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Background + signal describe EGRET data!WdB, C. Sander, V. Zhukov, A. Gladyshev, D. Kazakov,EGRET excess of diffuse Galactic Gamma Rays asBackground Tracer of DM, + astro-ph/0508617, DMA signal A&A, describe 444 (2005) EGRET 51 data!50 GeVICπ 0 WIMPSπ 0ICWIMPSBrems.IC70Brems.Blue: background uncertaintyBlue: WIMP mass uncertaintyWim de Boer, Karlsruhe Seminar Oxford, May. 3, 2007 12
Analysis of EGRET data in 6 sky directionsA: inner GalaxyB: outer discC: outer GalaxyTotal χ 2 for all regions :28/36 ⇒ Prob.= 0.8 Excess above background > 10σ.D: low latitude E: intermediate lat. F: galactic polesA: inner Galaxy (l=±30 0 , |b|
Page 1 and 2: The dark connection between Canis M
Page 3 and 4: Thermal History of WIMPsThermal equ
Page 5 and 6: Example of DM annihilation (SUSY)χ
Page 7 and 8: EGRET on CGRO (Compton Gamma Ray Ob
Page 9 and 10: What about background shape?No SMNo
Page 11: Basic principle for indirect dark m
Page 15 and 16: Background scaling factors agree wi
Page 17 and 18: N-body simulations show: Progenitor
Page 19 and 20: Excess of DM from Canis Major +tida
Page 21 and 22: Inner Ring coincides with ring of d
Page 23 and 24: Magnetic fields observed in spiral
Page 25 and 26: What about supersymmetry?Present da
Page 27 and 28: Expected SUSY mass spectra in mSUGR
Page 29 and 30: Direct Detection of WIMPsWIMPs elas
Page 31 and 32: DM annihilation in Sun and EarthSUN
Page 33: Summary on WIMP searchesIndirect de

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