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MEMPHYS non-oscillation physics

This document presents the MEMPHYS project, a large-scale water Cherenkov detector aimed at studying non-oscillation physics related to supernovae neutrinos. With a total fiducial mass of 440 kt and unique cylindrical module design, the experiment aims to explore crucial topics such as core-collapse supernovae, diffuse supernova neutrinos, proton decay, and various neutrino detection methods. The work emphasizes advancements in PMT technology and analyses of neutrino oscillation parameters, contributing significantly to our understanding of astrophysical sources of neutrinos.

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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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