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

2. 2 Physics using atmospheric neutrinos during Phase I Reconfirm atmospheric neutrino oscillationReconfirm atmospheric neutrino oscillation Improved measurement of oscillation parametersImproved measurement of oscillation parameters Search for potential matter effect in neutrino oscillationSearch for potential matter effect in neutrino oscillation Determining the sign of  m 2 23 using matter effectDetermining the sign of  m 2 23 using matter effect Measuring deviation from maximal mixing for  23Measuring deviation from maximal mixing for  23 Discrimination between      and     s oscillationDiscrimination between      and     s oscillation Probing CP and CPT violationProbing CP and CPT violation Constraining long range leptonic forcesConstraining long range leptonic forces Ultra high energy neutrinos and muonsUltra high energy neutrinos and muons

3. 3 Physics with Neutrino beam from NUFACT – Phase II Determination of  Determination of   Sign of  m 2 23Sign of  m 2 23 Probing CP violation in leptonic sectorProbing CP violation in leptonic sector Matter effect in      oscillationMatter effect in      oscillation

4. 4 Disappearance of Vs. L/E The disappearance probability can be measured with a single detector and two equal sources: = P(    ; L/E) N up (L/E) N down (L ’ /E) = 1 - sin 2 (2  ) sin 2 (1.27  m 2 L/E)

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

6. 6 Current knowledge on masses and mixing Parameter Best fit 3333  m 2 21 ( 10 -5 eV 2 ) 7.97.1-8.9  m 2 32 ( 10 -3 eV 2 ) 2.21.4-3.3 sin 2  12 0.310.24-0.40 sin 2  23 0.500.34-0.68 sin 2  13 <0.046

7. 7 Precision measurement of  m 2 31 and  23 Experiment |  m 2 31 | Sin 2   Current30%34% MINOS + CNGS 13%38% T2K (5 yrs) 6%22% NO A (5 yrs) 13%42% Combined4.5%20% SK20 (1.84 MTy) 17%24% INO ( 250 KTy) 10%30%

8. 8 Normal or Inverted ?

9. 9 Matter Effect Total no. of  charge current events: Neglecting  21 Where For positive   resonance occurs When  and E are such that   cos2  13 condition is satisfied R. Gandhi et al PRL 94, 051801, 2005

10. 10 Atmospheric Neutrino Events Can be used to study mass hierarchy Can be used to study maximality and octant of  23

11. 11 PePe For negative  31 no resonence occurs for neutrinos, but it occurs for anti-neutrinos

12. 12 Matter Effect Contd

13. 13 Matter Effect & Sign of   from event rate ++ --

14. 14  23 maximality and Octant ambiguity Sin 2   (false) can be excluded at 3  If Sin 2   (true) 0.573 for Sin 2   = 0.04

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

16. 16 INO Detector Concept

17. 17 Construction of RPC Pickup strips Two 2 mm thick float Glass Separated by 2 mm spacer 2 mm thick spacer Glass plates Resistive coating on the outer surfaces of glass

18. 18 The Magnet

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

20. 20 Long term stability of RPCs

21. 21 Cosmic Muon Test Stack of 10 RPCs Gas unit Telescope DAQ Streamer mode (R134a=62%, Argon=30% and the rest Iso-Butane) Argon=30% and the rest Iso-Butane) Recording hits, timing, noise rates etc Recording hits, timing, noise rates etc

22. 22 Some interesting events tracked

23. 23 Scheme of INO prototype detector 12, 1m 2 RPC layers12, 1m 2 RPC layers 6cm thick magnetised iron plates6cm thick magnetised iron plates About 1000 readout channelsAbout 1000 readout channels RPC and scintillation paddle triggersRPC and scintillation paddle triggers Hit and timing informationHit and timing information

24. 24 Location of the Underground Laboratory Studies were performed on two potential sites.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.INO Site Selection Committee after thorough evaluation have now recommended PUSHEP at Tamilnadu as the preferred site for the underground lab.

25. 25 Location of INO

26. 26 PUSHEP

27. 27 Underground Cavern Layout of the Underground Cavern Size of the experimental hall 150 m X 22 m X 30 m Access tunnel Experimental Hall Parking & Storage Electronics Experimental Hall

28. 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 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.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.Physics case for such a detector is strong as evident from recent publications. It will complement the existing and planned water cherenkov detectors.It will complement the existing and planned water cherenkov detectors. Can be used as a far detector during neutrino factory era.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.We have started a very active R & D work towards building such a detector. Looking for participation from international neutrino community.Looking for participation from international neutrino community. For more information on INO please visit the website For more information on INO please visit the website www.imsc.res.in/~ino www.imsc.res.in/~ino

29. 29 THANK YOU