Cosmic rays from the halo of the MW some weak hints°DM2 SUSY+bkg fit B heAt 200 ● Some astrophysics SUSY component D heAt 94+95 bkg. component observations can not be bkg. only fit m=238 Gev h2=0092 explained by the canonical physics They may indicate the signal of DM. however g no conclusion can be dr rawn now. ● One of such tanB=28 experiments is the m,=122 GeV HEAT. (The HEAT △ a, SUSY)=168×10-10 N=0.720,B=116.7 signal may indicate thel x2=138/dof non-thermal production or the positron energy (GeV) subhalo nearby)
Cosmic rays from the halo of the MW— some weak hints on DM ⚫ Some astrophysics observations can not be explained by the canonical physics. They may indicate the signal of DM, however, no conclusion can be drawn now. ⚫ One of such experiments is the HEAT. (The HEAT signal may indicate the non-thermal production or the subhalo nearby) Baltz et al. 2002
ASy and ARGO: (High Duty cycle, Large FO.v 100Gev Tev 中意合作ARGO实验RPC大厅 中日合作ASY实验区闪烁体探测器阵列 Here comes the two experiments hosted by yBJ observatory. One is ARGO hall, floored by call ASy, a sampling detector covering 1% of the area and have been operated for 15 years. The other full coverage one is called ARGO, still RPC. Half installed under installation A Sy use scintillation counter and aRgo use RPC to detector the arrival time and the number of secondary particles, with which the original direction and energy of Cr particle can be restored ASy has a threshold energy at a few Tev while aRGO down to about 100GeV. Both experiment have the advantages in hig large field of view. Because for both of the experiments there is only one layer of detector, it is very difficult to separate the y ray shower from CR nuclei showers. Working in the simi lar energy range on mountain Jemez near Los Alamos, by using water cherenkov technique milagro has two layer of pmt, which enable it a rather good capability to separate y ray from background. Though it locates in a low altitude, has a smaller effective area, it has similar sensitivity to greatly improve the sensitivity of our current EAS experiment d ASy experiment. To combine this technique with high altitude wo
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 ASg and ARGO： (High Duty cycle,Large F.O.V) ~100GeV ~TeV ARGO hall, floored by RPC. Half installed. Here comes the two experiments hosted by YBJ observatory. One is call ASg, a sampling detector covering 1% of the area and have been operated for 15 years. The other full coverage one is called ARGO, still under installation. ASg use scintillation counter and ARGO use RPC to detector the arrival time and the number of secondary particles, with which the original direction and energy of CR particle can be restored. ASg has a threshold energy at a few TeV while ARGO down to about 100GeV. Both experiment have the advantages in high duty cycle and large field of view. Because for both of the experiments there is only one layer of detector, it is very difficult to separate the g ray shower from CR nuclei showers. Working in the similar energy range on mountain Jemez near Los Alamos, by using water cherenkov technique, MILAGRO has two layer of PMT, which enable it a rather good capability to separate g ray from background. Though it locates in a low altitude, has a smaller effective area, it has similar sensitivity to ASg experiment. To combine this technique with high altitude would greatly improve the sensitivity of our current EAS experiments