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Neutrino Telescopes and Neutrinos from LHC

Neutrino Telescopes and Neutrinos from LHC. Rezo Shanidze University of Erlangen-Nuremberg & IHEPI, Tbilisi State University. ISPM – 2005 Physics at the future colliders 17-21/10/2005, Tbilisi, Georgia. Neutrino Telescope. Detector for registration of high energy

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Neutrino Telescopes and Neutrinos from LHC

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  1. Neutrino TelescopesandNeutrinos from LHC Rezo Shanidze University of Erlangen-Nuremberg & IHEPI, Tbilisi State University ISPM – 2005 Physics at the future colliders 17-21/10/2005, Tbilisi, Georgia

  2. Neutrino Telescope Detector for registration of high energy extra-terrestial neutrinos. High energy extra-terrestial radiation (cosmic rays, gamma radiation, neutrinos) – detected with the help of methods developed in particle physics. High Energy Astrophysics / Astroparticle Physics / Particle Astrophysics: understanding the nature of cosmic high energy phenomena. Energy of the highest energy CR: ECR > 1020 ev (108 TeV ~ x 10 7 LHC beam)

  3. Astroparticle Physics PAO H.E.S.S ANTARES Rezo shanidze

  4. The High Energy Cosmic Radiation gCMB Where and how Cosmic Particles get energy >1019 eV? gCMB Bottom-up models: gCMB Cosmic accelerators - gCMB Most energetic astrophysical Objects: AGN, GRB, SN,…? gCMB Top-down models: Decays of heavy particles, …?

  5. UHECR: EAS/Fluorescence Ei (AGASA/HiRes) Extensive Air Showers EAS Ei(xi,ti) g E(m0,Q,f) MC codes: HEMAS,CORSIKA,… Ep> 1019 eV: p +gCMBg Np GZK cut-off Greisen- Zatsepin- Kuzmin Fluorescence GZK cut-off ? Rezo shanidze

  6. Cosmic Ray Sources ? AGASA UHECR: E> 4 x 1019eV (72 events) 4-10 x1019 eV, E>1020 eV (11 events) ApJ, 522(1999), 225 UHECR and VHE g propagation is affected by CMB radiation. High Energy cosmic neutrinos do not Interact with CMB ! Galactic plane survey by H.E.S.S. VHE g ( > 200 GeV ) p g g g or e + g ge + g ? (Inverse Compton Scattering)

  7. High Energy n-Astronomy Sources of high energy cosmic n: Weak decays of hadrons cosQc= pgm nm 1/bn nm : ne : nt=2 : 1 : 0 m ge nmne n -interactions: n nm :ne : nt =1 : 1 : 1 m(n) W(Z) • + Ngm(n)+X PDF nm CC intearctions: High energy m has a longe range (~ km) in water/ice and produce Cherenkov radiation. • t ~ s0E0.363 s0=7.84x1036cm2 Rezo shanidze

  8. Rezo shanidze

  9. Baukal NT First n Telescope Baikal Neutrino Telescope Russia/Germany (INR, MSU, JINR, … /DESY Zeuthen) BAIKAL NT (36, 96, 192) 1.1 km depth Started: 1993 Fisrt n event 1998-1999 Data 4 km from shore 1070 m deep Rezo shanidze

  10. AMANDAn DetectorAntarctic Muon And Neutrino Detector Array (http://amanda.uci.edu) Location: South Pole Collaboration of 19 Instititions from US/Europe/ Venezuela AMANDA B10 (97-99): 10 strings, 302 OM AMANDA II (2000): 19 strings 677 OM Rezo shanidze

  11. ANTARES n-Telescope for high energies: Qs < 0.3o (Quality of water!) 12 lines 25 storeys/line 3 PMT/storey 900 PMT 0.1 km2 14.5m 2005-2007: deployment of the full detector Rezo shanidze

  12. Rezo shanidze

  13. The Sky View for High Energy NT ANTARES - 2/3 of time: Galactic Centre ANTARES AMANDA Rezo shanidze

  14. High Energy Neutrino Telescopes Baikal ANTARES NESTOR NEMO AMANDA/IceCube Rezo shanidze

  15. km3 scale NT: IceCube @South Pole http://icecube.wisc.edu Collaboration: 9 countries, 26 Institutions. 80 str./ 4800 OM (2010+) Instrumented volume: 1 km3 ~80.000 atm./y Rezo shanidze

  16. The KM3NeT Project KM3NeT project is EU-funded Design Study for km3 NT in the Mediterranenan Sea Consortium: 8 EU countries / 35 Institutions Coordinated by Erlangen University Time Schedule: 02/2006: Start of Design Study mid-2007: Conceptual Design Report End-2008: Technical Design Report 2009-13: Constraction From 2010: Data Taking

  17. High Energy Accelerator Neutrinos Accelerator neutrinos with well defined energy spectra : - significantly improve Neutrino Telescope performance - important role in neutrino physics. VLVnT - sensitive to high energy neutrinos (above ~ 50-100 GeV ) Currently several experiments performed/ planned with high energy accelerator neutrinos: K2K, NuMI/MINOS, CNGS, T2K Long-baseline neutrino experiments.

