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Indirect Dark Matter Search with YBJ-AS Observatory

Explore the search for dark matter using the YBJ-AS Observatory. This outline covers the status of ground-based observations, data analysis with the AS experiment, results, and conclusions presented by Wu Hanrong. Learn about galactic halo, galaxy clusters, and more in the Indirect Dark Matter search. Discover the advantages and disadvantages of IACT and EAS arrays for this study. Get insights into the analysis methods and statistical significance. Conclusions on substructure detection, DM limits, and future search directions are provided.

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Indirect Dark Matter Search with YBJ-AS Observatory

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  1. Indirect dark matter search with YBJ-AS Observatory Outline • Introduction • Status of ground-based observations • Data analysis with AS experiment • Results 5. Conclusions Wu hanrong on behalf of YBJ-ASg collaboration 2008.09.24 TeVPA-IV@IHEP

  2. Gamma-ray flux from WIMP annihilation: Indirect Dark Matter search Astrophysics : Dark matter halo Particle Physics From Observation

  3. Target of indirect search • Galactic Halo • external galaxies • galaxy clusters • substructures • Galactic Center(GC) • Local Group galaxies • Mini-spikes around IMBH

  4. Indirect DM search—ground based observatory IACT arrays Advantage: Good angular resolution; gamma/hadron discrimination Disadvantage: limited FOV and duty cycle Advantage: large FOV, 90% duty cycle Disadvantage: no good gamma/hadron identifintification EAS arrays

  5. Data analysis with AS experiment

  6. Tibet AS Observatory • a.s.l. 4300 m (YBJ , Tibet) • 606g/cm2 • Large field of view • Duty cycle (>90%) • Mode Energy: ASγ(~3TeV) ARGO ASγ

  7. Schematic map of the array and data using in analysis Tibet-II Tibet-IIIB4 Statistic (after selection): ~1.86*10^10

  8. Equal 迭代 • analysis method

  9. 1.M31(10.7,41.3) Non: 2876965 Noff: 2875325.3 Nexc: 1639.7 Significance: 0.97 M31 全天图以及M31显著性 2. No high siginificant point (>5sigma) except known source crab and Mrk421 is detected

  10. 1. 90%C.L. limit— M31

  11. -------substructure (>5 ) 2. 90%C.L. limit— substructure Significance for BKG Significance for BKG+DM signal

  12. 2. 90%C.L. limit— substructure preliminary

  13. Conclusions • Detect no any substructure in the field of YBJ ASgamma observatory • Detect no DM from M31 • 90% C.L. upper limit on “thermally averaged annihilation cross section” between 10^-19cm^3s^-1 and 10^-22cm^3s^-1 is given • Future search, ARGO-YBJ(~300GeV)

  14. Thanks!

  15. 1. 90%C.L. Flux limit— M31 90%C.L. flux limit： DM spectrum From Observation Monte Carlo

  16. 2. 90%C.L. Flux limit— substructure -----Number of substructure for 800 toy MC trials BKG BKG+DM signal

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