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MEMPHYS non-oscillation physics

NOW 2006 - Conca Specchiulla 9-16/09/06. MEMPHYS non-oscillation physics. Alessandra Tonazzo APC et Université Paris 7. 65m. 60m. The MEMPHYS detector. [see talk by S.Katsanevas]. Modane, France. Megaton Mass PHYSics @Fréjus Water Cherenkov (“cheap and stable”)

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MEMPHYS non-oscillation physics

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  1. NOW 2006 - Conca Specchiulla 9-16/09/06 MEMPHYSnon-oscillation physics Alessandra Tonazzo APC et Université Paris 7

  2. 65m 60m The MEMPHYS detector [see talk by S.Katsanevas] Modane, France Megaton Mass PHYSics @Fréjus • Water Cherenkov (“cheap and stable”) • Total fiducial mass: 440 kt • Baseline: 3 Cylindrical modules 65X65 m • Size limited by light attenuation length (λ~80m) and pressure on PMTs • Readout: 12” PMTs, 30% geom. cover (#PEs =40%cov. with 20” PMTs) • PMT R&D + detailed study on excavation existing & ongoing Laboratoire Souterrain de Modane Frejus Tunnel 4800 m.w.e. Bardonecchia, Italy http://www.apc.univ-paris7.fr/APC_CS/Experiences/MEMPHYS/ arXiv: hep-ex/0607026 Contacts: J.E.Campagne and M.Mezzetto A.Tonazzo - MEMPHYS: non-oscillation physics

  3. Physics goals (=outline of my talk) • SuperNovae core-collapse • Early SN trigger • Diffuse SuperNovae Neutrinos • Astrophysical sources of neutrinos • Proton decay • Oscillation measurements with  beams [see talk by T.Schwetz] A.Tonazzo - MEMPHYS: non-oscillation physics

  4. EARTH Flavor conversion n emission Shock wave SN neutrinos @ detector [slide “stolen” from A.Mirizzi] Core Collapse Event rate spectra [see talk by Cardall] • f: from simulations of SN explosions • P : from n oscillations + simulations (density profile) • s : (well) known • e : under control A.Tonazzo - MEMPHYS: non-oscillation physics

  5. SN neutrinos [see talk by Cardall] • Neutronization burst • E~1051 erg t~25 ms • Accretion + K-H cooling • E~1053 erg t~10 s • 99% of total explosion energy Propagation to Earth: • Matter effects Pee(12) • Level-crossing probability PH(E, V(x,t), m2,13) • Survival prob. p= Pee*PH “Sensitivity to θ13 one order of magnitude better than planned terrrestrial experiments” [see for ex. Lunardini-Smirnov hep-ph/0302033] Hierarchy of interaction strength  Fogli et al., hep-ph/0412046 Raffelt et al., astro-ph/0303226 A.Tonazzo - MEMPHYS: non-oscillation physics

  6. Detection of SN neutrinos e+ • Inverse-beta (89%) • Large statistics in detectors with lots of free p • Good determination of  time and energy • Option: add Gd to tag neutron from delayed-γ • Elastic scattering (~3%) • Pointing • NC on Oxygen (8%) n g [see talk by Vagins] e- ne,x Fogli et al., hep-ph/0412046 A.Tonazzo - MEMPHYS: non-oscillation physics

  7. SN @ MEMPHYS Evidence up to ~1Mpc Galactic SN: Huge statistics  we can do spectral analyses • in time • in energy • in flavour composition  Access to • SN explosion mechanism: shock waves, neutronization burst • Neutrino production parameters: rate, spectra • Neutrino properties (a partial overview in the following) Fogli et al., hep-ph/0412046 A.Tonazzo - MEMPHYS: non-oscillation physics

  8. SN spectral analyses (1) • Extracting the astrophysical parameters • Learning about black-hole formation • Abrupt cut-off of neutrino flux visible if a black-hole forms in the middle of a SN explosion Just an example (“old” paper) to get a feeling of the sensitivity w.r.t. smaller detectors Minakata et al., hep-ph/0112160 from UNO whitepaper A.Tonazzo - MEMPHYS: non-oscillation physics

