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HiRes Limits on the Tau Neutrino Flux at the Highest Energies

HiRes Limits on the Tau Neutrino Flux at the Highest Energies. HR2. HR1. Kai Martens High Energy Astrophysics Institute Department of Physics, University of Utah for the HiRes Collaboration. The Collaboration:.

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HiRes Limits on the Tau Neutrino Flux at the Highest Energies

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  1. HiRes Limits on the Tau Neutrino Flux at the Highest Energies HR2 HR1 Kai Martens High Energy Astrophysics Institute Department of Physics, University of Utah for the HiRes Collaboration

  2. The Collaboration: S. BenZvi, J. Boyer, B. Connolly, C.B. Finley, B. Knapp, E.J. Mannel, A. O’Neill, M. Seman, S. Westerhoff Columbia University J.F. Amman, M.D. Cooper, C.M. Hoffman, M.H. Holzscheiter, C.A. Painter, J.S. Sarracino, G. Sinnis, T.N. Thompson, D. Tupa Los Alamos National Laboratory J. Belz, M. Kirn University of Montana J.A.J. Matthews, M. Roberts University of New Mexico D.R. Bergman, G. Hughes, D. Ivanov, L. Perera, S.R. Schnetzer, L. Scott, S. Stratton, G.B. Thomson, A. Zech Rutgers University N. Manago, M. Sasaki University of Tokyo R.U. Abbasi, T. Abu-Zayyad, G. Archbold, K. Belov, Z. Cao, W. Deng, W. Hanlon, P. Huentemeyer, C.C.H. Jui, E.C. Loh, K. Martens, J.N. Matthews, K. Reil, J. Smith, P. Sokolsky, R.W. Springer, B.T. Stokes, J.R. Thomas, S.B. Thomas, L. Wiencke University of Utah Z. Cao, B. Zhang, Y. Zhang, Y. Yang IHEP Bejing Kai Martens, University of Utah

  3. The Experiment: Delta HiRes on DPG: HR2: 12/1999 42 mirrors 3-31 elevation Dugway Proving Grounds HR1: 6/1997 19 mirrors 3-17elevation 12.6 km apart Kai Martens, University of Utah

  4. Highest Energy n Cosmogenic Graph by Semikoz + Sigl Kai Martens, University of Utah

  5. Tau Neutrinos ? pion decay: p m + nm m  e + ne +nm flavor counting:  2 nm + 1 ne neutrino oscillation: 2 nm 1 nm + 1 nt DELIVERABLES: 1 ne + 1 nm + 1nt •  m + nm + nt 17%  track •  e + ne + nt 18%  shower •  hh + nt 65%  shower Kai Martens, University of Utah

  6. See the Mountains? t nt shower Daniele Fargion - or who’s idea was it? calorimeter HR1 target mass HR2 Kai Martens, University of Utah

  7. MC: Topology at Work Neutrino interaction points (tau decay above ground): Cedar Mtns Stansbury Mtns Oquirrh Mtns Deep Creek Rng Sheeprock Mtns Kai Martens, University of Utah Fish Springs Rng Thomas Rng

  8. Neutrino Injection: HiRes: Impact Parameter < 75km Earth Zenith: 9010 deg MC Kai Martens, University of Utah

  9. ANIS (by Gazizov & Kowalski, AMANDA) All Neutrino Interaction Simulation we use • Incorporates: • cross sections: • CC, NC, ne-e- (resonant) • - t(m) energy loss (parameterization) • decay tables • - TAUOLA for t-decay But: made for detectors inside a spherical earth… (i.e. underground) Kai Martens, University of Utah

  10. Neutrinos: Zenith Angle q > 90° up q shower axis nt • MC input: • triggered events • both detectors • MC generated geometries Cosmic Ray MC distorted: too many high E Cosmic Rays Zenith is the discriminator!  Get geometry right !!! Kai Martens, University of Utah

  11. Event Geometry I: 3-dim  2-dim Finding the Shower Detector Plane (SDP): Kai Martens, University of Utah

  12. Finding the Good Events and keeping as many as possible!!!  efficiency  sensitivity Quality of SDP reconstruction: MC MC good quality of SDP reconstruction Kai Martens, University of Utah

  13. Event Geometry II: 2-dim  1-dim shower  scanning range for Rp direction Rp  cut edge of Rp scanning range detector in the SDP: Kai Martens, University of Utah

  14. Curvature in the Timing Fit: shower  Rp detector longitude = in plane angle use ratio of tan(q/2) and linear fit in longitude Kai Martens, University of Utah

  15. Well Reconstructed Events: ratio tan(q/2) fit to linear fit > 100  MC MC Kai Martens, University of Utah

  16. Another Difference that Matters: shower Rp detector horizontal CR events: top of atmosphere  large Rp horizontal nt out of mountain: low in atmosphere  small Rp MC MC Kai Martens, University of Utah

  17. MC Reduction: ANIS: total of 494,440,080 nt towards HiRes  4297 trigger HR1, 2496 trigger HR2 MC survivors: Energy: ANIS input: HR1 HR2 stereo 1018 – 1019: 445,425,435 265 169 10 1019 – 1020: 44,558,618 97 38 11 1020 – 1021: 4,456,027 4 2 0 Kai Martens, University of Utah

  18. Data Reduction: 152 neutrinos ??? Conclusion: all lasers! some examples: Kai Martens, University of Utah

  19. Flux Limit for Cosmogenic Neutrinos: • Efficiency of HiRes to neutrino events from MC. • Zero events found. • Estimate upper limit with Poisson Statistics. • Cosmogenic Neutrino Flux: j(E) =fE-2 Φ[ eV s-1 sr-1 cm-2] HiRes-1 HiRes-2 Stereo Kai Martens, University of Utah

  20. The HiRes Tau Neutrino Limits: Injection: E-2 spectrum 90% CL, units: eV cm-2 s-1 sr-1 (uncertainty MC statistics only) 1018 – 1019: 420 -20 +25 1019 – 1020: 1340 -110 +140 1020 – 1021: 29400 -8900 +22100 Semikoz+Sigl ni,max See also: poster 1184 in poster session 1 For cosmogenic g and n fluxes from our HR-mono fits Kai Martens, University of Utah

  21. More on HiRes Neutrino Limits: L.M. Scott: HiRes ne shown in red HE 2.3 (Thursday 12:24) Kai Martens, University of Utah

  22. HiRes & Auger Limits Kai Martens, University of Utah

  23. Interpretation of HiRes monocular CR: galactic/extragalactic transition: composition change vs.slope change changed interpretation of ankle: Doug Bergman, Rutgers Fits interpret spectrum in terms of extragalactic protons that traveled from cosmological sources p+gD(1232) p+N p m + nm m  e + ne + nm Kai Martens, University of Utah

  24. Mapping out the lasers y-component SDP normal vector: x-component Kai Martens, University of Utah

  25. Interaction Length in Standard Rock: (1200m above SL) (earth diameter) (Rock???  r=2.65 g/cm3…) lInt,t Conclusion: NO upward going neutrinos @ 1018eV Kai Martens, University of Utah

  26. GTOPO 30 + ANIS: GTOPO30: 30 arcsec  1km 33 tiles; one boundary 22km south of our detectors… Kai Martens, University of Utah

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