Perspectives of neutrino oscillation physics with long baseline beams
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- Lilian Crawford
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1 Perspectives of neutrino oscillation physics with long baseline beams The European Program OPERA ICARUS The US Program MINOS The Japanese Program JHF-Kamioka Karlsruhe Lucia Votano L.N.F.
2 Neutrino Mass &Oscillation m n 0? Major consequences both for physics and astrophysics New physics beyond S.M. Three hints of nonzero mass: Atmospheric neutrinos ( M to 10-2 ) Solar ( M to 10-4 ) LSND ( M to 10 1 ) SNO Why m «m leptons, m quark? See-saw mechanism Why mixing in lepton»quark? Neutrino oscillation process can only occur if the neutrino has non vanishing mass Only neutrino oscillation can reveal the smallest neutrino masses
3 Neutrino mass scenarios 3 mass eigenstates and e 3 Analysis attempted in order to include solar, atmospheric and LSND in this scenario are controversial and somewhat inconsistent with some of the data. More easy solutions if LSND is set aside 4 mass eigenstates and e sterile 4 From the Z boson width, the fourth must be sterile solar LSND or Generates tension among data subsets atmos Note that oscillations determine only mass splitting not actual masses
4 The 3 ν matrix e U = U U e1 1 1 U U U e2 2 2 U U U e Atmospheric, K2K analysesterms probed by new experiments Solar, reactor analyses cos 13 0 sin 13 cos 12 sin 12 0 = 0 cos sin sin cos sin 23 cos i 23 sin 13 0 cos CP i e e CP Leading oscillations in vacuum P( e )=sin 2 23sin sin 2 23 P( e )=cos 2 23sin sin 2 23 P( )=cos 2 13sin sin m 2 23 L( km) E ν e ν µ is suppressed due to small m 12 2 m 23 2 and θ 23 dominate δ CP is the CP violation phase
5 PRESENT STATUS EXPERIMENTAL RESULTS: Atmospheric Neutrinos Super-Kamiokande Macro Soudan II Long Baseline Neutrino Beam From KEK to Super-Kamiokande 250 Km away, below threshold for production
6 Latest results from Super-Kamiokande and K2K (Lepton-Photon Conference 2001) disappearance in Super-K SuperK < m 2 < 5.4 x 10-3 ev 2 at 90% CL % Best fit m 2 = 2.4 x 10-3 ev 2 Sterile ν disfavoured at ~ 99% disappearance in K2K Expected (no osc.) Detected 44 (~ 2σ effect) Oscillation dip in the E ν spectrum at m 2 ~ 3 x 10-3 ev 2? appearance in Super-K Poor S/B ratio ~ 0.7%, statistical significance ~ 2σ events K2K? energy (GeV)
7 Why long baseline experiments? Check atmospheric neutrino results with a controllable beam See ν τ appearance Measure the product m 2 xθ precision Measure ν µ ν e and θ 13 Constrain or measure ν µ ν s with ~10%
8 The European Long Baseline Program
9 From disappearance to appearance experiments Disappearance Statistical deficit of SuperKamiokande, K2K MINOS at FNAL-Soudan Statistical appearance Apparent excess of NC interactions, imputable to MINOS at FNAL-Soudan Detection of Appearance with low background A new generation of τ detectors and technologies CHORUS and NOMAD at CERN CNGS detectors CNGS beam optimised for appearance (400 GeV proton energy)
10 Motivations Study neutrino oscillations at m 2 > 10-3 ev 2 in the region indicated by SuperKamiokande Establish unambiguously and definitively that the anomaly is due to oscillations by observing appearance in a beam containing negligible at production Search for e oscillations with higher sensitivity than CHOOZ Focussing on appearance: high energy beam optimized for appearance, clear signature, almost background free experiments, no need for near detectors, 730 Km baseline from CERN to Gran Sasso
11 Detection of the - signal and background rejection.. oscillation CC interaction - + X - ν τ ν µ R h - ν τ nπ ο e - ν τ ν e ν τ nπ ο ICARUS: Detailed general picture in Liq. Argon Kinematics ( à la NOMAD ) Momentum unbalance from unseen ν τ in τ decay Energy measurement Simulated event - - o 1 m OPERA: Observation of the decay signature at microscopic scale ( à la CHORUS ) nuclear photographic emulsion (~ 1 m granularity) Decay kink - ~1 mm ν
12 The Experimental Program CNGS: Approved at the end of 1999, civil engineering in progress, first neutrinos expected by 2005 OPERA: Approved in February 2001 (CNGS1), observation of the τ - decay kink in a high resolution detector consisting of emulsion films and lead plates for a mass of 2 Ktons, same technique as the one used by DONUT for the first direct observation of the ν τ charged current interactions (2000) ICARUS: Not yet approved. Liquid Argon TPC, kinematic technique a` la NOMAD, total detector mass of about 5 Ktons, 600 Ton demonstration module being completed, first results The two experiments are a natural continuation of the CHORUS and NOMAD short baseline experiments at CERN but: The conflicting requirements of large scale and at the same time very good space/energy resolution represent a big challenge solved by many years of R&D
13 GeV/c The CERN side
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15 Status of the civil engineering work Excavation is going on smoothly, very good ground conditions so far...