  9. SN spectral analyses (2) • Learning about the shock wave Shock-wave effects on survival probabilities (PH) depend on 13. Crossing of resonances can induce time-dependent matter effects in neutrino oscillations m2atm,13 m2sol,sol  self-interactions ? Duan et al., 0606616 Raffelt et al., 0608050 Schirato and Fuller, astro-ph/0205390 Fogli et al., hep-ph/0304056 A.Tonazzo - MEMPHYS: non-oscillation physics

  10. SN spectral analyses (2) • Learning about the shock wave “Double-dip” in <Ee> “Double-peak” in <E2e>/<Ee>2 vs time Time-dips are Energy-dependent: Compare bins of “low” and “high” E Fogli et al., hep-ph/0412046 Forward shock Forward+Reverse shock IH shock IH static NH For NH, some information can be gathered from time-spectrum of e+O events Tomas et al., astro-ph/0407132 A.Tonazzo - MEMPHYS: non-oscillation physics

  11. SN spectral analyses (2’) • Stochastic density fluctuations behind the shock front can have significant damping effects on the transition pattern and modify the observed spectrum Fogli et al., hep-ph/0603033  = fractional (random) variations of average  potential A.Tonazzo - MEMPHYS: non-oscillation physics

  12. SN spectral analyses (3) • Earth matter effects Dighe et al., hep-ph/0311172 Modulations of energy spectrum of and/or Observable with a single detector in Fourier-transform of y~1/E In water-Cherenkov, due to poor energy resolution, need >60k events: OK @Mton For Earth effect not seen  Inverted Hierarchy + large θ13 Earth effect seen  Degeneracy: NH or IH+small θ13 A.Tonazzo - MEMPHYS: non-oscillation physics

  13. SN spectral analyses (4) • Neutronization burst Kachelrieβ et al., astro-ph/0412082 • Signal: • Bkg: • mainly • rejected by angle and E cuts + Gd n-tag • ES of other  flavours Observation of time peak depends on oscillation scenario • Burst / no-burst  break degeneracy A/C if θ13 unknown • Measurement of SN distance D~1/N1/2 @10kpc within 5% A.Tonazzo - MEMPHYS: non-oscillation physics

  14. SN trigger Detection of SN from galaxies up to ~10Mpc • Coincidence of two neutrinos in the same detector within ~10sec • Bkg <0.7 ev/yr • Rate > 0.15/yr  Identify SN without optical confirmation (= anticipate by few hrs)  Detect SN heavily obscured by dust or optically dark • Neutrino-Optical coincidence  improve knowledge of start time of core collapse from ~1day (optical) to ~10s @Mton RSN @SK Ando et al., astro-ph/0503321 A.Tonazzo - MEMPHYS: non-oscillation physics

  15. Diffuse SN neutrinos We don’t need to wait and hope to be lucky… [see talk by C.Lunardini] (thanks for these slides!) Lunardini, astro-ph/0509233 A.Tonazzo - MEMPHYS: non-oscillation physics

  16. Diffuse SN ’s @H2O detectors Small signal over very large bkg: • Decay e from “invisible ” generated by CC interaction of -atm and with E<Cherenkov threshold • atmospheric e • Reactor (E<~10 MeV) Can be reduced with Gd (reject non- anti-e ) Malek et al. [SK Coll.], hep-ex/0209028 A.Tonazzo - MEMPHYS: non-oscillation physics

  17. We WILL see them in few years Direct measurement of  emission parameters Diffuse SN ’s @ MEMPHYS 5y SK+Gd =1y MEMPHYS+Gd Fogli et al., hep-ph/0412046 7-60 events in 4 yrs: “most conservative” estimate by C.Lunardini What can we learn ? astro-ph/0509233 Yuksel et al., astro-ph/0509297 A.Tonazzo - MEMPHYS: non-oscillation physics

