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TibetIII (2003-)

TibetIII (2003-). 观测站 西藏羊八井， 海拔4300m（大气深度606g/cm 2 ) 现有阵列: 50,400 m 2 闪烁体探测器 :0.5 m 2 x 789个 其中： 快时间光电倍增管 761个，动态范围：0－15个粒子，时间分辨0.8ns 大动态光电倍增管 277个，动态范围：15－500个粒子 Energy resolution: 10 TeV ~+70%-40% 100 TeV ~+40%-30% Angular resolution : 10TeV:0.5 o

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TibetIII (2003-)

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  1. TibetIII (2003-) 观测站 西藏羊八井， 海拔4300m（大气深度606g/cm2) 现有阵列:50,400 m2 闪烁体探测器:0.5 m2 x 789个 其中： 快时间光电倍增管 761个，动态范围：0－15个粒子，时间分辨0.8ns 大动态光电倍增管 277个，动态范围：15－500个粒子 Energy resolution:10 TeV ~+70%-40% 100 TeV ~+40%-30% Angular resolution: 10TeV:0.5o 100TeV:0.2o

  2. TibetIII (2003-) 观测站 西藏羊八井， 海拔4300m（大气深度606g/cm2) 现有阵列:50,400 m2 闪烁体探测器:0.5 m2 x 789个 其中： 快时间光电倍增管 761个，动态范围：0－15个粒子，时间分辨0.8ns 大动态光电倍增管 277个，动态范围：15－500个粒子 Energy resolution:10 TeV ~+70%-40% 100 TeV ~+40%-30% Angular resolution: 10TeV:0.5o 100TeV:0.2o 优势： 高海拔 全天候， 宽视场 缺点： 不能有效区分宇宙线强子与电磁成分

  3. TeV能区伽马点源的观测:Crab,Mrk421,Mrk501 Crab（6.3σ） Mrk501，1997 MrK421高态爆发，2000&2001 (6.9σ)

  4. All Sky Significance map Solid line--all sky; Dashed line-gaus fit; Dotted line-without Mrk421 and Crab; Dot-dashed line-without Mrk421,Crab and MGRO J2019+37; MGRO J2019+37 —Smooth radius is optimal angular resolution(0.99 °) thinking about the extension 0.32 ° of MGRO J2019+37 Mrk421 Crab HEGRA J2032+4130 MGRO J2031+41 MILAGRO C1

  5. 中日数据间接寻找暗物质湮灭信号 湮灭截面 暗物质质量

  6. 中日数据间接寻找暗物质湮灭信号 湮灭截面 灵敏度不够！ 暗物质质量

  7. Preliminary results on γ/e emission at 100TeV without having MUON detector (Zhaoyang Feng et al, ICRC2009) Upper：Hints of 100TeV 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 100TeV to 10 PeV. Lower: γ ray observation by famous satelite experiment EGRET at GeV energy.

  8. Preliminary results on γ/e emission at 100TeV without having MUON detector (Zhaoyang Feng et al, ICRC2009) Upper：Hints of 100TeV γ/e emission? Tibet-MUON will give answer and making important contribution to CRs research. 灵敏度不够！ Middle : EAS-1000 prototype array from 100TeV to 10 PeV. Lower: γ ray observation by famous satelite experiment EGRET at GeV energy.

  9. 排除CR本底的两种办法：横向分布和μ子数 100TeV伽马射线簇射在ybj高度 100TeV质子簇射在ybj高度 分辨二： 缪子数差别 分辨一： 横向分布差别

  10. Tibet MD：10,000m2 underground Muon Detector 10-100TeV能区世界上最灵敏的探测器 MD array --- 12 x 16 =192 muon detectors (~10,000 m2) --- 2.5m underground (~515g/cm2, ~19X0) Each muon detector --- Water pool, made of concrete --- 7.2m x7.2m x 1.5m depth --- White waterproof surface --- 20” inch PMT x 2 (HAMAMATSU R3600)

