1. TREND workshop agenda 0. Introduction and round-table
Radio detection of Extensive Air Shower & TREND present status
High energy cosmic ray physics: motivation & experimental status 20’
Radio-detection of extensive air showers 20’
The Tianshan Radio Experiment for Neutrino Detection 1h
Neutrino Astronomy & GRAND project
Motivations for neutrino astronomy 30’
Cosmic neutrino detection 30’
TREND Giant Radio Array for Neutrino Detection 30’

2. I.1. High energy cosmic ray physics: motivation & experimental status
Olivier Martineau-Huynh
TREND workshop,
April 19, 2013

3. Flux divided by 1000 when energy increased by factor 10
32 orders
of magnitude 1
1020
electron
-volt
Joules 16
103
106
1012
1015
Energy
Visible light
X rays
Energy at LHC  kinetic energy of a mosquito in flight
Kinetic energy of a tennis ball at 200km/h
(or a proton at v= x c)
F a E-3
Flux divided by 1000 when energy increased by factor 10
13 orders of magnitude

4. Issues at the highest energies
What are the Ultra High Energy CRs made of?
Nuclei? Light? Heavy?
g rays? neutrinos?
What are their sources?
Extragalactic objects?
Relic particles?
Manifestation of
New Physics?
1020eV ~ 20J  tennis ball at 200km/h… No sources known for these energies!

5. « Direct » CR
measurements
« Indirect » CR
measurements
Extensive
Air
Shower
surface arrays
Satellites & baloons

6. UHECRs : an experimental challenge
Extensive
Air
Shower
Detection of EAS: particle or fluorescence detectors (among others)
Challenges:
low flux
Shower development badly known (hadronic interactions at extreme energies)
Detection systematics

7. UHECRs puzzle: a complex experimental situation
HiRes
AGASA
Early 2000’s: diverging results on spectrum for HiRes (fluorescence) and AGASA (scintillators)…
Go for hybrid detectors
(Surface Detectors + Fluorescence Detectors)

8. The Pierre AUGER Observatory the key to the mystery of UHECRs?
A giant (3000km²) UHECRs detector built in Argentina between 2001 and 2003 (completed in 2008)
~60km

9. The Pierre AUGER Observatory
A hybrid detector: surface + fluorescence
Running since 2004

10. Hybrid detectors results
4+ years of data taking
UHECRs are mostly nuclei, coming for close-by astrophysical sources (z<0.02  few 100MPsecs)
AUGER
proton
(simu)
iron
Telescope
Array
ICRC2011
ICRC2011
Results not fully consistent on mass composition & anitropy. Also energy mismatch > 20%.

11. Next on UHECRs Improve EAS physics modelisation (fed by TOTEM@CERN)
Larger detectors
larger statistics
ICRC2011
High quality & redundant measurements (multi-hybrid) to control systematic biases.

12. Large High Altitude Air Shower Observatory
LHAASO Project: γastronomy and origin of CR
Wide FOV
C-Telescope
Array
&
Core Detector
μdetector
Array
Water C
Array
Charge
Particle
Array
Large High Altitude Air Shower Observatory

13. Radio-detection Cheap, reliable, easy to deploy, 100% duty cycle…
The perfect tool for UHECR physics?