伽马射线簇射在.PPT

排除CR本底的两种办法：横向分布和μ子数 Inside view of MD prototype 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） Background and signal Simulation study and data selection Simulation study and data selection Simulation study and data selection Event number by 1yr operation Sensitivity to diffuse electron 暗物质间接探测灵敏度：Sensitivity for diffuse electronvs electron fluxes from DM annihilation Pulsar Production of e+e- Potential power in detecting the electrons from nearby pulsar Survival efficiency 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 蟹状星云一年观测预期事例数 Sensitivity to DM electron Constrain to e+e- cross section GeV-TeV伽马射线源观测 宇宙线起源之谜 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 TibetIII+MD（5pool)+Einasto * 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 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 Mrk501，1997 TeV能区伽马点源的观测:Crab,Mrk421,Mrk501 Crab（6.3σ） MrK421高态爆发(6.9σ) All Sky Significance map  Solid line--all sky; Dashed line-gaus fit;