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A HiRes Limit On Cosmogenic Neutrino Flux

Explore cosmogenic neutrino flux origins from extragalactic protons, focusing on tau neutrino detection through tau decay channel simulations and event reconstructions. HiRes Collaboration at the University of Utah implements ANIS simulation, local topography considerations, and event reconstruction techniques to study cosmic rays vs. neutrinos. Learn about flux limits for cosmogenic neutrinos and efficiency evaluation for HiRes.

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A HiRes Limit On Cosmogenic Neutrino Flux

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  1. A HiRes Limit On Cosmogenic Neutrino Flux Weiran Deng High Energy Astrophysics Institute University of Utah APS-DPF 2006+JPS2006, Hawaii

  2. AGASA HR2 HR1 Auger UHE Cosmic Ray Spectrum and GZK 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 Neutrino Oscillation: 1 ne + 1 nm + 1nt Weiran Deng, University of Utah

  3. Cosmogenic Neutrino Flux From APS Multidivisional Neutrino Study (Neutrino Astrophysics and Cosmology Working Group) Weiran Deng, University of Utah

  4. HiRes 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 Weiran Deng, University of Utah

  5. Delta High Resolution Fly’s Eye Experiment HiRes on DPG: HR1: 6/1997 22 mirrors 3-17elevation HR2: 12/1999 42 mirrors 3-31 elevation Weiran Deng, University of Utah

  6. SUN: ½o Mirror Optics Camera: 16 x 16 PMT each sees 1o x 1o in sky Mirror surface 5.1 m2 Field of view: 16 x 14 Weiran Deng, University of Utah

  7. To detect a tau neutrino … t decay channel: t- → e- + ne + nt 18% t- → m- + nm + nt 17% t- → h- (p-,K-) + nt 65% Weiran Deng, University of Utah

  8. Simulate Tau Neutrino Propagation • All Neutrino Interaction Simulation (ANIS) by Gazizov & Kowalski, AMANDA • Extension and modification: Topography, atmospheric density profile, propagation routine • Incorporates: • cross sections: • CC, NC, ne-e- (resonant) • - t(m) energy loss (parameterization) • decay tables • - TAUOLA for t-decay Weiran Deng, University of Utah

  9. Local Topography Zenith 85o 95o Weiran Deng, University of Utah

  10. Event Reconstruction - Geometry Construct: Shower Detector Plane (SDP) Weiran Deng, University of Utah

  11. Find Good Events - SDP Reconstruction Error • Before Plane Reconstruction: • Remove calibration laser, flasher and aircraft events • Remove events triggered by noise – Random Walk Filter • Keep events with between 7 and 500 tubes. 0.23 Degree SDP reconstruction uncertainty [rad] Weiran Deng, University of Utah

  12. Outlier Removal q3 q2 q1 scanning range for Rp direction Rp detector: light arrival times ti Time Fitting Within SDP • Determine Fitting Quality: • Curvature of the track • Angular scanning range to find Rp Weiran Deng, University of Utah

  13. shower Rp detector Cosmic Rays vs. Neutrinos • Cosmic ray events from neutrino events: • Zenith Angle > 85.9 degree • Rp Distance [1km, 20km] Zenith Rp distance [km] Weiran Deng, University of Utah

  14. Final Events From Reconstruction All clear? Hr1: 77 - Hr2: 59 Events with same geometry Suspicious? Weiran Deng, University of Utah

  15. 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 Flux Limits for Cosmogenic Neutrinos 1018 eV -> 1019 eV: 167±5 1019 eV -> 1020 eV: 320±14 1020 eV -> 1021 eV: 5162±940 (errors statistical only) Weiran Deng, University of Utah

  16. Summary Weiran Deng, University of Utah

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