Physics potentials of a magnetized iron calorimeter detector

Transcription

1 Physics potentials of a magnetized iron calorimeter detector Srubabati Goswami Physik-Department T30d Technische Universität München, Germany & Harish-Chandra Research Institute, Allahabad, India INO collaboration CERN, JUNE 006 Srubabati Goswami, CERN, 006 p./5

2 Magnetized Iron Calorimeter Detector Currently feasibility study for such a detector is underway in India by the India-Based Neutrino Observatory (INO) collaboration. Detector choice based on Technological capabilites available in the country Existing/Planned other neutrino detectors in the world Modularity and the possibility of phasing Compactness and ease of construction MONOLITH collaboration had earlier proposed similar design Srubabati Goswami, CERN, 006 p./5

3 The detector Magnetised iron calorimeter ( 50kT) 40 horizontal (vertical) iron layers interspersed with Glass RPC Modular structure Sensitive to muons Energy determination from Track length Track curvature in a magentic field Direction of parent neutrino from the track Charge identification from track curvature in magentic field Srubabati Goswami, CERN, 006 p.3/5

4 Current Activities Detector R & D Physics Studies Detector Simulation Data Acquisition System Site Survey Human Resource Development Interim Report submitted to funding agencies Srubabati Goswami, CERN, 006 p.4/5

5 Cost Estimates and Time Schedule Cost Lab. Construction 90 crores INR ( crore = 0 million) Detector (00 (iron) + 00 (others)) crores in INR Total cost 500 crores in INR ( Euro INR 50) Time Scale : 5 years from approval Details: INO interim report, ino Srubabati Goswami, CERN, 006 p.5/5

6 Site Two sites were considered Rammam in North India and PUSHEP in South India PUSHEP is recommended for ease of accessibility, less seismicity.. Geotechnological studies are going on Srubabati Goswami, CERN, 006 p.6/5

7 Physics Goals for INO First phase measurement of atmospheric neutrino flux Reconfirmation of the first oscillation dip as a function of L/E Improved precision of oscillation parameters Determination of the octant of θ 3 Matter effects and determination of sign of m 3 Probing CPT violation, Lorentz violation Discrimination between ν µ ν τ and ν µ ν s Constraining long range leptonic forces Second Phase end detector for beta beams, neutrino factory hierarchy, θ 3, CP violation CERN to INO baseline 7000 km, the magic baseline Srubabati Goswami, CERN, 006 p.7/5

8 INO as a long baseline detector PUSHEP Rammam JHF (488) (6556) JHF CERN (745) CERN (687).7 3. FERMI LAB (300) FERMI LAB (0480) Srubabati Goswami, CERN, 006 p.8/5

9 Atmospheric Neutrino Oscillation Parameters... Two generation ν µ ν τ oscillation (θ atm θ 3, m atm m 3) ( ) P µµ = sin θ atm sin θ 3 (π/ θ 3 ) symmetry m atm L 4E 0 - m (ev ) 99% C.L. 90% C.L. 68% C.L sin θ Y. Ashie et al. hep-ex/ Srubabati Goswami, CERN, 006 p.9/5

10 Atmospheric Neutrino Oscillation Parameters... Two generation ν µ ν τ oscillation (θ atm θ 3, m atm m 3) ( ) P µµ = sin θ atm sin m atm L 4E θ 3 (π/ θ 3 ) symmetry 0 - Best-fit m atm =. 0 3 ev, sin θ atm =.0 m (ev ) 99% C.L. 90% C.L. 68% C.L sin θ Y. Ashie et al. hep-ex/ Srubabati Goswami, CERN, 006 p.9/5

11 Atmospheric Neutrino Oscillation Parameters... Two generation ν µ ν τ oscillation (θ atm θ 3, m atm m 3) ( ) P µµ = sin θ atm sin m atm L 4E m (ev ) θ 3 (π/ θ 3 ) symmetry % C.L. 90% C.L. 68% C.L sin θ 3σ range ( χ = 9, parameter) m atm = ev, sin θ atm > 0.9 (SK Zenith) spread in m atm = 53% spread in sin θ 3 = 5% Improvement in m atm data Y. Ashie et al. hep-ex/ spread with L/E δ( ) 3% precision is worse than sin θ 3 precision near maximal mixing δ(sin θ) = δ(sin θ) cos θ Srubabati Goswami, CERN, 006 p.9/5

