曹臻，高能物理研究所 全国高能物理大会，非加速器分会 2010.04，南昌 羊八井ARGO实验综述 曹臻，高能物理研究所 全国高能物理大会，非加速器分会 2010.04，南昌

ASγ,ARGO (4300m，大视场，全天侯，低阈能) 第一代,~TeV 第二代,~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 ARGO RPC地毯 MILAGRO,（美国）（2630m） AS γ 闪烁计数器 e m g

中意合作ARGO十二年发展大事记 1998 50m2 RPC 试验性地毯在Italy测试成功 1998.11 INFN 与高能所签合作协议并于2000年ARGO立项 2001.6 羊八井大厅落成 2002.5 安装16 Clusters RPC，调试运行2 Cluster 2003.12 安装1500m2RPC,长期调试运行6 Clusters 2004.11 16个Clusters试运行获得成功后开始全面安装 2006.6 地毯(130Clusters ，5800m2)安装、调试成功， 开始正常运行 2006.7-9 捕捉到Mrk421爆发 2007.12 外围24个保护性Clusters投入运行 2009.1 第一篇科学论文在美国Astroparticle Phys. 发表 2009.10 大动态模拟读出系统安装 2010.04 第一篇γ天文论文在美国Astrophys.J.Lett.发表

按计划分阶段实现整个阵列的运行 2004.2 (6) 2004.6 (16) 2005.10 (78) 2004.12 (42) 子课题完成情况9： 按计划分阶段实现整个阵列的运行 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 35 36 37 38 39 40 41 42 43 44 45 46 47 48 49 50 51 52 53 54 55 56 57 58 59 60 61 62 63 64 65 66 67 68 69 70 71 72 73 74 75 76 77 78 79 80 81 82 83 84 85 86 87 88 89 90 91 92 93 94 95 96 97 98 99 100 101 102 103 104 105 106 107 108 109 110 111 112 113 114 115 116 117 118 119 120 121 122 123 124 125 126 127 128 129 130 131 132 133 134 135 136 137 138 139 140 141 142 143 144 145 146 147 148 149 150 151 152 153 154 155 156 157 158 159 160 161 162 163 164 165 166 167 168 169 170 171 172 173 174 175 176 177 178 179 180 181 182 183 184 185 186 187 188 189 190 191 192 193 194 195 196 197 198 199 200 201 202 203 204 205 206 207 208 209 210 211 212 213 214 215 216 217 218 219 220 221 222 223 224 225 226 227 228 229 230 231 232 233 234 235 236 237 238 2006.6 (130) 2006.1 (104) 2005.10 (78) 2004.12 (42) 2004.2 (6) 2004.6 (16) 何会海，2008-5-29 羊八井RPC地毯式阵列的建造及技术开发研究 4

报告内容 γ天文： 宇宙线物理： 反质子流强 太阳活动监测 AGN短期和长期监测 新γ源（扩展源）的全天搜索与观测研究 GRB follow-up 宇宙线物理： pp截面 宇宙线能谱 各向异性分布 反质子流强 太阳活动监测

月亮阴影和角度分辨率 月亮阴影量: 55σ 角分辨率: 0.5°系统偏差:<0.2°

Crab nebula as a Standard candle Angular resolution: <0.5˚ Pointing systematic: ~0.2 ˚ 累计14.5σ 灵敏度:~8σ/yr 0.63ICrab Crab 14.5σ

All Sky Survey Mrk421 is the brightest source except Crab Nebula: many flares MGRO 1908+06 confirmed by HESS Cygnus region: mystery New survey method GRB follow-up

Mrk421 flare monitoring: 10ICrab Whipple ARGO has seen a 4σeffect for 2008/05/02 and 2010/02/18 transient events.

