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EHE Cosmic Rays (HE1.4, 1.5, 2.1) Shigeru Yoshida Department of Physics Chiba University 29th ICRC Pune 29th ICRC Pune No GZK ? When I was a rapporteur 6 years ago (ICRC Salt Lake) 7 events above 1020 eV 29th ICRC Pune Anisotropy : UHECR Sky? 29th ICRC Pune New measurements HiRes Two FD Eyes allows STEREO observation • HiRes1 Most statistics above 10 EeV Only 1 ring • HiRes2 Lower Threshold Energy (~0.2 EeV) 2 rings 29th ICRC Pune New measurements Auger SD (Ground Array) + 3(+1) FD Eyes • SD 50% Completed ~1500 km2 • FD 3 Eyes completed mostly for Energy Calibration 29th ICRC Pune Present Exposure @ 1019 eV HiRes1 (mono) HiRes (Stereo) Auger ~5000 km2 sr yr ~2500 km2 sr yr 1750 km2 sr yr ~ AGASA 29th ICRC Pune HiRes Aperture HiRes-2 mono Stereo data: best resolution, optimized for E>31018eV Uses timedependent calibration of detector and atmosphere HiRes-2 monocular: can reach down to as low as 1017.2eV HiRes-1 monocular data began ~3 years earlier: largest statistics, Uses profile constrained fit (PFC) unreliable <1018.5eV Wayne Springer (this conference) HiRes stereo HiRes-1 mono HiRes Apertures 29th ICRC Pune HiRes 1 (mono) “GZK” Statistics • Expect 42.8 events • Observe 15 events • ~5 s Bergman (this conference) 29th ICRC Pune HiRes 1 (mono) Integral Spectrum Flux attenuation starts At around 1019.75 eV Consistent with the GZK hypothesis Bergman (this conference) 29th ICRC Pune You need some caution HiRes1 is strongly BIASED measurement. It’s MONOCULAR and only 1 ring! Viewing limited volume of the atmospheric volume. Aperture continues increasing with energy Profile constrained fit to estimate energy Stereo measur. should provide a confident data 29th ICRC Pune HiRes Stereo Flux Fit to power law. Single index gives poor chi2 Evidence for changing index Wayne Springer (this conference) 29th ICRC Pune HiRes Stereo (and others) Exhibits cutoff structure Expect 33.7 events Observe 9 events ~4.8s Some details DIFFERENT from mono! The Mono spectrum may contain unknown syst. 29th ICRC Pune Some Remarks HiRes Stereo Cut “sort of” narrow Opening angle events Require careful estimation of detect. Eff. Scanning simple parameters continues AGASA conflicts Energy scale? Old MC? Auger Hybrid measurement 29th ICRC Pune Auger Hybrid Paul Sommers (this conference) Log (E) = -0.79 + 1.06 Log(S38) E = 0.16 S381.06 (E in EeV, S38 in VEM) Uncertainty in this rule increases from 15% at 3 EeV to 40% at 100 EeV 29th ICRC Pune Auger SD spectrum Energy scale uncer. still large ~40 % in 100 EeV improvement will come soon Paul Sommers (this conference) 29th ICRC Pune S(1000): The energy indicator (Ghia, this conference) 29th ICRC Pune S(1000): The energy indicator Less mass composition sensitive Not just muons but emg component make sizable contributions (Alan Watson, private comminication) S(1000)Fe-P ~10 % difference (Paul Sommers, private com) s s(1000) ~15% @ 10 VEM (Ghia, this conference) BUT ALL these rely on EAS MC!! S.Yoshida 29th ICRC Pune A scary scenario When more statistics Intrinsic fluctuation Of EAS development!! (Sako, this conference) LHCf interaction point 96mm 140m The beam pipes of LHC are separated by 96mm at 140m from the interaction point. Charged particles are swept out by magnets. LHCf measures the distribution of the Feynman x parameter (practically energy) of neutral particles emitted in the very forward region using position sensitive calorimeters placed in this 96mm gap. LHCf Prototype test Main detector Silicon tracker for position calibration 29th ICRC Pune Event cluster > 40 EeV No significant excess: AGASA’s triplet Pch ~0.28 (Westerhoff, this conference) 29th ICRC Pune AGASA triplet story HiRes stereo event 6060 60° 180 ° 180 ° 170 ° 170 ° One event added – BUT below 40 EeV!! (Westerhoff, this conference) 29th ICRC Pune HiRes: BL Lac