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The Gran Sasso Laboratory and the Neutrino Beam from CERN

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The Gran Sasso Laboratory and the Neutrino Beam from CERN The Gran Sasso laboratory and the neutrino beam from CERN Eugenio Coccia [email protected] Erice 2 september 2006 Content • The Gran Sasso Laboratory • Neutrino physics activity • The Cern to Gran Sasso neutrino beam • First events • Perspectives Underground Laboratories Very high energy phenomena, such as proton decay and neutrinoless double beta decay, happen spontaneously, but at extremely low rates. The study of neutrino properties from natural and artificial sources and the detection of dark matter candidates requires capability of detecting extremely weak effects. Thanks to the rock coverage and the corresponding reduction in the cosmic ray flux, underground laboratories provide the necessary low background environment to investigate these processes. These laboratories appear complementary to those with accelerators in the basic research of the elementary constituents of matter, of their interactions and symmetries. LABORATORI NAZIONALI DEL GRAN SASSO - INFN Largest underground laboratory for astroparticle physics 1400 m rock coverage Research lines cosmic µ reduction= 10–6 (1 /m2 h) • Neutrino physics underground area: 18 000 m2 (mass, oscillations, stellar physics) external facilities • Dark matter easy access • Nuclear reactions of astrophysics interest 756 scientists from 24 countries • Gravitational waves Permanent staff = 70 positions • Geophysics • Biology LNGS most significant results with past experiments Evidence of neutrino oscillation GALLEX / GNO - solar ν MACRO - atmospheric ν Unique cosmic ray studies EAS-TOP with LVD ν beam from CERN: Gravitational OPERA Waves Lisa test Fundamental physics VIP PRESENT EXPERIMENTS Dark Matter ββ decay and rare events Cuoricino DAMA/LIBRA; CRESST CUORE; GERDA WARP; Xenon test Solar ν ν from Supernovae Luna LVD Borexino Borexino ICARUS Occupancy HALL C HALL B LISA MI R&D XENON ICARUS Borexino HALL A BAM - OPERA LVD OPERA DAMA/LIBRA WARP LUNA2 GERDA VIP CRESST LOW ACTIVITY LAB CUORE CUORICINO GENIUS-TF 2004 - 2005 - 2006 Important safety and infrastructures upgrade of the Laboratory • Floor waterproofing • Upgrade of the ventilation system • Realization of containment basins • Upgrade of the cooling capability • Safety measure for the drinkable water • Upgrade of the electrical power Collab.: LVD Large Volume Detector Italy, Brazil, Russia, USA, Japan Running since 1992 1000 billions ν in 20s from the SN core Measurement of neutrinos spectra and time evolution provides important information on ν physics and on SN evolution. Neutrino signal detectable from SN in our Galaxy or Magellanic Clouds 2 - 5 SN/century expected in our Galaxy. Plan for multidecennial observations 1000 tons liquid scintillator + layers of streamer tubes 300 ν from a SN in the center of Galaxy (8.5 kpc) SN1987A Early warning of neutrino burst important for astronomical observations with different messengers (photons, gravitational waves) SNEWS = Supernova Early Warning System LVD, SNO, SuperK in future: Kamland, BOREXINO Large Volume Detector • 3 identical towers in the detector • 35 active modules in a tower • 8 counters in one module SNO (800) LVD (400) Super-Kamiokande (104) MiniBooNE (190) BBoorreexxiinnoo ((8800)) Kamland (330) Tra parentesi il numero Amanda di eventi da una SN al IIcceeCCuubbee centro della Galassia BOREXINO 300 tons liquid scintillator in a nylon bag 2200 photomultipliers 2500 tons ultrapure water Energy threshold 0.25 MeV Real time neutrino (all flavours) detector Measure mono-energetic (0.86 MeV) 7Be neutrino flux through the detection of ν-e. 40 ev/d if SSM Sphere 13.7 m diam. supports 18 m diam., 16.9 m the PM s & optical concentrators height Space inside the sphere contains purified PC Purified water outside the sphere Collab.: Italy, France, USA, Germany, Hungary, Russia, Belgium Poland, Canada Solar, atmospheric, reactor neutrino experiments Emerging picture Tasks and Open Questions • Precision for θ and θ Normal Inverted 12 23 • How large is θ13 ? 3 µ τ 2 e µ τ • CP-violating phase ? Sun • Mass ordering ? 1 e µ τ (normal vs inverted) • Absolute masses ? Atmosphere (hierarchical vs degenerate) • Dirac or Majorana ? Atmosphere • Anything beyond ? 