16 CNGS beam characteristics Nominal beam ( m -2 / pot) 7.78x10-9 CC / pot / kton 5.85x10-17 Interactions with 1.8 kton target x 5 years ~ NC+CC < E > ( GeV ) 17 ~ 140 CC (@full mixing, m 2 = 2.5x10-3 ev 2 ) ( e + e ) / 0.87 % / 2.1 % prompt negligible Shared SPS operation 200 days/year 4.5x10 19 pot / year
17 The beam at Gran Sasso CERN FWHM=2.8 Km Flat region 500 m Beam transverse dimensions at Gran Sasso given by -> kinematics: max p T = 30 MeV/c =0.03/E (GeV)
18 The OPERA experiment Brick (56 Pb/Emulsions. cells ) 8 cm (10X 0 )
19 The experimental technique 1 mm Emulsion Cloud Chamber (ECC) ( emulsions for tracking, passive material as target ) Basic technique works charmed X-particle first observed in cosmic rays (1971) DONUT/FNAL beam-dump experiment: ν τ events observed Pb Emulsion layers m 2 = (1.6-4) x10-3 ev 2 ( SuperK) M target ~ 2 kton of compact ECC (baseline) large detector sensitivity, complexity modular structure ( bricks ): basic performance is preserved Ongoing developments, required by the large vertex detector mass: industrially produced emulsion films automatic scanning microscopes with ultra high-speed Experience with emulsions and/or searches : E531, CHORUS, NOMAD and DONUT
20 1947 : discovery Sensitivity of nuclear emulsion discovery with cosmic rays 1971 : charm Emulsion Cloud Chamber (Pb-emulsion sandwich) Charm first seen as X-particle in cosmic ray interactions Nuclear Emulsion: unique to see the decay of short-lived particles X 10 µm 1985 : beauty WA75 hybrid experiment First observation of beauty production and decay 50 years after discovery Automatic scanning, massive targets Search for decay from ν τ interactions - D D - If zero background : 1 event gives a result
21 Material DONUT Fe OPERA Pb better for physics analysis (Fe density : too large or too small)
22 detection by Emulsion-Counter Hybrid Experiments Emulsion gel Track density In emulsion Scan area CHORUS 400 liter 10 4 /cm 2 6x10 4 cm 2 DONUT 50 liter 10 5 /cm 2 2x10 4 cm 2 OPERA 10 4 liter diluted 5000 liter equivalent 10 2 /cm 2 5x10 6 cm 2 10 x CHORUS 100 x CHORUS UTS S-UTS : x 20 # of S-UTS : x 5 Industrial emulsion films ( as for X-rays ) Scanning speed x 10 every few years
23 Microscope for automatic image analysis Computer controlled Multidisciplinary applications: e.g. biophysics Digitised 3D image Third dimension: emulsion thickness CCD camera CCD camera Optics Emulsion Optics ~ mm focal depth optical slice Emulsion mm thickness Movable stage
24 Progress in automatic emulsion scanning Scanning speed road map (Nagoya University) Scanning speed (views/sec, log scale) Scanning speed (view/sec) New tools always made a difference! From B.Kurtén, Our earliest ancestors Columbia University Press (1993) Aim for OPERA ~20 cm 2 /hour/system Road map : speed x 10 every few years At present : Ultra Track Selector ~ 1 cm 2 / h / s R&D in Japan and in Europe
25 Target Tracker task : a) trigger on neutrino interactions b) select bricks efficiently c) initiate muon tagging 10 cm Selected bricks extracted daily using dedicated robot
26 Drift tube trackers Reject charm background Tag and analyse - - candidates 1 m 6.7 m B. B Target Drift Tube trackers muon momentum measurement Magnetised Fe plates + RPC Muon spectrometer (top view )
27 Dipolar spectrometer magnet (weight: ~ 950 ton) Prototype of magnet section being assembled at Frascati B= 1.55 Tesla
28 The detector at Gran Sasso (modular structure, three supermodules ) supermodule spectrometer Magnetised Iron Dipoles Drift tubes and RPCs ~ 10 m module target and decay detector Each supermodule is a sequence of 24 modules consisting of - a wall of Pb/emulsion bricks - planes of orthogonal scintillator strips brick wall scintillator strips