Mrk421 monitoring for flares Short time scale and Long time scale Flares in 3 days: June 13th: ApJL714,208(2010)

γ天文II：Mrk421爆发现象观测 2006年7月至8月：5.9σ 2007年：非常平静 2008年1月至4月：~5.7σ 5.9σ ASM of RXTE 2006/07-08 2006/09 2006/10 2006/11 中方为主的初步结果提交了2007国际宇宙线大会,并写入INFN向政府提交的CVI2007报告! 5.9σ ARGO 2006年7月至8月：5.9σ 2007年：非常平静 2008年1月至4月：~5.7σ RXTE

A correlation between ARGO-YBJ and X-ray (hard and soft) in 2yr observation Swift Hard X-ray (15-50keV) 2008 flare 2009 flare

Differential light Curve no lag is found between X-flares and Gamma flares evidence for SSC model

3yr all sky survey sources with significance greater than 5σ Mrk421 11.9 σ 3yr all sky survey sources with significance greater than 5σ Crab 14.5σ MGRO 1908+06 5.4 σ

MGRO1908+06 LAT named it as PSR J1907.5+0602. It is a PWN. Discovery by Milagro, confirmed by HESS and VERITAS. HESS result shows that its intrinsic extension is 0.34˚ Big difference between spectra measured by HESS and MILAGRO ARGO-YBJ seems to support MILAGRO. in progress

Cygnus region: mystery Milagro VERITAS Tibet ASr R=1.5 deg Fermi LAT ARGO-YBJ At a level of +4σ, two new VERITAS sources seems to be seen by ARGO-YBJ However, the brightest MILAGRO source MJRO 2019+37 is NOT observed by ARGO. Variable source? Very hard spectrum? Or other reasons?

A Population study: Search for a group of sources 125 out of 205 LAT sources in ARGO FOV A Population study: Search for a group of sources For 8 LAT sources seen by Milagro with S>4 15 galactic PSR/PWN (Crab is excluded) top 11 TeV sources (F>10%ICrab)

GRB follow-up observation preliminary ≥20 GRBs in the FOV of the ARGO-YBJ detector per year. GRB 090902B，ARGO-YBJ sets an Ecut ≤ 55GeV. If the Ecut is due to EBL, it could be 15,50,60,70 GeV for such a GRB at z=1.822 according to different EBL models. ARGO-YBJ limit

1100 GeV 区间的流强上限 (scaler mode) 2005.08.15 以来,约40个SWIFT的GRB处于ARGO视场,且ARGO处于正常运行状态; “单粒子”数据(阈能较低)中没有观测到GRB; 流强上限已经被估计; 对已知红移的GRB（红色）,光子在传播过程中的吸收已经被考虑 Limits estimated assuming 2.5 as spectral index above 230 keV (peak of BATSE distribution)

ARGO-YBJ measurement on p-Air and p-p cross section TienShan,previous slide: 350+-15mb

Preliminary Preliminary energy spectrum From S. P. SWORDY, Space Science Reviews 99: 85–94, 2001. Preliminary Preliminary energy spectrum Using CRTNT+ARGO hybrid technique

The variation of CR anisotropy with median energy by using of 2 years data 0.7TeV [20-60] 1.5TeV [60-100] 3.9TeV >100 ASγ 22

Moon shadow and anti-particle Proton Anti-Proton ang. res. icrc0432

Sun shadow of 44.6σ Clear Off set of the position in N-S There is almost not off set in E-W. 6/2006-10/2009 906 days Θ<50 deg Nhit>100

Folding with Carington period of 27.3 days 18 sectors with 20º each Folding with Carington period of 27.3 days

Displacement vs. solar longitudes

Measurement of IMF (with a conventional model) At 1AU: B0 is the only parameter B(θ)=B0 sin(θ-θ0) IMFmedole(r>5Rsun) 8分钟 6-7天 R-3 1.6天 R-1

This corresponds to “see” IMF with 1.6 days in advance of actually sweeping the earth. This implies a potential capability of “forecasting” for magnetic storm due to solar events Cosmic ray deflection method vs. direct measurements using orbiting detectors

Conclusion 经过6年的艰苦摸索，2004年底开始大规模建设ARGO阵列，2006年中ARGO投入运行 自在第一个季度的观测中就捕捉到一个AGN Flare后，经历了3年漫长的统计量累积期，达到55σ月影、15σCrab，今年（2010年）终于迎来了收获期： γ天文：AGN短期和长期监测：ApJL和即将发表 γ源（扩展源）的全天搜索与观测研究：started GRB follow-up：尚未探测到GRB（APP，ApJ for ULs） 宇宙线物理：pp截面（PRD）、宇宙线能谱、各向异性分布 新物理探索：反质子流强 太阳活动监测：空间天气预报研究等（合作组内审阅）