  18. KM3NeT Design Study • MC simulations in Erlangen: Testing different concepts and options for photodetectors/Optical Modules and design geometry. 2nd Workshop on Very Large Volume neutrino Telescopes Catania, 8-11/2005 Rezo shanidze

  19. Long-baseline n Beams Neutrino telescopes: 103-106 ND ANTARES - ~ 10 Mtone KM3NeT ~ 1Gtone (109 m3 ) E(LHC) > 17.5 E (SPS) Rezo shanidze

  20. NuMI/MINOS Experiment R.Plankett (FNAL), 23/02/2005 Talk @ XI International Workshop on Neutrino Telescopes p gm nm , lp=g ct, g=Ep/mp, ct=7.8m 2.5 1013 p/pulse (1.9s) nm CC Events in MINOS 5kt detector (2.5 x1020 POT/y) Low ~ 1600/yr Medium ~ 4300/yr High ~ 9250/yr Rezo shanidze

  21. NT projects for Mediterranean ANTARES NESTOR NEMO KM3NeT Rezo shanidze

  22. Large Hadron Collider LHC@CERN - from 2007 Beam energy: - 7000 GeV Protons per beam: 4 x1014 • Beam lifetime 14.9 h • Protons/year = • 200 d x(24/14.9)x41014=1.3x1017 • How LHC beams are used: • 1) High Luminosity pp interaction: • ATLAS, CMS exprerimets (~10%) • 2) Low Luminosity pp interaction: • ALICE, LHC-b • 3) Unused (dumped) ( ~ 80%) Rezo shanidze

  23. Neutrinos from High Energyproton-proton Interactions • Neutrino sources: • - Weak decays of hadrons: • unflavored: neutrons, p • Flavored : strange, charm, • bottom • Decays of leptons (m, t) and weak • bosons (W, Z)

  24. Charged Pions and Flavored Particles Charged pions: p (139.5 MeV) BR ( p g mn) = 100 %, l=gct , ct=7.8 m Strange Particles: K(493.7 MeV), KL (497.6) BR(K gmn ) = 63.34 % , ct= 3.7 m BR(KLgpen ) = 38.81 % , ct=15.8 m BR(KLgpmn ) = 27.12 % Charmed mesons: Do(1.865 GeV ), D(1.869 ) , Ds (1.968) BR(Dog eX)=6.9 % ct=123 mm BR(DogmX)=6.5 BR(D±g eX)=17.2 % ct=312 mm

  25. The LHC Interaction Points Beam dumping Arrea pA,14.9 h (Dt: 86 ms), Ecm=114 GeV pp – 25 ns, ~ 109 pp/s, Ecm=14 TeV

  26. Neutrinos from High Luminosity IR • pp interactions @ 14 TeV: PYTHIA 6.2 (minimal bias interactions) • spp=100 mb , ~ 50 p/ pp E ~ 360 GeV 1 mrad angle: • beam pipe: R=25 10-3 m, L=23 m, ~ 1 p/pp, Ep ~ 900 GeV Decay probability: w(p)=1-exp(-L/glp) ~ L/glp , gp=Ep/mp • w(Ep=100 GeV) ~ 4 10-3 • ~ 106nm / sec (X 2 p beams X 2 IR)

  27. Charm Production at LHC ppg 2HC + X gn + X • Charm production at high energies: • Diffractive production (soft process) • - gluon-gluon, quark-antiquark sub-process (QCD) N P Caclucable in QCD: Implemented in MC (PYTHIA) Q P Q

  28. Neutrinos from High Luminosity IR • Neutrinos from • different sources: • a) from p decays • b) from K decays • c) from Charm • particles

  29. Neutrinos from Beam Dumpimg System pA interactions at 114 GeV High energy neutrinos from charmed particles. p - absorbed, strange particles – multiple interctions before decay

  30. Event Rates in Neutrino Telescopes Nn=∫ F(En) sn(En) M(En) NAe(En) dEn F(En) neutrino flux sn(En) neutrino cross-section M(En)=Veff(En)r detector target mass NA Avogadro number e(En) neutrino detection efficiency Nn=∫ F(En)Aeff(En) dEn

  31. Effective Arrea for a Future Mediterranean NT NT: Aeff(En,Q)= Veff(En,Q) (r NA) s(En) e(En)

  32. Neutrino Event Rates • m-neutrino • CC event • Rates in km3 • NT as a function • of energy. • L=1000 km • pp neutrinos • beam dump • neutrinos KM3NeT

  33. Summary and Outlook • LHC proton beams will produce large flux of high energy neutrinos. • A future VLVnT (KM3NeT) in Mediterranean Sea can detect large statistics of LHC neutrinos. • Feasibility study for LHC/KM3NeT neutrino experiment is necesary.

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