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Neutrinos @ HiRes

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  1. Neutrinos @ HiRes HR2 HR1 Kai Martens High Energy Astrophysics Institute Department of Physics, University of Utah

  2. 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

  3. HiRes Optics: SUN: ½o low resolution high speed Camera: 16 x 16 PMT each sees 1o x 1o in sky Mirror surface 5.1 m2 Field of view: 16 x 14 UV filter !!! (protecting PMTs) Kai Martens, University of Utah

  4. HiRes: Stereo!!! July 11, 1999; Energy: 19 EeV Light Propagation: Atmosphere Kai Martens, University of Utah

  5. 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

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

  7. ( Imagine ) a Mountain: t nt shower calorimeter target mass Daniele Fargion - or who’s idea was it? Kai Martens, University of Utah

  8. 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

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

  11. 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

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

  13. 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

  14. Finding the good guys and keeping as many as possible!!!  efficiency  sensitivity Review reconstruction: First step: SDP SDP normal uncertainty: Kai Martens, University of Utah

  15. 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

  16. 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

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

  18. 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 Kai Martens, University of Utah

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

  20. 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

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

  22. 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

  23. The HiRes Tau Neutrino Limits: Injection: E-2 spectrum 90% CL, units: eVcm-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 Kai Martens, University of Utah

  24. 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

  25. 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

  26. Some Input: garbage in, garbage out… (this is MC!) Kai Martens, University of Utah