of Oscillation of Atmospheric Neutrinos The first oscillation dip should be clearly visible

6. Current knowledge on masses and mixing

7. Precision measurement ofDm231 andq23

8. Normal or Inverted ?

9. Matter Effect R. Gandhi et al PRL 94, 051801, 2005 Total no. of nm charge current events: Neglecting D21 Where For positive D31 resonance occurs When r and E are such that A=D31cos2q13 condition is satisfied

10. Atmospheric Neutrino Events • Can be used to study mass hierarchy • Can be used to study maximality and octant of q23

11. Pme For negative D31 no resonence occurs for neutrinos, but it occurs for anti-neutrinos

12. Matter Effect Contd

13. Matter Effect & Sign ofD31 from event rate m- m+

14. Q23 maximality and Octant ambiguity Sin2q23 (false) can be excluded at 3s If Sin2q23 (true) <0.421 or >0.573 for Sin2q13 = 0.04

15. CPT Violation The expression for survival probability for the case of CPTV 2-flavour oscillations and

16. INO Detector Concept

17. 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

18. The Magnet

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

20. Long term stability of RPCs

21. Cosmic Muon Test 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

22. Some interesting events tracked

23. Scheme of INO prototype detector • 12, 1m2 RPC layers • 6cm thick magnetised iron plates • About 1000 readout channels • RPC and scintillation paddle triggers • Hit and timing information

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. Location of INO

26. PUSHEP

27. 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

28. Summary • A large magnetised detector of 50-100 Kton is needed to achieve some of the very exciting physics goals using atmospheric neutrinos. • A case for such a detector was highlighted earlier by the Monolith Collaboration. • 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. For more information on INO please visit the website www.imsc.res.in/~ino

29. THANK YOU