12 Disappearance of ν µ vs L/E down θ θ L N up (L/E) N down (L/E) P µµ = sin θ 3 sin 3 L/4E up Expect to determine 3 with 0% precision Up-rate/Down-rate m (ev ) m = 0.00 ev sin θ = 0.00 Fitted parameters : m = 0.00 ev 0. sin θ = Log 0 (L/E ν ) sin θ Srubabati Goswami, CERN, 006 p.0/5

13 Comparison with Long Baseline Experiments 3σ spread ( m 3 = 0 3 ev, = 0.5). m 3 current 44% 39% MINOS+CNGS 3% 39% TK 6% 3% Nova 3% 43% INO, 50 kton, 5 years 0% 30% Table refers to the older NOνA proposal; the revised March 005 NOνA detector is expected to be competitive with TK. M. Lindner, hep-ph/05030 Srubabati Goswami, CERN, 006 p./5

14 Comparison with Long Baseline Experiments Relative error at σ MINOS ICAL m 3 -precision NOνA TK CNGS SK+KK exluded at 3σ SK+KK TK ICAL -precision CNGS MINOS NOνA SK+KK current data True value of m 3 [0-3 ev ] 3 4 True value of m 3 [0-3 ev ] Srubabati Goswami, CERN, 006 p./5

15 Constraints from future SK Data 5 = 0.34 = 0.38 m 3 [0-3 ev ] = 0.4 = σ spread after 0 SKyr m 3 [0-3 ev ] 4 3 ( 3 = 0.00eV, = 0.5) m 3 = 7% sin θ 3 = 4% m 3 [0-3 ev ] = 0.50 = 0.54 Gonazalez-Garcia et al. hep-ph/ = 0.58 = 0.6 m 3 [0-3 ev ] Srubabati Goswami, CERN, 006 p.3/5

16 Ambiguity in Mass Hierarchy tanθ 3 m = m 3 sinθ 3 m 3 cos θ 3± G F n e E Normal Hierarchy Inverted Hierarchy For m atm > 0 matter resonance in neutrinos For m atm < 0 matter resonance in anti neutrinos m 3 m 3 >0 m m Experiments sensitive to matter effects can probe the mass hierarchy m m 3 <0 Matter effects for m atm channel depend crucially on θ 3 m m 3 Thus both parameters get related Srubabati Goswami, CERN, 006 p.4/5

17 Ambiguity in Mass Hierarchy Hierarchy difficult to determine in superbeams Sensitivity limited by correlation and degeneracies Synergistic use of experiments Use of Magic Baseline M. Lindner, hep-ph/05030 Srubabati Goswami, CERN, 006 p.4/5

18 Earth Matter Effects at Long Baselines Problem of δ CP degeneracy less at longer baselines (a) 9700 Km E (GeV) P µe P µτ P µµ m 3 > Vacuum m 0. 3 < 0 (b) 7000 Km E (GeV) Significant matter effect in P µτ at 9700 km and for E 5 GeV Genuine three flavour effect Impact on P µµ P µµ = P µe P µτ At 7000 km drop in P µµ induced by P µe At 9700 km rise in P µµ induced by P µe and P µτ R. Gandhi et. al, PRL, 005 Srubabati Goswami, CERN, 006 p.5/5

19 Determining Hierarchy by Atmospheric Neutrinos Using µ rates in magnetized iron calorimeter detectors like INO φ µ /φ 0 µ P µµ + rp eµ = P µµ ( r) rp µτ + r For m 3 > 0 matter effect in ν µ (N mat µ + N vac µ + ) r = φ 0 e /φ0 µ Srubabati Goswami, CERN, 006 p.6/5

