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Innovative Approaches for High-Energy Astroparticle Experiments

This discussion centers on novel ideas for advancing high-energy astroparticle experiments, as presented at the TAE 2010 in Barcelona. Key topics include potential methods for detecting high-energy neutrinos using techniques like radio, optical, acoustic, and atmospheric showers, alongside established experiments like AMANDA, IceCube, and KM3NeT. The session explores the viability of various detection strategies, including inclined showers and Earth-skimming neutrinos, while highlighting the role of multi-messenger astronomy and emerging technologies in enhancing detection sensitivity.

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Innovative Approaches for High-Energy Astroparticle Experiments

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  1. Discussion session: other (crazy ?) ideas for High-Energy Astroparticle Experiments TAE 2010 1-10 Sept.2010 Barcelona Manel Martinez

  2. How to go beyond:- KM3Net for HE Neutrinos ?- AUGER North for UHE CRs ?- CTA for gamma rays ?

  3. Other possible HE neutrino detection techniques ?...

  4. Detection of extra-terrestrial neutrinos Radio Optical Cherenkov Acoustic Atmospheric showers Earth based In space In space Earth based In Ice In water Baikal ANTARES NEMO NESTOR ANITA FORTE AMANDA B-10 AMANDA II IceCube RICE GLUE SalSA CODALEMA ARIANNA SAUND SADCO (Greece) ANTARES R&D IceCube AUTEC AGAM Auger EUSO OWL KM3NeT

  5. UHE neutrinos: Detection alternatives • Inclined Showers: Deep showers • Downgoing neutrinos interacting in the atmosphere • All flavors • Earth-skimming neutrinos • nt interacts at Earth crust • t exits to atmosphere • t decay generates an upcoming air shower • Coherent Radio pulses • Ice: RICE, ANITA • Salt: Salsa • Moon: Glue, Lunaska • Coherent sound (1500 km3, 100 hydroph/km3)

  6. Radio detection ?...

  7. Cherenkov in radio (Askary’an 1960) g e- Compton e+ e+ e- e- e- e- Bhabha Möller But Ne-> Ne+ Coherencee- and e+ cancel !! e+ e- Annihilation media electrons

  8. ICE ZHS:FH,TS,EZ, PRD(91) Askary’an predicted ~10% charge excess

  9. SLAC experiment: sand & salt Bunches of ~ GeV bremss g in sand & salt: Total energy (sand) ~ 6 x 1017 – 1019 eV . Askaryan effect confirmed!!! E-field ~ Ebunch MC vs Data Polarized SAND D. Saltzberg et al. PRL 86 (2001) P.W. Gorham et al. astro-ph/0412128 Pulse correlated to charge excess

  10. The radio technique Efield~25% Ne ~ Eshowerpower ~ Eshower2 MOON REGOLITH

  11. NuMoon Kalyazin ANITA R.J. Protheroe, R. Ekers et al. GLUE Many experiments around the world 1017 eV < Ethreshold< 1020 eV ICE RICE AURA ARIANNA MOON, ... FORTE

  12. Acoustic detection ?...

  13. AMADEUS (Antares Modules for Acoustic DEtection Under the Sea)

  14. SPATS an Acoustic Array at the South Pole

  15. IceCube Future Plans • Deep Core • Greatly enhances IceCube sensitivity to lower energy ’s • Lower mass solar WIMPs • Atmospheric neutrinos • Six new strings • 60 high QE DOMs in clear ice • First string deployed 08/09, • Remaining strings deployed 09/10 • Multi-messenger astronomy • Correlations with ROTSE, AGILE, MAGIC, and LIGO • New Technologies • 3 Prototype digital radio strings deployed with IceCube strings • 4 Hydrophones deployed above IceCube Dust concentration Very clear ice D. Cowen, Neutrino 2008

  16. Other possible UHE CR detection techniques ?...

  17. Other possible VHE gamma ray detection techniques ?...

  18. HAWC: The High Altitude Water Cherenkov Experiment 300 water Cherenkov tanks @ Sierra Negra observatory (Mexico, 4100 m asl) near pico Orizaba

  19. A 5 meter diameter tank as simulated in Geant4 for a single vertical muon. The number of photons are reduced by a factor of 50 for vizualization.

  20. Discussion: Pros and cons of a VHE gamma ray particle detector at the moon… does it make sense ?

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