  11. Tibet MD：10,000m2 underground Muon Detector 10-100TeV能区世界上最灵敏的探测器 MD array --- 12 x 16 =192 muon detectors (~10,000 m2) --- 2.5m underground (~515g/cm2, ~19X0) Each muon detector --- Water pool, made of concrete --- 7.2m x7.2m x 1.5m depth --- White waterproof surface --- 20” inch PMT x 2 (HAMAMATSU R3600)

  12. Inside view of MD prototype

  13. 8 8 8 Sr :Sum of particle density by all scintillation det. Shower Size（a measure of energy） SNPE :Sum of photoelectrons by all muon det. the number of muons in air showers Number of muons vs. Shower Size (Simulation) Survival Efficiency (Simulation) Eg: 1.9 10 100 1000 TeV

  14. 5s or 10 ev. sensitivity to Point-like Gamma-ray Source 10-100TeV能区世界上最灵敏的探测器 Background free 10 gamma-ray events sensitivity

  15. 宇宙线轻子起源与强子起源，多波段联合观察 A&A，464(2007)235-243 SNR RXJ1713.7-3946 • 已有的多波段观测 + 100TeVγ射线观测有助于确定宇宙线强子源 • 极大地增强了我们对宇宙线强子源的认识，有望回答宇宙线起源的问题 强子模型

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

  17. Background and signal

  18. Full simulation of Tibet III and MD for CRs and electron • Data selection to get maximum S/B ratio： • Theta<25o（secTheta<1.1) • R<50m • Performace@10TeV： • Energy Resolution：-30%-+50% • Angular Resolution: 0. 5o Simulation study and data selection

  19. Full simulation of Tibet III and MD for CRs and electron • Data selection to get maximum S/B ratio： • Theta<25o（secTheta<1.1) • R<50m • Performace@10TeV： • Energy Resolution：-30%-+50% • Angular Resolution: 0. 5o Simulation study and data selection

  20. Full simulation of Tibet III and MD for CRs and electron • Data selection to get maximum S/B ratio： • Theta<25o（secTheta<1.1) • R<50m • Performace@10TeV： • Energy Resolution：-30%-+50% • Angular Resolution: 0. 5o Simulation study and data selection

  21. Event number by 1yr operation 100TeV 10TeV

  22. Sensitivity to diffuse electron

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

  24. e+e- pair production between CR s and radiation BKG => knee ApJ 700:L170–L173, 2009 August 1; (astro-ph/0901.1520)

  25. => electron, positron excesses ApJ 700:L170–L173, 2009 August 1; (astro-ph/0901.1520)

  26. Pulsar Production of e+e- arXiv:0812.4457

  27. Potential power in detecting the electrons from nearby pulsar

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

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

  30. Survival efficiency

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

  32. 蟹状星云一年观测预期事例数 ECR：4.0 5.0 7.0 11.1 19 39 80 184 348 900 TeV Eγ： 1.9 2.4 3.5 5.6 9.8 20 39 89 210 550 TeV

  33. Sensitivity to DM electron

  34. Constrain to e+e- cross section TibetIII+MD（5pool)+Einasto

  35. P, He byTibet 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.

  36. GeV-TeV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（100MeV-100GeV) 106个TeV point Source （61 gal + 45 extra-gal, up to 2010/11/11）

  37. 宇宙线起源之谜 • 主要是原子核：P，He，…, Fe,… • 也有：，e± • 还有：γ，ν • 非热能谱 dN/dE∝E-α • 各向同性的分布 一些能区有微弱各向异性 流强 1030 河外？ “膝”区（4PeV） 以下是河内起源？ 1912-, Hess，但 • 哪里产生？ • 如何加速？ 1011 能量

  38. CR+photon->CR+(e+e-) CR knee has a energy of 4PeV, and is related mainly withproton and Helium. Many observation suggests that the major component is He. 4PeV energy to He corresponds to a Lorentz factor of 106, just the right value for (e+e-) pair production when interacting with 5000Ko(~1eV)background photon and can produce e+/e- at ~500GeV! The energy flow of ATIC excess electron is10-4GeV/cm2sSr, between 80GeV- 900GeV, as same as the energy loss of CRs assuming that the cosmic rays change their spectrum indices from -2.7 to -3.1 above ~ PeV;

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