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Neutrino mixing at high energy neutrino telescopes

Neutrino mixing at high energy neutrino telescopes. Pasquale D. Serpico MPl –Munich CARE ’05 - ECFA/BENE. Overview of the Talk. Neutrino telescopes: an overview. Neutrino mixing at neutrino telescopes. “Galactic b -beams” and muon-damped sources. Conclusions.

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Neutrino mixing at high energy neutrino telescopes

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  1. Neutrino mixing at high energy neutrino telescopes Pasquale D. Serpico MPl –Munich CARE ’05 - ECFA/BENE

  2. Overview of the Talk • Neutrino telescopes: an overview • Neutrino mixing at neutrino telescopes • “Galactic b-beams” and muon-damped sources • Conclusions P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  3. Neutrino-telescopes: an overview

  4. High-Energy n astronomy: a new sky Neutrinos: a powerful tool for high energy astrophysics +)Directional signal (differently from CR) +)No absorption (differently from g) +) HEn guaranteed (HECR & HEg observed) Main problem -)Small s P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  5. Solutions (I) • o huge volumes • sparse instrumentation • natural media 1 km3: Gigaton scale! 300 m 1500 m 50 m IceCube Collaboration 2500 m P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  6. Status of Optical Cherenkov Telescopes 80’s: DUMAND R&D 90’s: BAIKAL, AMANDA, NESTOR 2k’s: ANTARES, NEMO R&D <2010: ICECUBE (km3 at the SouthPole) ……? Mediterranean km3 (Km3Net) Baikal BAIKAL Pylos Mediterranean km3 DUMAND La Seyne South Pole Capo Passero AMANDA ICECUBE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  7. Flavour discrimination (I) 1st detection channel: O(km) m tracks directional error: ~ 1° σ[log10(E/TeV)]: ~ 0.3 coverage: 2 energy range: ~ 50 GeV to 100 PeV nm + N →m + X (DIS) optical sensors (PMT) Cherenkov light cone (blue light) P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  8. Flavour discrimination (II) 2nd detection channel: cascades from ne & n CC + all flavors NC directional error: ~ 10-40° σ[log10(E/TeV)]: ~ 0.1 coverage: 4 energy range: ~ 1 TeV to 100 PeV ne + N → e + X (DIS) P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  9. Flavour discrimination (III) - ne+ e-→W- → anything - Unique to ne s enhanced at E ≈ 6.3 PeV - s(ne N) nt + N →t + X (DIS) “Glashow Resonance” E > few PeV Gandhi et al. ‘95 P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  10. Solutions (II) 3000 km2 P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  11. Upgoing ntshower (seen by Los Leones telescope) P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  12. Solutions (III) n ANtarctic Impulsive Transient Antenna 600 km radius, 1.1 million km2 P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  13. n-mixing at n-telescopes

  14. n-telescopes and n-mixing Standard Paradigm: Neutrino mixing studies hopeless at high energy neutrino telescopes Astrophysical n fluxes come from pp→pX pg→pX flavour ratios at source →fe:fm:ft≈⅓:⅔:0 at Earth after oscillations → fe:fm:ft≈⅓:⅓:⅓ quite insensitive to mixing parameters dsource>> Losc → no sensitivity to Dmsol2 , Dmatm2 I shall try to argue that this is misleading! P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  15. n-telescopes and n-mixing 4. “Peculiar” (but not “exotic”!) neutrino sources may exist sensitive to mixing parameters (including q13and dCP) • Standard oscillation phenomenology “rescues” signals, allowing some interesting measurements • Matter effects might imply observations sensitive to Dm2’s, e.g. to hierarchy 3. Input from n-mixing very important for diagnostics of astrophysical sources Only standard oscillation scenarios considered! P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  16. A “rescued” signal: The Galactic diffuse nt Independent confirmation of the (large) mixing in the m-t sector via nt appearence H. Athar et al. APP 18 (2003) 581 n-flux from CR hitting Galactic matter develops a large nt-component via oscillations. Atmospheric n background is o softer (relevant energy losses of mesons) o n t-suppressed (prompt nt) Losc(E≈TeV-PeV)is too large Event rate of O(1 yr-1 sr-1) for two separable and contained showers with E ≈ PeV in a km3 n-telescope P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  17. Earth matter effectwith a SN at IceCube Flux vs. time at IceCube + SK (or HK) can detect Earth matter effects (normal hierarchy and sin2q13 >10-3) Exploits high statistics for a galactic SN Dighe et al. 06 (2003) JCAP 005 Livermore Garching P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  18. n-telescopes, the Glashow resonance and q12 - “Standard” astrophysical sources produce both n and n via pp→pX pg→pX Both give flavour ratios at production fe:fm:ft≈⅓:⅔:0 but pgmainly gives ne (via p+), while pp almost equally ne and ne - The measurable ratio RGR ≡ neGR/(nm+nm)CC≈ 15[Sin2 2q12 +k(1-0.5 Sin2 2q12)] (q13=0oand q23=45o) is sensitive both to mixing angles (mainly q12) AND to the production mechanism (% of pp “contamination” ≡ k) (Bhattacharjee & Gupta, astro-ph/0501191) - - P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  19. n-telescopes, the Glashow resonance and q12 • q12=45o q12=32.5o q12=15o q12=0o • ------ q23=40o • q23=45o • q13=0o • q12=45o q12=32.5o q12=15o q12=0o • q23=45o • ------ q13=9o • q23=0o P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  20. “Peculiar” high energy neutrino (re)sources - 1. neutrons beams from nuclear dissociations → purenebeam - 2. pion beams from muon damped sources → purenm+nmbeam In both cases, the observable ratio of m tracks to e+t showers fm (fe+ft) is sensitive to crucial information of the neutrino mixing matrix !!! R= P.S. & M. Kachelrieß PRL 94, 211102(2005) [hep-ph/0502088], P.S., work in progress P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  21. Neutrino Mixing - Probabilities Flavor ratios at detector Flavor ratios at source slk≡ Sin qlk , clk≡ Cos qlk Mixing Matrix U • Matter effects negligible • dsource>> Losc :Terms sensitive to Dm2, sign(dCP) average out • Also imply equal expressions for neutrinos and antineutrinos P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  22. “Galactic b-beams”

