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Analysis strategies and recent results from AMANDA-II

Analysis strategies and recent results from AMANDA-II. Overview. Introduction: Neutrino detection AMANDA-II Analysis strategies results: Point-source Stacking of point-source (AGN) Isotropic / diffuse analysis Diffuse energy spectrum. Astroparticle physics. 677 PMTs on 19 strings

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Analysis strategies and recent results from AMANDA-II

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  1. Analysis strategies and recent results from AMANDA-II

  2. Overview • Introduction: • Neutrino detection • AMANDA-II • Analysis strategies results: • Point-source • Stacking of point-source (AGN) • Isotropic / diffuse analysis • Diffuse energy spectrum

  3. Astroparticle physics

  4. 677 PMTs on 19 strings Cherenkov light South Pole Dome road to work AMANDA Summer camp 1500 m Amundsen-Scott South Pole Station 2000 m [not to scale] AMANDA/IceCube

  5. Stacking strategy – sum signal of point sources of same source class Search for a diffuse signal: use complete northern hemisphere Analysis strategies Point source searches – significance map ?clustering of neutrinos identified photon sources AMANDA/IceCube field of view: northern hemisphere

  6. Other strategies • Cascade analyses • Transient searches: • Flares of permanent objects • Gamma Ray Bursts  stacking approach, temporal clustering • SGR 1860-20 • Dark matter searches • WIMPs • Magnetic Monopoles • Atmospheric muons, charm contribution great but too short time!

  7. Search for single point sources Event map 4282 events in 5 years (2000-2004) –effective time: 1001 days 90% confidence levelflux upper limits for the northern hemisphere in 0.5 deg bins (15% systematic error included) Achterberg et al. 2007,astro-ph/0611063

  8. Search for single point sources Limit map No significant signal 90% confidence levelflux upper limits for the northern hemisphere in 0.5 deg bins (15% systematic error included) Achterberg et al. 2007,astro-ph/0611063

  9. Stacking of AGN • GeV blazars (EGRET) – GeV • Unidentified EGRET sources – unidGeV • Infrared sources – IR • HAEO-A-detected keV sources – keV(H) • ROSAT-detected keV sources – keV(R) • TeV blazars - TeV • Compact Steep Spectrum and Giga-Hertz peaked sources – CSS/GpS • FR-I galaxies including M87 – FR-I(M) • FR-I galaxies without M87 – FR-I • FR-II galaxies – FR-II • Radio-weak quasars – QSO Achterberg et al. 2007,astro-ph/0611063

  10. Stacking of AGN Achterberg et al. 2007,astro-ph/0611063

  11. Isotropic / diffuse analysis • Atmospheric neutrino flux follows Eν-3.7 • Search for extra-galactic contribution • AGN (1) (Becker/Biermann/ Rhode) • AGN (3 and 4) (Mannheim/Protheroe/ Rachen) • GRBs (2) (Waxman/Bahcall)

  12. AMANDA 2000-03 W-B IceCube 1 yr Isotropic / diffuse analysis Achterberg et al., astro-ph/0705.1315

  13. Diffuse energy spectrum • General case: • measured distr. → unfolding → true distr. • Using RUN for unfolding: • measured distr. A (E) • measured distr. B (E) → RUN → energy distribution • measured distr. C (E) • More than three measured distributions (E): • combine N-2 observables to a new variable • using a neural network for combining

  14. Diffuse energy spectrum variable 1 variable 2 variable 3 variable 4 variable 5 variable 6 Neural Net RUN variable 7 variable 8

  15. Diffuse energy spectrum comparison: result 2000 with 2000-2003 preliminary preliminary

  16. Fit on atm. prediction (2000-2003) preliminary preliminary • Fit on the atmos. prediction (Volkova) • (atmos.+ extrat.)  flux – (fit value)  flux

  17. Limits preliminary [1] Achterberg et al., astro-ph/0705.1315

  18. Summary • Data from 2000-2004 taken with AMANDA-II are analyzed • Different search strategies: • Steady point sources (single sources & stacking) • Diffuse search, spectrum up to 100 TeV • …and more… • Analyses show so far no signal above atmospheric flux • Constraints on current models possible • Future: IceCube

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