1. D.Fargion@roma1.infn.itAstronomia con i neutrini1 Showering Neutrino Astronomies at Horizons

2. D.Fargion@roma1.infn.itAstronomia con i neutrini2 Update article

3. D.Fargion@roma1.infn.itAstronomia con i neutrini3 Why Neutrino may see where and what gamma and UHECR are no allowed to accelerated protons interact: => the energy fluences in  -rays and neutrinos are comparable due to isospin symmetry. For neutrinos the observable spectrum is practically identical to the production spectrum, whereas  -rays pile up below the pair production threshold on the CMB at a few 10 14 eV. The Universe acts as a calorimeter for the total injected electromagnetic energy above the pair threshold. This constrains gamma but only part of the neutrino fluxes.

4. D.Fargion@roma1.infn.itAstronomia con i neutrini4 High Energy Neutrino Astronomy are a Must just behind the corner Solar,Supernovae Neutrino Astronomy are probed. Cosmic rays flux as rich as BBR, being charged, are bent and smeared, blinding most CR astronomy. UHECR are direct, but BBR cut them, GZK cut, locally. UHECR themselves must produce GZK- EeV neutrinos. AGN, GRBs, Star Burst Galaxy must also produce PeV neutrinos. UHE neutrinos must emerge above atmospheric neutrino noises: muons tracks and tau showers by their decay in flight (double bang) are their best trace.

5. D.Fargion@roma1.infn.itAstronomia con i neutrini5 Many New Astronomies : Gravitons, Susy UHE Neutralino, low and UHE Neutrinos

6. D.Fargion@roma1.infn.itAstronomia con i neutrini6 Local number flux of particles

7. D.Fargion@roma1.infn.itAstronomia con i neutrini7 Why Horizontal – Upward Tau air- showers are easier to be revealed than muon tracks ? Because an air- shower is amplified By its huge secondary number. Millions muons, billions gamma and e-pairs, trillions or more Cerenkov photons. Muon is single, alone and shine little.

8. D.Fargion@roma1.infn.itAstronomia con i neutrini8 Why Horizontal – Upward Tau Showering is so much linked to neutrino mass and mixing ? Because mixing, even for minimal masses guarantee the flavour transformation from Muon Neutrinos to the Tau Neutrinos. Galactic and cosmic distances are huge respect oscillation lenghts. 8.3 pc

9. D.Fargion@roma1.infn.itAstronomia con i neutrini9  26th ICRC,He 6.1.09, p.396-398.1999.

10. D.Fargion@roma1.infn.itAstronomia con i neutrini10 Tau Air-Showers:In principle Astronomy versus Elementary Particle Tau Channels Modes

11. D.Fargion@roma1.infn.itAstronomia con i neutrini11 Tuning to Air Showers by atmosphere filter at different angles and altitudes Earth Horizons edge 20 km.

12. D.Fargion@roma1.infn.itAstronomia con i neutrini12 Horizontal Air Showers : A new Cosmic Ray Frontier A New mountain of views The Iceberg peak of a New Cosmic Ray Spectroscopy Neutrino and UHECR Air-showers telescopes versus Muon lepton tracks. Atmospheric Versus astrophysical signals: The vertical downward pollution versus the upward Earth opacity  

13. D.Fargion@roma1.infn.itAstronomia con i neutrini13 Earth Opacity by Inner Earth Density Structures

14. D.Fargion@roma1.infn.itAstronomia con i neutrini14 The Earth act as a beam dump and the atmosphere as a calorimeter to amplify the Tau Air-Shower Charged current: Neutral current: Glashow Resonance(E = 6.3 × 10 15 eV): Glashow Resonance(E = 6.3 × 10 15 eV): Cascade

15. D.Fargion@roma1.infn.itAstronomia con i neutrini15 Muon interaction lenght Muon interaction lenght

16. D.Fargion@roma1.infn.itAstronomia con i neutrini16 Unstable tau versus muons at highest energy

17. D.Fargion@roma1.infn.itAstronomia con i neutrini17 Expected Tau events at different angles. GZK input neutrino flux Rock Water Rock

18. D.Fargion@roma1.infn.itAstronomia con i neutrini18 Expected μ ± events by Tau Air Showers (Hortaus) GZK input neutrino flux. Rock Water Rock