29 Target Trackers spectrometer ν Pb/Em. target Pb/Em. brick A hybrid experiment at work 8 m Basic cell (DONUT) Extract selected brick 8 cm Pb Emulsion 1 mm Electronic detectors select interaction brick ID, charge and p Emulsion analysis vertex search decay search e/ ID, kinematics
30 From the CNGS to physics ν CNGS brick extraction ~30/day cosmic ray exposure emulsion processing no vertex : extract other bricks? vertex search candidate : extract other bricks? Gran Sasso decay search Emulsion read-out facilities (quasi-online ) candidate events ~3/day FULL emulsion analysis Scanning Labs Physics All Labs
31 Exploited decay channels Long decays kink angle kink > 20 mrad Long decays e Progr. Rep Progr. Rep h (n Proposal search 2001 emulsion film plastic base Short decays impact parameter I.P. > 5 to 20 m Pb e Proposal
32 Summary of detection efficiencies (in % and including BR) DIS long QE long DIS short Overall* e h Total (8.7) * weighted sum of DIS and QE events Efficiency given in the Proposal
33 Expected background (5 year run with kton average target mass) e h Total LONG DECAYS SHORT DECAYS Charm production e CC and Large angle scattering Hadron reinteractions CC NC Total Charm production Large angle scattering e CC and 0 « «0.01 Total Total New estimates 0.57 in the Proposal
34 Expected number of events (5 year run with kton average target mass) Full mixing, Super-Kamiokande best fit and 90% CL limits as presented at the 2001 Lepton Photon Conference (update with respect to the EPS 2001 results taken for the written Status Report) Decay mode Signal Signal 2.4*10-3 Signal 5.4*10-3 Bkgnd. e long long h long e short short Total In the Proposal: m x x x 10-3 events
35 Exclusion plot in the absence of a signal (5 year run with kton average target mass) 90 % CL upper limit obtained on average by a large ensemble of experiments m 2 < 1.2x10-3 ev 2 at full mixing sin 2 (2 ) < 5.7x10-3 at large m 2 Gives an indication of the sensitivity but of course we expect to see a signal Uncertainties on background (±33%) and on efficiencies (±15%) accounted for here and in the following
36 Statistical significance for discovery Poisson distribution of the expected background Probability that the b.g. fakes the signal: < P n if #observed events N n Significance (equivalent ) N n #events observed N 4 Events observed P 4 = 6.3x10-5 P 3 = 2.7x events 4 discovery
37 Probability of 4σ significance Simulate a large number of experiments with oscillation parameters generated according to the SuperK probability distribution N 4 events required for a discovery at 4 Evaluate fraction P 4 of experiments observing N 4 events N 4 P 4 m 2 (ev 2 ) Schematic view of the SK allowed region 1 - P 4 sin % 68% 9% Events observed (log scale) years P 3 P % 80% 5 97% 92%
38 Determination of m 2 (mixing constrained by SuperK) 90 % CL limits * m 2 ( 10-3 ev 2 ) Upper limit Lower limit (U - L) / True 41 % 19 % 12 % OPERA 90 % CL in 5 years * assuming the observation of a number of events corresponding to those expected for the given m 2
39 ICARUS liquid argon imaging The ICARUS technique is based on the fact that ionization electrons can drift over large distances (meters) in a volume of purified liquid Argon under a strong electric field. If a proper readout system is realized (i.e. a set of fine pitch wire grids) it is possible to realize a massive "electronic bubble chamber", with superb 3-D imaging. C.R. shower from 3 ton prototype
40 The ICARUS Liquid Ar Time Projection Chamber Event reconstruction in 3D with measurement of the primary ionization 1. drift time 2. induction wires 3. collection wires Space resolution around 1 mm Maximum drift length in the Liq. Ar 1.5 m in the 600 ton module (requiring < 0.1 ppb O 2 equiv. impurities) Calorimetric energy resolution: ( E) E 0.03 E ( Em.) ( E) E 0.12 E ( Hadr.)