2 e µ τ Sun 1 e µ τ 3 µ τ Gran Sasso 2nd generation neutrino experiments Mass scale / Dirac or Maiorana? (CUORE, GERDA) Oscillation parameters (neutrino tau appearence, unitarity of the mixing matrix , matter effect) (OPERA, ICARUS, Borexino) How small θ13 ? ==> Improve limits (only if θ13 ≠0 and δ ≠0 CP leptonic violation possible) (OPERA) Neutrinoless ββ Decay 0ν mode, enabled ν Standard 2ν mode Some nuclei decay only by Majorana mass by the ββ mode, e.g. 76As 2– 76Ge O+ 76Se 2+ O+ Half life ~ 1021 yr Measured quantity Best limit from 76Ge Neutrino masses and 0ν2β decay Heidelberg Moscow experiment 0.1< mν (0.4) <0.6 eV 4 sigma HV Klapdor et al, NIMA: Data Acquisition and Analysis of the 76-Ge Double Beta experiment in Gran Sasso 1990-2003 CUORE 400 kg cryogenic detector (now Cuoricino 42Kg) to search for double beta neutrinoless events using TeO2 crystals. Approved in 2004 The setup will probe the neutrinoless double beta decay of 76Ge crystals with a sensitivity of T1/2 > 10-24 y at 90% confidence level, corresponding to a range of effective neutrino mass < 0.09 - 0.20 eV within 3 years. Approved in 2005 ββ decay neutrinoless experiments β decay n --> p + e- + ν 2β0ν is a very rare decay: T(half life) ≥ 10-25 years) Upper limit on MIBETA (Milan) ν = ν 20 detectors of natural TeO2 the mass of νe crystals Majorana neutrino 0,39 eV 130Te mass = 2.3 kg CUORICINO Sensitive 130Te mass = 40 kg Heidelberg-Moscow Status: running 11 kg of enriched 76Ge detect. The most sensitive experiment in CUORE the world proposal approved in 2004 76Ge -->76Se + 2e- 130Te mass = 400 kg GENIUS-TF Test facility for GENIUS 40 kg HM Ge Approved: GERDA Sensitive mass: 1 ton enriched Ge crystals in Liquid N2 Cuoricino The CUORICINO set-up, 11 planes of 4 cristals 5x5x5 cm3 and 2 planes 3 having 9 cristals 3x3x6 cm of TeO2 . The total mass is 40 kilograms, one order of magnitude bigger than other cryogenic detector The experiment is in data taking at Gran Sasso With Cuore neutrino mass sensitivity < 10-2 eV (dependent from the model) Now m < 0.4-2 eV Cern Neutrinos to Gran Sasso (CNGS) 1979 Nobody has observed unambiguously the appearance of new flavours. You can’t do it at the solar scale (E too small to produce muons) At the atmospheric scale oscillations are very likely 4 2 2 2 P(νµ → ντ) ≈ cos ϑ13 sin 2ϑ23 sin [1.27 Δm 23L(km)/E(GeV)] Hence, you must be able to identify unambiguously τ leptons CNGS has been designed for it Over the next five years the present generation of oscillation experiments at accelerators with long-baseline beams are expected to confirm the νµ ντ interpretation of the atmospheric 2 2 ν deficit and to measure sin 223 and |∆m 23| within 2 -3 2 10 ÷ 15 % of accuracy if |∆m 23| > 10 eV . Neutrino facility P momentum (GeV/c) L (km) E (GeV ) p.o.t./year (1019) KEK PS 12 250 1.5 2 FNAL NUMI 120 735 3 36 CERN CNGS 400 732 17.4 4.5 K2K and MINOS are looking for neutrino disappearance, by measuring the νµ survival probability as a function of the neutrino energy while OPERA will search for evidence of ντ interactions in a νµ beam. “today” CNGS schedule (schematic, simplified version) 18 August 2006 The 2 ways of detecting τ appearance @GRAN SASSO - - µ ντ νµ ΒR 18 % ….. → + X - ο νµ ντ τ h ντ nπ 50 % - oscillation CC e ντ νe 18 % interaction + - - ο π π π ντ nπ 14% OPERA: Observation of the decay Decay “kink” ν topology of τ in photographic emulsion τ- ντ (~ µm granularity) ICARUS: detailed TPC image in liquid argon and kinematic criteria (~ mm granularity) OPERA: an hybrid detector ν interaction Electronic detector Spectrometer → finds the (drift tubes-RPCs) brick of ν interaction → µ ID, Emulsions+lead + target tracker charge and (scintillator strips) p Basic “cell” Emulsion analysis: Vertex Decay kink e/gamma ID Multiple scattering, kinematics Pb Emulsion 1 mm 8 cm CNGS beam performances 10.5 µs 10.5 µs 50 ms LVD monitor of the CNGS beam Neutrinos from CNGS are observed through: the detection of muons produced in neutrino CC interactions with the surrounding rock or in the detector the detection of the hadron jets produced in neutrino NC/CC interactions in the detector Gran Sasso rock ν LVD µ * µ CNGS beam LVD monitor of the CNGS beam The neutrino candidate are defined as at least a signal from a counter of the detector with an energy deposit greater than 100 MeV. We can discriminate CNGS event from cosmic muons requiring: horizontal direction of the reconstructed muon time coincidence of the event with the CNGS time spill (cosmic muon background is then about 0.2 events/day) From the Montecarlo simulation we expect 6.67 10-16 events/proton on target (p.o.t.) 1 year of data (200 days) -> 4.5 1019 p.o.t. -> 150 events/day The first CNGS event: OνE Event Display: µ from rock Event Display: internal ν NC/CC? LVD rate 7 1 : 4 0 0 , 3 : 8 7 2 2 1 0 : 2 , 9 8 0 1 , 2 0 8 3 : 0 1 2 1 , 8 8 1 Agreement between the observed events and the expected from the beam intensity! Time event distribution The LVD CNGS events time distribution with respect to the time spill agrees with the duration of the spill! The analisys of data taking with the LVD detector shows that: the CNGS beam is working very well as it was expected we continue to collect data and update the results we want to make a deeper analisys of the data to extract more informations (external/internal, CC/NC) OPERA Beam event CC event originated from material in front of the detector
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