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What is known about Dark Matter?• 95% of the energy of the Universe isnon-baryonic23% in the form of Cold Dark MatterFrom CMB + SN1a + surveys• Dark Matter enhanced in Galaxies and Clustersof Galaxies but DM widely distributed in halo->DM must consist of weakly interacting andmassive particles -> WIMP’sIf it is not darkIt does not matter• Annihilation with =2.10 -26 cm 3 /s,if thermal relicDM halo profile of galaxycluster from weak lensingWim de Boer, Karlsruhe Seminar Oxford, May. 3, 2007 2
Thermal History of WIMPsThermal equilibrium abundanceActual abundanceComoving number densityT=M/22x=m/TJungmann,Kamionkowski, Griest, PR 1995T>>M: f+f->M+M; M+M->f+fTf+fT=M/22: M decoupled, stable density(when annihilation rate ≅ expansionrate,i.e. Γ=nχ(x fr ) ≅ H(x fr ) !)WMAP -> Ωh 2 =0.113±0.009 ->=2.10 -26 cm 3 /sDM increases in Galaxies:≈1 WIMP/coffee cup ≈10 5 .DMA (∝ρ 2 ) restarts again..Annihilation into lighter particles, likequarks and leptons -> π 0’s -> Gammas!Only assumption in this analysis:WIMP = THERMAL RELIC!Wim de Boer, Karlsruhe Seminar Oxford, May. 3, 2007 3
Page 1: The dark connection between Canis M
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 and 12: Basic principle for indirect dark m
Page 13 and 14: Analysis of EGRET data in 6 sky dir
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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