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

2. April 18, 2007Kai Martens, University of Utah2 The Experiment: 12.6 km apart HR2: 12/1999 42 mirrors 3  -31  elevation Dugway Proving Grounds HR1: 6/1997 19 mirrors 3  -17  elevation Delta HiRes on DPG:

3. April 18, 2007Kai Martens, University of Utah3 HiRes Optics: Mirror surface 5.1 m 2 Field of view: 16  x 14  Camera: 16 x 16 PMT each sees 1 o x 1 o in sky SUN: ½ o UV filter !!! (protecting PMTs) low resolution high speed

4. April 18, 2007Kai Martens, University of Utah4 HiRes: Stereo!!! July 11, 1999; Energy: 19 EeV Light Propagation: Atmosphere

5. April 18, 2007Kai Martens, University of Utah5 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

6. April 18, 2007Kai Martens, University of Utah6 Highest Energy  Cosmogenic Graph by Semikoz + Sigl

7. April 18, 2007Kai Martens, University of Utah7 ( Imagine ) a Mountain:   target mass calorimeter showe r Daniele Fargion - or who’s idea was it?

8. April 18, 2007Kai Martens, University of Utah8 Tau Neutrinos ? pion decay:      +     e  + e +  flavor counting:  2  + 1 e neutrino oscillation: 2   1  + 1  DELIVERABLES: 1 e + 1  + 1     +  +  17%  track   e + e +  18%  shower   hh +  65%  shower

9. April 18, 2007Kai Martens, University of Utah9 ANIS (by Gazizov & Kowalski, AMANDA) But: made for detectors inside a spherical earth… (i.e. underground) All Neutrino Interaction Simulation Incorporates: - cross sections: CC, NC, e  e - (resonant) -  (  ) energy loss (parameterization) - decay tables - TAUOLA for  -decay we use

10. April 18, 2007Kai Martens, University of Utah10 GTOPO 30 + ANIS: GTOPO30: 30 arcsec  1km 33 tiles; one boundary 22km south of our detectors…

11. April 18, 2007Kai Martens, University of Utah11 MC: Topology at Work Neutrino interaction points (tau decay above ground): Cedar Mtns Deep Creek Rng Stansbury MtnsOquirrh Mtns Fish Springs Rng Thomas Rng Sheeprock Mtns

12. April 18, 2007Kai Martens, University of Utah12 Neutrino Injection: Earth HiRes: Impact Parameter < 75km Zenith: 90  10 deg

13. April 18, 2007Kai Martens, University of Utah13 Neutrinos: Zenith Angle  > 90° Cosmic Rays  MC input: - triggered events - both detectors - MC generated geometries Zenith is the discriminator!  Get geometry right !!! up shower axis  Cosmic Ray MC distorted: too many high E

14. April 18, 2007Kai Martens, University of Utah14 Finding the good guys and keeping as many as possible!!!  efficiency  sensitivity Review reconstruction: First step: SDP SDP normal uncertainty:

15. April 18, 2007Kai Martens, University of Utah15 Event Geometry II: 2-dim  1-dim in the SDP: RpRp  detector shower  scanning range for R p direction  cut edge of R p scanning range

16. April 18, 2007Kai Martens, University of Utah16 Curvature in the Timing Fit: RpRp  detector shower  longitude = in plane angle use ratio of tan(  /2) and linear fit in longitude

17. April 18, 2007Kai Martens, University of Utah17 Well Reconstructed Events: ratio tan(  /2) fit to linear fit > 100 

18. April 18, 2007Kai Martens, University of Utah18 Another Difference that Matters: RpRp detector shower horizontal CR events: top of atmosphere  large R p horizontal  out of mountain: low in atmosphere  small R p

19. April 18, 2007Kai Martens, University of Utah19 Mapping out the lasers SDP normal vector: x-component y-component

20. April 18, 2007Kai Martens, University of Utah20 MC Reduction: ANIS: total of 494,440,080  towards HiRes  4297 trigger HR1, 2496 trigger HR2 MC survivors: Energy:ANIS input:HR1HR2stereo 10 18 – 10 19 :445,425,43526516910 10 19 – 10 20 : 44,558,618 97 3811 10 20 – 10 21 : 4,456,027 4 2 0

21. April 18, 2007Kai Martens, University of Utah21 Data Reduction: 152 neutrinos ??? some examples: conclusion: all lasers!

22. April 18, 2007Kai Martens, University of Utah22 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) =  E -2 Φ  [ eV s -1 sr -1 cm -2 ] HiRes-1HiRes-2Stereo

23. April 18, 2007Kai Martens, University of Utah23 The HiRes Tau Neutrino Limits: Semikoz+Sigl i,max 90% CL, units: eVcm -2 s -1 sr -1 (uncertainty MC statistics only) 10 18 – 10 19 : 420 -20 +25 10 19 – 10 20 : 1340 -110 +140 10 20 – 10 21 : 29400 -8900 +22100 Injection: E -2 spectrum

24. April 18, 2007Kai Martens, University of Utah24 (1200m above SL) Interaction Length in Standard Rock: (Rock???   =2.65 g/cm 3 …) Conclusion: NO upward going neutrinos @ 10 18 eV (earth diameter) Int, 

25. April 18, 2007Kai Martens, University of Utah25 Interpretation of HiRes monocular CR: Doug Bergman, Rutgers Fits interpret spectrum in terms of extragalactic protons that traveled from cosmological sources changed interpretation of ankle: galactic/extragalactic transition: composition change vs. slope change p+    (1232)   +N      +     e  + e + 

26. April 18, 2007Kai Martens, University of Utah26 Some Input: garbage in, garbage out… (this is MC!)