Recent As γ results +History+Future

1. Recent Asγ results+History+Future Introduction Brief history of the experiment Recent results γ ray observation Knee physics Future plan MUON dector “Shower” Core detector

2. CR spectrum LHC Ecm LHC Elab 3PeV Steepenning spectrum: Ground based Observation is necessary 3EeV Emax~ Z (Berezhko)

3. Emax=βZBL Solar flares:1011eV AGN: 1018-20eV Crab :1016eV SN1006: 1016eV (Hillas plot)

4. 宇宙线在地球 大气层中引发 广延大气簇射 (Extensive Air Shower) 的原理示意图

5. Advantage of YangBaJingaltitude(4300M) Number of secondary reach maximum, infavor of knee physics, including composition and spectrum measurement. Low energy threshold, in favor of γ ray astronomy Better angular,energy resolution knee γ ray astronomy (Ong)

6. YBJ Satisfy all the requirements 90km NW from Lhasa ~1º slope; 4300 m a.s.l. 90º53’E, 30º11’N Shigatse

7. Requirements on Observation Site high quality operation, low cost and long life-span: • Altitude4300m a.s.l. • Topographyflat and wide, plenty of space. • Climate easy for construction, operation & living. • Traffic accessible to highway, airport or railway station. • Power existed electric power line network. • Logistics not far from local town/modern city. • Neighborhood 1000s of residents: clinic, post office, school … • CommunicationTelephone, mobile phone, high speed optical fibre network (155Mbps today).

8. History of ASγ development 3TeV;115Hz;0.9 o; 3TeV;1700Hz;0.87 o BD(1996)

9. Asγ,ARGO (High Duty cycle,Large F.O.V) e m g ~TeV ~100GeV 中意合作 ARGO实验RPC大厅 中日合作 AS γ实验区闪烁体探测器阵列 ARGOhall, floored by RPC. Half installed. AS γ scintillation counter MILAGRO,Jemez（2630M）

10. Gamma ray emission from Crab (TibetII-HD : 5.5σ,ApJ 525,L93,1999)

11. Mrk501 (TibetII HD)ApJ 532,302(2000) Feb.1997-Aug.1997. Only observation from conventional air shower array.

12. Mrk421 (6.9σ) AS γ比切伦可夫望远镜更长时间地观测了2000-2001年间Mrk421的爆发。

13. 太阳宇宙线 1) 最先观测到宇宙线太阳阴影； 2）寻找与太阳耀斑，GLE事件相伴随的高能宇宙线发射。

14. Allsky Survey (1999.11-2004.10) PRELIMINARY

15. Flux Limit (1999.11-2004.10) Preliminary Milagro limit

16. Indirect search of DM

18. Diffuse TEV gamma ray from the Galactic Plane γ>100MeV　（EGRET） Effective Area ９９％C.L. ９９％C.L. ９９％C.L. Tibet-III (22,050m2) 1041.3 days (1999 Nov.~2004 Oct.)

19. Two dimensional observation on large scale anisotropy of TeV Cosmic-ray using the Tibet Air Shower Array (Preliminary)

20. EC and BD Total EC area : 80 m2 ; 80 channels electronics + 600 channels from shower array

21. KASCADE (~100K channels of electronics！！！） e/m Hadron

22. All All Preliminary Preliminary Proton Proton KASCADE (P) -3.11 Present Results Present Results -3.13 KASCADE (P) J. Huang Primary proton spectrum(analyses based on Corsika_QGSJETand SIBYLL ) (KASCADE data: astro-ph/0312295)

23. Tibet III + MUON 8,640 m2

24. （μ数＝0　→　0.12　と表示） 0.4 10TeV 10TeV 100TeV (gamma) 100TeV (gamma) Number of μ in MUON detector

25. MAGIC Tibet-III VERITAS HESS Tibet-III+WC Detection Sensitivity of Tibet-III+WC (3 years 5σ) Tibet-III Scintillation Counters 37,000m2 + Underground Water Cherenkov Detector 8,640m2 Crab orbit Flat region (> 200TeV) Background << 1 event 15 photon sensitivity (Poisson 5σ)

26. Consistent with power low Extrapolation Energy Spectrum of HESS sources Aharonian et al, ApJ, 636, 777 (2006) Indices are harder (If it is constructed in the southern hemisphere) Most of HESS sources detectable by Tibet III+WC!

27. Pb Iron Scint. Box Design of detector 20 detectors Conclusion Pb=7cu, Spacing=3.75m, Nb>100 YAC array 20 detectors 7cu Tibet III 3.75m YAC 3.75m AS

28. Primary energy range M. Shibata

29. Summary YangBaJing is an unparalleled observatory AS γ has been very successful Looking forward to seeing TIBET-III/MUON, HAWC & other projects will get going in YBJ