41 The ICARUS liquid Ar Image TPC An electronic Bubble Chamber (BC) A interaction in the 50 liters test TPC Large sensitive volume (as BC) Detector = Target (as BC) High spatial granularity (as BC) Energy measurement (as BC) High energy resolution Specific ionisation (de/dx) measurement de/dx vs. range for particle identification Continuous sensitivity Self triggering capability Collection wires Longitudinal plane (46x32 cm 2 ) Induction wires Transverse plane (46x32 cm 2 ) New detector new physics potentialities Under construction : 0.6 kton module proton decay For physics : multi kton atmospheric long baseline solar 0 oscillation Drift time (µs) 400
42 ICARUS 5kton x year physics reach (I) Atmospheric neutrinos Large event statistics with Detection down to production thresholds Complete event final state reconstruction Identification all neutrino flavors Identification of neutral currents Excellent resolution on L/E reconstruction Direct τ appearance search Neutrinos from CERN Search for ν µ ν τ extract m 2 32, 23 m 2 12 m Search for ν µ ν e Solar neutrinos Energy threshold: 5 MeV Large statistics, precision measurements Smoking gun : CC & NC m 2 12, 12
43 ICARUS 5kton x year physics reach (II) Proton decay Large variety of decay modes accessible study branching ratios free of systematics Background free searches linear gain in sensitivity with exposure Neutrino factory Precise measurement oscillation Matter effects, sign of m 2 23 First observation of e CP violation m m 2 32 >0 or m2 32 <0? Unitarity of mixing matrix 0?
44 The ICARUS T600 module 3
45 Internal Detector view Wire Chamber Side B Wire Chamber Side A Drift distance 1.5 m
46 Drift H.V. and field electrodes system Race-track 75kV Horizontal wires readout cables Drift distance 1.5 m E
47 The three wire planes at 0,±60 (wire pitch = 3mm) and one PMT
48 Current T600 status Total run duration in Pavia 3 months (100 days) Day 1 to 10 Day 11 to 15 Day 16 to 20 Day 21 to 30 Day 31 to 45 Day 46 to 55 Day 56 to 65 Vacuum (including leak detection) Pre-cooling Cooling Filling Liquid recirculation Complete detector start-up Data taking with horizontal tracks Big Track Day 66 to 70 Data taking with vertical tracks Day 71 to 75 Data taking with internal trigger only Day 76 to 90 Data taking with DEDALUS triggers Day 91 to 93 Data taking with liquid recirculation on Day 94 to 100 Data taking with 1 kv / cm drift field We are here!
49 ICARUS The T600 is a milestone towards future evolutions. In order not be statistically limited a multi-kton detector is needed for the CNGS. This could come naturally from a cloning strategy of the T600. The option proposed: 2 x T1200 +T600 ICARUS T600
50 ν µ ν τ oscillations (I) Analysis of the electron sample Exploit the small intrinsic ν e contamination of the beam (0.8% of ν µ CC) Exploit the unique e/π 0 separation 8 years of shared running N +jet; Charged current (CC) e Br ~18% m 2 = ev 2 Background: 110 events e N e+jet 470 e CC Charged current (CC) Statistical excess visible before cuts this is the main reason for performing this experiment at long baseline!
51 ν µ ν τ oscillations (II) Reconstructed visible energy spectrum of electron events clearly evidences excess from oscillations into tau neutrino signal e CC Reconstructed energy
52 ν µ ν τ oscillations (II) Reconstructed visible energy spectrum of electron events clearly evidences excess from oscillations into tau neutrino signal e CC Reconstructed energy
53 ν µ ν τ oscillations (III) Kinematical selection in order to enhance S/B ratio Can be tuned a posteriori depending on the actual m 2 For example, with cuts listed below, reduction of background by factor 100 for a signal efficiency 33% e CC Transverse missing P T
54 Search for θ 13 0 (I) m 2 32 =3.5x10 3 ev 2 ; sin = 1 8 CNGS P( ) = cos 4 13 sin P( e ) = sin sin
55 Search for θ 13 0 (II) m 2 32 =3.5x10 3 ev 2 ; sin = 1 ; sin = 0.05 Total visible energy Transverse missing P T P( ) = cos 4 13 sin P( e ) = sin sin
56 Sensitivity to θ 13 in three familymixing 8 CNGS Estimated sensitivity to ν µ ν e oscillations in presence of ν µ ν τ (three family mixing) Factor 5 improvement on sin 2 2θ 13 at m 2 = 3x10 3 ev 2 Almost two-orders of magnitude improvement over existing limit at high m 2
