TREND workshop agenda 0. Introduction and round-table

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Presentation transcript:

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’

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

Flux divided by 1000 when energy increased by factor 10 32 orders of magnitude 1 1020 electron -volt Joules 1.6 10-19 16 103 106 1012 1015 1.6 10-16 1.6 10-10 1.6 10-7 1.6 10-4 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=0.999999999999999999999 x c) F a E-3 Flux divided by 1000 when energy increased by factor 10 13 orders of magnitude

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!

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

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

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)

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

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

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 http://arxiv.org/abs/1111.2507v1 ICRC2011 http://arxiv.org/abs/1207.4823v1 Results not fully consistent on mass composition & anitropy. Also energy mismatch > 20%.

Next on UHECRs Improve EAS physics modelisation (fed by TOTEM@CERN) Larger detectors larger statistics ICRC2011 http://arxiv.org/abs/1207.4823v1 High quality & redundant measurements (multi-hybrid) to control systematic biases.

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

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