  18. Decays of DSN modifications of spectrum Constraints on Dark Energy parameters Diffuse SN ’s @ MEMPHYS +estimate of SN rate from future SN surveys 10 y with Gd Mirizzi et al., hep-ph/0405136 Hall et al., hep-ph/0607109 A.Tonazzo - MEMPHYS: non-oscillation physics

  19. Neutrino astrophysics • Low-E ’s from GRB • accompanying UHE-’s and optical emission seen in other experiments • “GRB  background” detectable in few years • ’s from Black-Hole formation death of stars with M>40Msun • ’s from interaction of ’s “from below” • Point-sources, such as AGNs • WIMPs annihilating in Earth, Sun or Galaxy [cfr SK analysis: hep-ex/0404025] • High-E ’s from GRBs Nagataki et al., astro-ph/0203481 Sumiyoshi et al., astro-ph/0608509 A.Tonazzo - MEMPHYS: non-oscillation physics

  20. Proton decay Complete review: Nath and Perez, hep-ph/0601023 • Forbidden in SM • Non-SUSY GUTs (dim-6 operators) • Favours p  e+0 • Predictions: p~1034-1036 yrs • Predictions depend only on fermion mixing • SUSY GUTs (dim-4 and dim-5 operators) • Favours p  K+ nu-bar • Predictions: p~3x1033-3x1034 yrs • Predictions depend on SUSY particle spectrum, Higgs sector and fermion masses (note interplay with direct searches @LHC) Current limits by SuperKamiokande: • p  K+ nu-bar p>2.3x1033y • p  e+0p>1.6x1033y • Complementarity of the two main decay channels • No dedicated study done for MEMPHYS: rely on UNO simulation results (see UNO whitepaper) A.Tonazzo - MEMPHYS: non-oscillation physics

  21. Proton decay • Search for p  e+ π0 • Main bkg: • Ask: 2 or 3 “e-like” rings, Ptot<PFermi, Minv~Mp • => Eff. ~44% • MEMPHYS coverage 30% with 12”PMTs is equivalent to SK coverage 40% with 20”PMTs in terms of #PE H2O is best for this channel MEMPHYS XXX XXX MEMPHYS From UNO whitepaper A.Tonazzo - MEMPHYS: non-oscillation physics

  22. Proton decay • Search for p  K+ + anti- • K below Ch. Threshold : infer from decays 90% of K decay at rest K decay channels: • K  monoenergetic  • + 6.3 MeV prompt- from capture • K +0 with  H2O is not as good as LAr, LScint for this channel A.Tonazzo - MEMPHYS: non-oscillation physics

  23. Summary and outlook MEMPHYS - Megaton Mass PHYSics @ Fréjus • Supernova Explosion • Evidence up to 1 Mpc • Spectral analyses  information on explosion mechanism,  emission and propagation • Diffuse Supernova Neutrinos • Evidence within few years • Information on  emission parameters and more • Early SN trigger • Neutrino astrophysics • Proton decay: • Optimal detector for p  e+ π0 • Important synergies with LAr, LiqScint  LAGUNA A.Tonazzo - MEMPHYS: non-oscillation physics

  24. BACKUP

  25. SN spectral analyses (2) • Learning about the shock wave: Normal Hierarchy A.Tonazzo - MEMPHYS: non-oscillation physics

  26. SN187A by Lunardini A.Tonazzo - MEMPHYS: non-oscillation physics

  27. SN1987A Yukserl et al., astro-ph 0509297 Other analyses: Jegerlehner et al., PRD 54 (1996) 1194 Lunardini, astro-ph/0509233 (5-par fit) A.Tonazzo - MEMPHYS: non-oscillation physics

  28. SN spectral analyses (2) • Learning about the shock wave Time-dips are Energy-dependent: Compare bins of “low” and “high” E “Double-dip” in <Ee> “Double-peak” in <E2e>/<Ee>2 vs time Fogli et al., hep-ph/0412046 Tomas et al., astro-ph/0407132 A.Tonazzo - MEMPHYS: non-oscillation physics

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