20 Determining Hierarchy by Atmospheric Neutrinos Using µ rates in magnetized iron calorimeter detectors like INO φ µ /φ 0 µ P µµ + rp eµ r = φ 0 e /φ0 µ = P µµ ( r) rp µτ + r For m 3 > 0 matter effect in ν µ (N mat µ + N vac L = 6000 to 9700 Km, E = 5 to 0 GeV µ + ) L = 8000 to 0700 Km, E = 4 to 8 GeV = 0.00 ev sin θ 3 =0. N µ -, N µ sin θ 3 = 0. 3 = 0.00 ev N µ N µ -m = 04 N µ -v = 6 N µ +m = 03 5 N µ -v = 75 N µ -m = 9 N µ +v = Log 0 L/E [Km/GeV] Log 0 L/E [Km/GeV] Gandhi et al., hep-ph/045 Palomarez-Ruiz, hep-ph/ Murthy,Indumathi hep-ph/ Srubabati Goswami, CERN, 006 p.6/5

21 Determining Hierarchy by Atmospheric Neutrinos Using µ rates in magnetized iron calorimeter detectors like INO φ µ /φ 0 µ P µµ + rp eµ = P µµ ( r) rp µτ + r For m 3 > 0 matter effect in ν µ (N mat µ + N vac µ + ) r = φ 0 e /φ0 µ 3-4σ signal for matter effects at sin θ 3 = 0. for 000kTy using the total event rates for fixed values of parameters Parameter uncertainties spoil the sensitivity Srubabati Goswami, CERN, 006 p.6/5

22 Bin by bin χ -analysis Results for a iron calorimeter detector χ analysis of µ event in 4 L/E bins 5% energy and 5 o angular resolution 0% systematic error 85% efficiency Marginalized over m 3, sin θ 3, sin θ 3 χ min χ min 500 kt yr 000 kt yr Gandhi et al. work in progress. Srubabati Goswami, CERN, 006 p.7/5

23 Bin by bin χ -analysis Results for a iron calorimeter detector χ analysis of µ event in 4 L/E bins 5% energy and 5 o angular resolution 0% systematic error 85% efficiency Marginalized over m 3, sin θ 3, sin θ 3 χ min χ min 500 kt yr 000 kt yr Gandhi et al. work in progress. Effect of Smearing χ (NH vs IH) per 00 events solid: 5% energy resolution dashed: 5% energy resolution µ-like events e-like events solid: 5 o angular resolution dashed: 5 o angular resolution e-like events µ-like events angular resolution [degree] energy resolution [%] Petcov and Schwetz,hep-ph/0577 Srubabati Goswami, CERN, 006 p.7/5

24 Bin by bin χ -analysis Results for a iron calorimeter detector χ analysis of µ event in 4 L/E bins 5% energy and 5 o angular resolution 0% systematic error 85% efficiency Marginalized over m 3, sin θ 3, sin θ 3 χ min χ min 500 kt yr 000 kt yr Gandhi et al. work in progress. Comparison with water-cerenkov detector No charge sensitivity: N µ = N + µ + N µ sin θ 3 χ min (6 Mt yr) Gandhi et al., hep-ph/ Srubabati Goswami, CERN, 006 p.7/5

25 Deviation of from maximal value D / D gives the deviation of sgn(d) gives the octant of Current 3σ limits: D < 0.6 at 3σ from the SK data No robust information on sgn(d) Srubabati Goswami, CERN, 006 p.8/5

26 Can Earth matter effects determine D? P µµ L=000 km =0.50 (matter) =0.50 (vacuum) =0.36 (matter) =0.36 (vacuum) L=7000 km P m µµ = P m µµ P m µµ P m µµ 3 P m µµ = c 3m sin θ 3 sin [.7( 3 + A + m 3)L/E] L=3000 km P m µµ = s 3m sin θ 3 sin [.7( 3 + A m 3)L/E] P µµ L=9000 km L=5000 km P m µµ 3 = sin 4 θ 3 sin θ m 3 sin (.7 m 3L/E) 0.6 P µµ E (GeV) L=000 km E (GeV) Dependence on θ 3 in the form sin 4 θ 3 Octant sensitivity? S.Choubey. and P. Roy hep-ph/ Also Indumathi et al. hep-ph/ Srubabati Goswami, CERN, 006 p.9/5

