Te V Crab Mrk 421 Mrk 501 Crab6

Te. V能区伽马点源的观测: Crab, Mrk 421, Mrk 501 Crab（6. 3σ） Mrk 501，1997 Mr. K 421高态爆发，2000&2001 (6. 9σ)

All Sky Significance map —Smooth radius is optimal angular resolution(0. 99 °) thinking about the extension 0. 32 ° of MGRO J 2019+37 Mrk 421 Crab HEGRA J 2032+4130 MGRO J 2031+41 MGRO J 2019+37 MILAGRO C 1 Solid line--all sky; Dashed line-gaus fit; Dotted line-without Mrk 421 and Crab; Dot-dashed linewithout Mrk 421, Crab and MGRO J 2019+37;

Preliminary results on γ/e emission at 100 Te. V without having MUON detector Upper：Hints of 100 Te. V γ/e emission? Tibet-MUON will give an answer, which is due to contribute to origin problem of CRs. Middle : EAS-1000 prototype array from 100 Te. V to 10 Pe. V. Lower: γ ray observation by famous satelite experiment EGRET at Ge. V energy. (Zhaoyang Feng et al, ICRC 2009)

Preliminary results on γ/e emission at 100 Te. V without having MUON detector Upper：Hints of 100 Te. V γ/e emission? Tibet-MUON will give answer and making important contribution to CRs research. ！够不度敏灵 Middle : EAS-1000 prototype array from 100 Te. V to 10 Pe. V. Lower: γ ray observation by famous satelite experiment EGRET at Ge. V energy. (Zhaoyang Feng et al, ICRC 2009)

Tibet MD： 10, 000 m 2 underground Muon Detector 10 -100 Te. V能区世界上最灵敏的探测器 MD array --- 12 x 16 =192 muon detectors (~10, 000 m 2) --- 2. 5 m underground (~515 g/cm 2, ~19 X 0) Each muon detector --- Water pool, made of concrete --- 7. 2 m x 1. 5 m depth --- White waterproof surface --- 20” inch PMT x 2 (HAMAMATSU R 3600)

Inside view of MD prototype

Number of muons vs. Shower Size (Simulation) Sr : Sum of particle density by all scintillation det. 8 Shower Size （a measure of energy） SNPE : Sum of photoelectrons by all muon det. 8 the number of muons in air showers Survival Efficiency (Simulation) Energy SNPE cut value BG rejection g survival Sensitivity Eg: 1. 9 8 10 1000 Te. V 1. 9 Te. V 10 PEs ~30 PEs ~910 PEs 95. 4% ~99. 7% >~99. 99% 59% 2. 8 times improved ~61% ~11 times improved ~99% BG free

5 s or 10 ev. sensitivity to Point-like Gamma-ray Source 10 -100 Te. V能区世界上最灵敏的探测器 Background free 10 gamma-ray events sensitivity

Indirect Detection of DM at 10 Te. V region Ø In a model independent way, Ø χχ-> e+ e- , Natural Scale: <σv> = 3*10 -26 cm-3 s-1 Ø Einasto distribution, only considering the main halo Ø Considering transportation（GALPROP） FOV of YBJ 90 o 180 o -90 o

Background and signal

Simulation study and data selection l. Full simulation of Tibet III and MD for CRs and electron l. Data selection to get maximum S/B ratio： Theta<25 o（sec. Theta<1. 1) R<50 m l. Performace@10 Te. V： Energy Resolution：-30%-+50% Angular Resolution: 0. 5 o

Event number by 1 yr operation 10 Te. V 100 Te. V

Sensitivity to diffuse electron

暗物质间接探测灵敏度： Sensitivity for diffuse electron vs electron fluxes from DM annihilation

e+e- pair production between CR s and radiation BKG => knee Ap. J 700: L 170–L 173, 2009 August 1; (astro-ph/0901. 1520)

=> electron, positron excesses Ap. J 700: L 170–L 173, 2009 August 1; (astro-ph/0901. 1520)

Pulsar Production of e+ear. Xiv: 0812. 4457

Potential power in detecting the electrons from nearby pulsar

Summary l Tibet ASγ Experiment has been successfully operated since 1989 and fruitful results have been obtained. l 5 out of 12 MUON detectors are under construction in 2010. Tibet. III-MD is expected to resume data taking in 2011. Sensitivity of ASγ experiment for observing the γ ray point source will be Improved by about a factor of 10 at several tens of Te. V. le+ e- from DM annihilation could be detected in 10 Te. V region by Tibet. III+MD, If it follows the DM models used to explain the ATIC and PAMELA excess. l. Tibet III-MD will be sensitive in testing the models related to the astrophysics origin of e+/e- excesses

Pulsar Production of e+e. Advances in Space Research, Volume 27, Issue 4, 2001, 653 -658

Survival efficiency

Pollution of CRs and diffuse γ • Systematic error of cosmic rays survival efficiency ----Calibrated by Crab and Moon Shadow l Galactic and extra-Galactic diffuse γ rays at 10 Te. V region ----Detailed consideration, other experiments, theoretic calculation

蟹状星云一年观测预期事例数 ECR： 4. 0 5. 0 7. 0 11. 1 19 Eγ： 1. 9 2. 4 3. 5 5. 6 9. 8 39 20 80 39 184 89 348 210 900 Te. V 550 Te. V

Sensitivity to DM electron

Constrain to e+e- cross section Tibet. III+MD（5 pool)+Einasto

P, He by Tibet hybrid Experiment (Phys. Lett. B, 632, 58 (2006)) Primary Proton spectrum Primary Helium spectrum (All - (P+He)) /All 1) Our results shows that the main component responsible for the knee structure of the all particle spectrum is heavier than helium nuclei. ２） The absolute fluxes of protons and helium nuclei are derived within 30% systematic errors depending on the hadronic interaction models.

Ge. V-Te. V伽马射线源观测 Fermi卫星发射后前11个月观测到的1451个点源（100 Me. V 100 Ge. V) 106个Te. V point Source （61 gal + 45 extra-gal, up to 2010/11/11）

CR+photon->CR+(e+e-) • CR knee has a energy of 4 Pe. V, and is related mainly with proton and Helium. • Many observation suggests that the major component is He. • 4 Pe. V energy to He corresponds to a Lorentz factor of 106, just the right value for (e+e-) pair production when interacting with 5000 Ko (~1 e. V) background photon and can produce e+/e- at ~500 Ge. V! • The energy flow of ATIC excess electron is 10 -4 Ge. V/cm 2 s. Sr, between 80 Ge. V- 900 Ge. V, as same as the energy loss of CRs assuming that the cosmic rays change their spectrum indices from -2. 7 to 3. 1 above ~ Pe. V;