1. July 10, 2007 Detection of Askaryan radio pulses produced by cores of air showers. Suruj Seunarine, Amir Javaid, David Seckel, Philip Wahrlich, John Clem D. Seckel, Univ. of Delaware

2. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Topics Concept: –A source to test radio techniques –CR composition ? Askaryan pulses & air shower dimensions Air shower properties (AIRES & CORSIKA) –Particle content –Radial and energy distributions Calculation of RF signal –Coherent addition of subshowers –Issues: near zone/far zone, ray tracing Composition studies Detection –IceCube: shallow array, AURA –ANITA

3. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Theorist’s view of the UHE neutrino sky

4. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Recall how radio works 5 m 10 cm JC, SY: “How do you know when you haven’t seen anything?”

5. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Radio Goals & Staging 100 events/yr above 10 18 eV >1000 km 3 sr Validation of design for field work Prototype projects – more than upper limits Detect Air Showers: Signal/Background/Calib

6. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Askaryan pulses from air shower core

7. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Critical dimensions

8. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) High energy ground level particles at SP CORSIKA/AIRES –Primary energy: 1,10,100,1000 PeV –Cutoff: 1,10,100,1000 GeV –Compositionp & Fe Explore –Particle content rad - meson - baryon - mu –Radial profilesE sh vs r –Shower development dN/dE, ancestry

9. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Ground level particles  e-e-   n,p

10. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Radial distributions by particle ID radiating mesons baryons muons

11. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) E vs r (AIRES)

12. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) E vs r (CORSIKA) Fraction of available energy approaches 10% by 100 PeV Scaling allows use of high cutoff

13. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Synthesis of Askaryan pulses Many ground level particles –Superposition Individual RF pulses –Event: (id, t e, x e, n, E) –SubShower:(t s, x s, n, (r,l,s)) –Resolve geometry to antenna –Launch EM pulse(scaled AVZ) –Propagation effects (1/r, attenuation) –Adjust phase to common time basis Response –CoAdd spectra(t, n, pol, (complex spectrum)) –Antenna/DAQ

14. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Subshowers & Coherence of RF pulses

15. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Time Domain Waveforms

16. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) RF: (E p = 1 EeV, E cut = 1 TeV )

17. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) EeV/TeV again

18. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) RF Cerenkov Rings

19. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) RF vs Core Size

20. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Determining Cosmic Ray Composition AIRES showers (from S. Seunarine) E sh (r<20 cm) as proxy for radio High-lite: 10 PeV, True iron

21. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Comparison of Fe/p

22. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Scaling & Rates Rate independent of D Threshold increases with D True for E -3 –But not for E -2 Rate for 30m*30m @ 3PeV = 1/hour

23. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Shallow Array Concepts Drill 16 x 30m holes –1 dom per hole –4 antennas per dom 2 x 50m cables to each of four nearby strings & SJB 2 doms per cable

24. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) AURA geometry

25. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) ANITA (A. Javaid) Rate –A  1.5 10 6 km 2 sr – 1400/day E>10 19 – ? /dayE>10 20 High, Thin, Ice

26. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Summary Test beam for radio sure would be nice Air Shower Cores: E eff ~ 10% E p (at EeV) Synthetic RF looks usable CR Composition Measurement –Core energy anti-correlated with deep-  –p-Fe separation Three scenarios –Small subsurface array w/IceTop –AURA –ANITA

27. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) END

28. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Radial distributions by energy

29. Askaryan pulses from air shower cores, Merida, 30 th ICRC, July 10 2007 (Seckel) Sample the Cerenkov Ring