57 The MINOS Experiment Two Detector Neutrino Oscillation Experiment (Start 2004) Near detector: 980 tons Far detector: 5400 tons Iron/Scintillator Sampling calorimeter 1 cm x 4 cm plastic scintillator cm iron plates
58 The neutrino beam SK best fit Oscillation Probability 1st oscillation maximum Target and horn 2 are moveable the beam energy can be changed Need the low energy beam with <E ν > = 7.6 GeV to see 1st oscillation maximum which occurs at 2 GeV
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61 Physics Measurements Obtain firm evidence for oscillations Charge current (CC) interaction rate and energy distribution NC/(CC+NC) ratio (T-test) Measurement of oscillation parameters, m 2, sin 2 2 CC energy distribution Determination of the oscillation mode(s) ν τ or ν s from NC and CC energy distributions ν µ ν e limits or observation by identification of electrons
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65 Limit from the T-test T = N CC N CC like + like N NC like N CC-like events with identified muon N NC-like events with no muon 10 kton-yr exposure 2% overall flux uncertainty 2% CC efficiency uncertainty 2% NC trigger efficiency uncertainty
66 Limit from the CC Energy Spectrum 10 kton-yr exposure 2% overall flux uncertainty 2% bin-to-bin flux uncertainty 2% CC efficiency uncertainty
67 CC Energy Spectrum for various m 2
68 m 2, sin 2 2θ sensitivity 10 kton-yr exposure 2% overall flux uncertainty 2% bin-to-bin flux uncertainty 2% CC efficiency uncertainty For m 2 = ev 2 should be able to achieve better than 10% error at 68% C.L on both m 2 and sin 2 2θ
69 Limit on ν µ ν e MINOS 10 kt-yr 90% C.L. limit Chooz 1999 m 3 > m 2 Matter effects included m 2 solar = ev 2 θ 12 = θ 23 = 45 degrees δ = 0 10% systematic error on background U e3 2 < m 2 > ev 2 sin 2 2θ 13 < m 2 > ev 2 Already close to systematics limited with 10% error on background
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71 JHF-Kamioka neutrino experiment 50 GeV PS machine Super-Kamiokande as a far detector Baseline 295 km Low energy neutrino beam tuned at the oscillation maximum Approved in December 2000 Construction
72 Physics measurements Factor 10 improvement in ν µ disappearance δ(sin 2 2θ 23 )~0.01 δ( m 2 23 )~2x10-4 ev 2 Search for ν µ ν e appearance with a sensitivity 20 times better than CHOOZ limit sin 2 2θµe 0.5 x sin 2 2θ 13 > Search for a small admixture of sterile neutrinos
73 Layout of JHF and the ν beam Narrow Band Beam Off Axis beams Thin solid line shows the WBB A large variety of ν beams is available to tune the energy at the oscillation maximum Neutrino beam energy scan possible Energy peak around 1 GeV Electron neutrino contamination well below 1%
74 ν µ disappearance All events m 2 = ev 2 sin 2 2θ 23 = 1 non-qe events w/o oscillations with oscillations ν energy reconstruction for QE (red) and non-qe interactions The error bar is from the statistics of 5 years
75 ν µ disappearance sensitivity Ratio of measured spectrum with oscillations to the expected one after subtraction of non-qe events Final sensitivity to oscillation parameters: Off Axis 2 beam NBB 1.5 GeV π NBB 3 GeV π
76 ν µ ν e appearance search Signal: ν e (Far)/ν µ (Near) expected to appear at the ν µ disappearance dip Backgrounds ν µ misidentification: negligible ν e contamination ~0.2-03% π 0 (neutral current) background ~0.3% Sensitivity to sin 2 2θ µe > A factor 20 better than the CHOOZ limit
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78 Neutrinos from a muon storage ring A very complex acceleration and storage system ~ 3x10 20 e yr ~ 3x10 20 yr The CERN present scenario
79 Search for long-baseline detector laboratories Optimal baseline is around 3000 km for CP violation + matter effects.
80 Physics from µ e ν e ν µ with a long baseline program at a Neutrino Factory disappearance ( m 2 ) ~ 5 x 10-5 (sin ) ~ 5 x 10-3 e appearance sensitivity down to sin2 2 e ~ Matter effects sign of m 13 CP violation High energy e essential and unique Neutrino interaction rates x 10 or more w/r to present beams Very large detectors needed
Detectors at (1994-1998) CHORUS NOMAD Roberto Petti Neutrino beam NETSCAN location (Phase II): Pick up all track segments (θ < 0.4 rad) in the scanning volume (1.5 x 1.5 mm 2 8 plates) Offline
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