Astrophysical signatures of light dark matter

Not so dark matter

Reality

The 511 keV line

Gamma rays

Heat from cold dark matter?

Conclusions



  • Why dark matter?
    • Intensity
    • Morphology

  • Free parameters (Ascasibar et al. 2006)
    • Dark matter mass
    • Decay or annihilation rate
    • Milky Way density profile

  • A picture of the dark matter halo
    • Inner slope 1.03 ± 0.04

  • Constraints on the dark matter zoo
    • Annihilating, not decaying
    • a=10 -30mMeV2 cm3 s-1 => F
    • m<100 MeV => Z'
    • m>100 MeV => secondary e+

Yago Ascasibar (Astrophysikalisches Institut Potsdam)
XLI Rencontres de Moriond (La Thuile, 24 March 2006)