  23. Sensitivity to q13 (and q23) Pem Rº = Pee+Pet fm (fe +ft) Note the octant dependence! q12=p/6 q23=p/4 Variation of order 25-50% in 0o<q13< 10o, depending on q23 (q12=32.5o, best case dCP=0) For q23=45o, R is reduced even to ½ of the canonical R=0.5 P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  24. Sensitivity to dCP For experimental best fit q12=32.5o andq23=45o, the flux ratio has a maximal variation of about 30% NOTE: only sensitive to Cos (dCP) [CP-even term] not “direct” observation of CP-violation P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  25. Determination of the octant of q23 Pem R= Pee+Pet R<0.21 → q23 > p/4 Backgrounds can only increase R! Model-independent statement P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  26. Neutrinos from nuclei in the Galaxy L. Anchordoqui et al. Ann. Phys. 314 (2004) 145 In cosmic rays, at E ≈ O(1 EeV) a transition between High-Z nuclei of the Galactic spectrum (acceleration and confinement requirements are alleviated) and p-dominated Extragalactic contribution is expected. Recent CR data support this scenario n from nuclei dissociations in matter and g-fields in (a few) galactic accelerators might become visible at EeV. Favored regions: Nuclear Bulge, dense clouds (high B-field) … P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  27. Hint: A Galactic Plane excess in EeV Cosmic Rays AGASA reported a 4% excess in UHECR around 1018 eV (1 EeV) from a couple of hot-spots in the galactic disk Similar, indepentent hints also from SUGAR and Fly’s Eye (but negative results from preliminary analysis of Auger data) P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  28. The birth of Galactic neutron Astronomy? Harari et al. JHEP 9908 Neutrons are natural candidates to explain the signal no GMF bending (huge for p too!) Energy-range of the Signal ≈ boosted n-lifetime ctn≈ 10 kpc (En / EeV) P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  29. From Neutrons to Neutrinos The existence of galactic neutron beams would imply ne fluxes up to the PeV from n-decay. (En/ En ~ Q / mn ~ 10-3→ En ~ PeV, for En ~ EeV) - Notice that n are undetectable as CR anisotropies below E~ 1017 eV: similar sources of lower Energy might show-up only in the ne channel !!! - If neutrons come from nuclear photodissociations on Optical/UV photons, the flux is likely to extend down to(at least)TeV region This energy range nicely fits the energy-window accessible to n-telescopes under construction. P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  30. A model of galactic neutron beams

