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Telescope Array for Extremely High Energy Cosmic Rays. July 30th, 2003 Masaki FUKUSHIMA

Telescope Array for Extremely High Energy Cosmic Rays. July 30th, 2003 Masaki FUKUSHIMA ICRR, Univ. of Tokyo. Extra‐Galactic. Galactic. Magnetic Confinement. 1. ０. HiRes: Composition Change from Heavy to Light. Ankle Structure. 3. ２. ＡＧＡＳＡ： Ａｎｉｓｏｔｒｏｐｙ towards Galactic Center.

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Telescope Array for Extremely High Energy Cosmic Rays. July 30th, 2003 Masaki FUKUSHIMA

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  1. Telescope Array for Extremely High Energy Cosmic Rays. July 30th, 2003 Masaki FUKUSHIMA ICRR, Univ. of Tokyo

  2. Extra‐Galactic Galactic Magnetic Confinement 1 ０ HiRes: Composition Change from Heavy to Light Ankle Structure 3 ２ ＡＧＡＳＡ： Ａｎｉｓｏｔｒｏｐｙ towards Galactic Center

  3. Galactic to extra-galactic transition We are starting to collect First samples of extra-galactic Matter-Particles

  4. AGASA Log ( FLUX x E3) Log（ENERGY［eV］） Energy Spectrum of the Highest Energy Cosmic Rays There is a Horizon for Cosmic Rays with Energy exceeding 10 20 eV by GZK mechanism Cosmic Rays with Energy above GZK cutoff exists. No obvious astronomical counterpart within ~ 50 Mpc.

  5. E > 10 19 eV > 10 20.0 eV > 10 19.6 eV > 10 19.0 eV Arrival Directions and Clustering “Point” Sources AGASA E > 10 19.6 eV Isotropic Distribution

  6. super-GZK + cluster Hard to explain by standard Astrophysics ・ Particle Physics ・ Cosmology

  7. Possibilities of creating continued spectrum exceeding GZK-cutoff Acceleration problem unresolved for 2-4.

  8. Establish ・　Galactic to Extra-galactic transition Confirm / Refute ・　super-GZK ・　cluster

  9. “AGASA” x 10 Plastic Scintillator Array + 3-station “HiRes” Fluorescence Telescope + Low energy extension

  10. 20 km 20 km TA Detector Configuration Millard County Utah/USA 24 x 24 Scintillators (1.2 km spacing) AGASA x 9 3 x Fluorescence Stations AGASA x 10 Low Energy Hybrid Extension

  11. SD - FD；　Two Independent Methodsfor Energy Determination. • ○E>1019 eV ~ 100 ev. / Year • ○　E>1020 eV ~ 1 ev. / Year • Phase-1 Hybrid TA gives ENERGY SCALE by • ●SCINTILLATOR ARRAY • ●AIR FLUORESCENCE • Energy Spectrum by Only-one, Unique Energy Scale • （Systematic Energy Uncertainty　＜　１０％　Aimed） e /γ meas. Calibration Comparison Energy Calibration by SD-FD Coincidence Meas..

  12. TA Scintillator Development proto: 50 cm x 50 cm, 1cm thick Wave Length Shifter Fiber readout 50 modules used in L3 for 2.5 years. cutting 1.5 mm deep groove WLS: BCF-91A （ 1 mm Φ） Final: 3 m2 by 2 PMT readout.

  13. “μ” Density at 1km for p/Fe Energy Loss in the Air ~10% of Total Energy MODEL p / Fe Uncertainty EAIR / E0 ｐ Ｆｅ ~90% of Total Energy AUGER water tank simulation Plastic Scintillator:Water Tank: e＋e－ μ＋μ－ & soft γ • Electron Measurementby Scintillator • ●Reasonable resolution • ●Small model / composition dependence

  14. Shower Image Telescope：　３ｍΦSpherical Mirror TA Telescope Development Electronics： ２００ ns continuous ADC ＋ Signal recognition by software Imaging Camera：１６Ｘ１６ PMT Array 1 0 x 1 0 FoV/PMT

  15. 3 Fold Stereo Measurement ① ３ independent energy meas. for 60% of events at 1020 eV Estimate of Systematics 　　　　・　Atmosph. Clarity 　　　　・　Cherenkov Light ② ③

  16. 20 MeV 40 MeV 100 m away 100 m away Shoot electron Linac beam into the sky. 20 MeV / particle x 109 ppp =2 x 1016 eVtotal energy deposit. Absolute End-to-End energy calibration. Feasibility study

  17. Participants * : Ａｄｖｉｓｅｒｓ** : Kakenhi Reviewers

  18. AGASA HiRes AUGER AUGER Construction Plan of Hybrid TA: 2003 SITE PREPARATION TELESCOPE TEST IN UTAH TELESCOPE PRODUCTION TELESCOPE INSTAL. ARRAY TEST IN UTAH ARRAY PRODUCTION ARRAY PRODUCTION CALIB. with AGASA SD only Start Obs. with SD only Start Hybrid Obs. SD + FD construction observation

  19. Telescope Array ; Summary • Well-defined purposes; • ①Establish galactic to extra-galactic transition. • ② Confirm/Refute cluster + super-GZK. • Seamless coverage from 1016 to 1020.5 eV. • Fluorescence + Surface hybrid. • Common technology and existing resources • based on AGASA + HiRes. • Start measurement in 2006(SD) / 2007(+FD).

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