correlation? “BL” BL Lacs with m<18, all HiRes events (no energy cut): F = 2×10-4 All confirmed BL Lacs (“BL+HP”) with m<18, HiRes E>10 EeV: F = 10-5 Confirmed TeV blazars, all HiRes events (no energy cut): F = 10-3 These are not independent results: the samples overlap. Analysis has been a posteriori, so F values are not true chance probabilities. (Finley, this conference) 29th ICRC Pune HiRes2 Mono: Galactic anti-center? (Thomson, this conference) (Letessier-Selvon, this conference) 29th ICRC Pune Auger: Galactic Center Coverage Significance (1.5º) 3.0 2.0 1.0 300 270 240 0.0 -1.0 -2.0 Significance (3.7º) Significance (13.3º) -3.0 29th ICRC Pune Mass Compositon (Xmax) Filled circles, HiRes; Triangles, HiRes/MIA, Open circles, Fly’s Eye (shifted). HiRes+Fly’sEye(shifted) LightHeavyLight? (Sokolsky, this conference) 1EeV 29th ICRC Pune Particle Physics Outputs HiRes : s inp Air 456 17 ( stat ) 39( sys ) 11( sys ) mb (Mathews, this conference) 29th ICRC Pune So What we have seen? GZK strikes back! Needs cautions on energy scale, but the spectrum is consistent with the cutoff No anisotropy…. Except some possible indication.. Deficit in anti-galactic center, BL-Lac correlation Then… what we can do to pin down UHECR origin ? ADDING MORE (GOOD) DATA! 29th ICRC Pune Multi Wavelength Particle spices observation GZK photons/Neutrinos lead to information on EHE cosmic ray source distribution, radio background, and extragalactic B. Photon-induced EAS search LPM + Geomagnetric Preshower effects Xmax anomaly •HiRes (O’Neill, this conference) •Auger (Risse, this conference) Fg(Eg>10EeV) < 26 % 29th ICRC Pune EHE Neutrino Observatory Deeply penetrating inclined EAS search Auger (Nellon, this conference) HiRes …. IceCube (In-ice Cherenkov light detector) (Chirkin, this conference) Rice (In-ice Cherenkov Radio detector) ANITA (In-Flight Cherenkov Radio detector) (Duvernois, this conference) Acoustic Extension (In-ice Acoustic detector) (Nahanhauer, this conference) 29th ICRC Pune IceCube IceTop 1km3! Deep Ice Array (Chirkin, this conference) 29th ICRC Pune IceCube Conventional Technique extends up to EHE! 1EeV t 300 PeV cascade IceCube Yoshida et al PRD 69 103004 (2004) 29th ICRC Pune “Hybrid” tech to extend ++1km3 “conventional” detector provides “test” beam! Use IceCube holes 3 distant holes down to 400 m 7 stations per hole sensor, transmitter, auxiliary det. per station Deployment January 2006 Results Summer 2006 Rolf Nahanhauer (this conference) 29th ICRC Pune Future Outlook Auger: 7 x AGASA by 30th ICRC HiRes: <2 years STEREO data to be analyzed. ~70% more statistics “independent” dataset for testing the “BL Lac” New observatory in the Northern sky Telescope Array Telescope Array 576 plastic scintillation Surface Detectors (SD) 5 communication towers 3m2 1.2cm t Atmospheric fluorescence telescope 3 stations FD Middle Drum SD two layers 1.2km spacing Black Rock Mesa Long Ridge 20km Sensitivity of SD : ~9 x AGASA 29th ICRC Pune Test Observations @ Millard county, Utah (Ogio, this conference) 3-13 July, 2005 @ Black Rock Mesa site Single telescope with 256ch PMTs camera Typical waveform with fluorescence light (RUN65,TRIG165, CH89) Total observation time: 31.5 hours s5 ADC count = 2.5 p.e./100 ns 1st level trigger threshold: 6 - 6.5 sigma Trigger rate: 0.6 - 1.5 Hz An observed shower-like track (11 July, 2005) ch# Recorded waveforms degree Analysis result SDP dc cc ba preliminary aa 99 89 78 logE(eV) = 18.05 68 57 46 Xmax = 674.9 g/cm2 q = 46.2o 35 Relative time degree 29th ICRC Pune Future Outlook Auger: 7 x AGASA by 30th ICRC HiRes: <2 years STEREO data to be analyzed. ~70% more statistics “independent” dataset for testing the “BL Lac” New observatory in the Northern sky Telescope Array • EHE gamma ray/Neutrino search EAS detector, IceCube, Rice, ANITA etc. 29th ICRC Pune Thank you! Nos vemos en Mejico!! S.Yoshida