  31. Detectability in IceCube Normalizing to the CR anisotropy, ~ 20 events per year from Cygnus region in IceCube (under construction at the South pole) Standard noscillation phenomenology implies ≈ 4nm/yr tracks in 0.7o circle (Atm. background is~2.3 nm/yr) ≈ 16ne+ntshowers/yr in 25o, cone, due to poor resolution. (Atm. background fluctuation is~12 ne+nt/yr) In a few years, IceCube should attain discovery sensitivity for n→ne→nm!!! L. Anchordoqui, H. Goldberg, F. Halzen & T.J. Weiler PLB 593 (2004) 42 P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  32. How large is the expected “pion contamination”? Viable models of A → n →n scenarios exist, e.g.: Cygnus region: L. Anchordoqui et al. PLB 593 (2004) 42 SGR A East SN remnant: Grasso and Maccione [astro-ph/0504323] From astrophysical data e.g. on the Cygnus region (e.g. UV g density) and hadronic physics data (e.g. secondary population yields in hadronic interactions) Vnuclear dissociation ≈ 27 xVpp hadronic interactions In this case, likely p contaminations to n flux are at the O(10%) level →DR ≈ + 0.02 only! Within the expected statistical accuracy of IceCube & at the same subleading level of other effects neglected in our estimate P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  33. Is this scenario falsifiable? Normalizing the anisotropy to the “n-chain” model, n →n-fluxes should easily observable in IceCube, with a detailed measurement in a decade. If the p-chain dominates, the flux should be much higher, though with a flavour ratio of about 1:1:1 Also g-rays constraints! High n flux and R=0.5 would disprove the dominance of A →n→n! P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  34. muon-damped sources

  35. Sensitivity to the octant of q23 Pmm Rº = 1-Pmm fm (fe+ft) R>0.78 → q23 > p/4 Backgrounds can only decrease R! Model-independent statement P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  36. Why pion beams? Effective “pion beams” produced in sources where muons (but not pions) are damped sources → purenm+nmbeam - Boosted Lifetime µ E E.m. cooling time µ E-1 (Inv. Compton), E0 (adiabatic expansion),… Their ratio increases with E, at a certain e0 the particle is stopped before decaying. The lifetime implies e0m << e0p For AGN, p beams @ O(106) TeV → unobservable at OCT For GRB, p beams possibily @ O(10) TeV→ optimal for OCT!!! Flavour ratios can be used for astrophysical diagnostics Kahsti & Waxman, PRL 95 (2005) 181101 P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  37. Concluding remarks

  38. Overview - I Neutrinotelescopes are optimized for astrophysical purposes, but they may have a potential for n-mixing physics, too. nt appearence expected to be seen within 3-4 years (IceCube completed + 1 year of running) “Calorimentric” detection of a galactic core-collapse SN possible. Earth matter effect (and thus hierarchy/q13) possibly identified at IceCube+”HK”, or +Mediterranean km3 P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  39. Overview - II I showed that it is conceivable or even likely that Nature might provide “b-beams” (or pion beams) for free, that could be studied at n-telescopes already in construction. Measurable flavor ratios are sensitive to q13, dCP , and to the octant of q23 . The latter is particularly suitable for a model-independent determination (if q23 > p/4) Going beyond the paradigm of a “canonical” flavor equipartition would repropose at neutrino telescopes the fruitful synergy between neutrino physics and astrophysical diagnostics P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  40. Synergy between Earth & Heaven THANK YOU!

  41. Neutrino mixing parameters Solar/Kamland Best Fit:Sin2qsol=0.29, Dmsol2=8.1 x 10-5 eV2 3 s range: 0.23 < Sin2q12 < 0.37, 7.3x 10-5<Dmsol2/eV2 < 9.1 x 10-5 Best Fit: qsol= 32.6° 3 s range: 28.7 °< qsol <37.5° Atmospheric/K2K Best FitSin2 qatm=0.5, Dmatm2=2.2 x 10-3 eV2 3 s range 0.34 < Sin2qatm < 0.66; 1.4 x 10-3 <Dmatm2/eV2 < 3.3 x 10-3 Best Fit: qatm= 45° 3 s range: 35.7 °< qsol <54.3° Global (CHOOZ+others) Best Fit: Sin2q13 =0 3 s range:Sin2q13<0.047, q13 <12.5° Maltoni et al., NJP 6 (2004) 122 P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  42. s(nN) vs. E R. Gandhi, C. Quigg, M. H. Reno and I. Sarcevic, Neutrino interactions at ultrahigh energies, Phys. Rev. D 58, 093009 (1998) [hep-ph/9807264]. P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  43. - s(nN) vs. E R. Gandhi, C. Quigg, M. H. Reno and I. Sarcevic, Neutrino interactions at ultrahigh energies, Phys. Rev. D 58, 093009 (1998) [hep-ph/9807264]. P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

  44. Clarification on dCP Jarlskog determinant CP-even CP-odd Apollonio et al. hep-ph/0210192 P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE n telescopes” 23-25/11 /05 ECFA/BENE Week – CERN

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