19. D.Fargion@roma1.infn.itAstronomia con i neutrini19 Expected GZK neutrino flux

20. D.Fargion@roma1.infn.itAstronomia con i neutrini20 Detectors extended in deep valley : ARGO-Tibet    

21. D.Fargion@roma1.infn.itAstronomia con i neutrini21 The Ande Mountains as a target for detecting UHE neutrino tau by Horizontal Air-Showers at AUGER: ANDE SHADOWs on GZK Cosmic Rays from West and Young Horizontal Tau Air-Showers at EeVs D.Fargion The Astrophysical Journal,570,p.909. 2002  

22. D.Fargion@roma1.infn.itAstronomia con i neutrini22 The Ande Shadows on AUGER Pastor et. All 2005

23. D.Fargion@roma1.infn.itAstronomia con i neutrini23 Milagro: Vertical TeV gamma versus Muon bundle by tau air-showers on horizons    

24. D.Fargion@roma1.infn.itAstronomia con i neutrini24 The EUSO telescope seeing Hortaus in wide FOV: tens of events in three years

25. D.Fargion@roma1.infn.itAstronomia con i neutrini25 Showering Up - Down on MAGIC Horizons : Cosmic Rays at PeVs –EeVs energy versus Glashow Resonant 6.3 Pevs and Tau EeVs Air-Showers Muon’ s Rings and Arcs, Gamma Lateral Traces: Fan –like Horizontal Shower   

26. D.Fargion@roma1.infn.itAstronomia con i neutrini26 Horizons distance d= 167 km √(h/2.2 km) Cerenkov Shower opening angle  ~ 1 ° Conic Air Base Area A ~ 30 km 2 Truncate Air Cone height h ~ 100 km Truncate Air Cone Volume V ~ 1000 km 3 Truncate Cone Mass M ~ 1 km 3 MAGIC, while pointing a GRB or a SGR Burst at Horizons ( ~ 3% of the GRB-SGRs events ) behave as a km 3 NEUTRINO TELESCOPE astro-ph/0505459 Neutrino Astronomy beyond and beneath the Horizons : D. FargionD. Fargion

27. D.Fargion@roma1.infn.itAstronomia con i neutrini27 MAGIC, while pointing a GRB, SGR or BL Lac Below The Horizons ( ~ 1% of the GRB-SGRs events ) on rock behave (near EeV n t energy) as a 75 km 3 NEUTRINO TELESCOPE L t = 10 km w.e. l t = 0.5 km w.e. Horizons distance d= 167 km √(h/2.2 km) Cerenkov Shower opening angle ~ 0.3° Inclined Rock Cilinder depth L t ~ 10 km Inclined Conic Rock Base Area A ~ 3*50 =150 km 2 Rock Cilinder depth l t ~ 0.5 km w.e. astro-ph/0511597 D. Fargion Progh.Part.Nucl.Phys.57 (2006) 384-393.  

28. D.Fargion@roma1.infn.itAstronomia con i neutrini28 UHECR Mirror air-showers and their polarization Reflection on the Sea of UHECR air-Showers Cherenkov lightsReflection on the Sea of UHECR air-Showers Cherenkov lights

29. D.Fargion@roma1.infn.itAstronomia con i neutrini29 Arrays in Space Station to track Gamma and Cherenkov Horizontal Air-Showers

30. D.Fargion@roma1.infn.itAstronomia con i neutrini30 Air Showers on the Crown array telescope  

31. D.Fargion@roma1.infn.itAstronomia con i neutrini31 In Conclusion, while muon tracks may hide in deep underground up-ward Muon-Neutrino Astronomy, the Tau air-Shower Neutrino Sky lay just under our own Sky: it is the Earth      

32. D.Fargion@roma1.infn.itAstronomia con i neutrini32 Conclusioni 1.Tau Neutrino Earth Skimming Astronomy is at the edges 2.Milagro,Shalon, ASHRA,CRTNT, MAGIC and Veritas may discover its air-showers 3.AUGER and ARGO may find it in inclined events 4.Tau Airshowers may arise from the space as Terrestrial Gamma Flashes 5.Time will show that the Tau sky lay just behind our own foot 6.OUR EARTH