27 Can Earth matter effects determine D? Using atmospheric neutrinos in INO sin θ 3 (true)=0.0 sin θ 3 (true)=0.0 3 sin θ 3 (true)=0.04 m 3 (true)[0 3 ev ] m 3 (true)[0 3 ev ] MtonY 3.37 MtonY (true) (true) (true) D can be measured to 7%(0%) at 3σ for s 3 = 0.04(0.00) with MtonY exposure and 50% detector efficiency S.Choubey. and P. Roy hep-ph/ Srubabati Goswami, CERN, 006 p.0/5

28 Is the atmospheric mixing maximal? Using long baseline experiments 5 Conventional Beams 5 JPARC SK 5 NuMI off axis 0 3 ev True value of m ev True value of m ev True value of m True value of sin Θ True value of sin Θ True value of sin Θ 3 5 After ten years 5 JPARC HK 5 NuFact II 0 3 ev True value of m ev True value of m ev True value of m True value of sin Θ True value of sin Θ True value of sin Θ 3 Antusch, et al, hep-ph/ Maximality can be tested to 4% at 3σ for m atm = ev after 0 years. Srubabati Goswami, CERN, 006 p./5

29 Is the atmospheric mixing maximal? Using atmospheric neutrino data in SK Sensitivity comes from m driven oscillations Main effect in sub-gev e-effects electron excess 5 (A) Theo+Sys+Stat (B) Sys+Stat (C) Stat only m 3 [0-3 ev ] SK x 0 m 3 [0-3 ev ] 4 3 SK x Gonzalez-Garcia et al, hep-ph/ Also Huber et al. hep-ph/ Maximality can be tested to % at 3σ at all m atm with SK0 Srubabati Goswami, CERN, 006 p./5

30 Resolving the octant ambiguity in INO Using atmospheric neutrinos in INO For every non-maximal (true) there exists a (false) (false) = - (true) 0 Normal Mass Ordering Inverted Mass Ordering sin θ 3 (true)=0.04 sin θ 3 (true)=0.03 sin θ 3 (true)=0.0 sin θ 3 (true)=0.0 χ [ (true) (false)] (true) (true) S.Choubey. and P. Roy hep-ph/ Srubabati Goswami, CERN, 006 p./5

31 Comparing the Octant Sensitivity of Experiments Long baseline experiments No octant sensitivity LBL+atmospheric LBL accelerator + reactor Huber et al hep-ph/ Atmospheric neutrinos in water Cerenkov detectors (false) can be excluded at 3σ if: Minakata et al hep-ph/06058 (true) < 0.36 or > 0.6 Gonzalez-Garcia et al, hep-ph/ Atmospheric neutrinos in large magnetized iron detectors (false) can be excluded at 3σ if: (true) < 0.36 or > 0.63 for sin θ 3 (true) = 0.0, (true) < 0.40 or > 0.59 for sin θ 3 (true) = 0.0, (true) < 0.4 or > 0.58 for sin θ 3 (true) = 0.03, (true) < 0.4 or > 0.57 for sin θ 3 (true) = S.Choubey. and P. Roy hep-ph/ Srubabati Goswami, CERN, 006 p.3/5

32 Detector and Physics Simulation Simulation studies with atmospheric neutrinos are in progress at many collaborating Institutions Nuance Event Generator Generates of atmospheric neutrino events inside the INO detector GEANT Monte Carlo Package Simulates the detector response for the neutrino events Event Reconstruction Fits the raw data to extract neurtrino energy and direction Physics Performance Analysis of reconstructed events to extract physics. Srubabati Goswami, CERN, 006 p.4/5

33 Conclusion A large magnetized iron calorimeter detector has substantial physics potential using atmospheric neutrinos. Reconfirmation of L/E dip and precision of m 3 Matter effect and Sign of m 3 Determination of octant of θ 3 CPT violation, Long Range Forces... It will complement the planned water Cerenkov, Liquid Scintillator and Liquid Argon Detectors as well as the long baseline and reactor experiments Can be used as a far detector for neutrino factories Should be an International Facility Srubabati Goswami, CERN, 006 p.5/5