Tran - DESY Theory workshop 2008

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The Antideuteron Spectrum No cosmic-ray antideuterons have been detected yet, only upper limits exist Antideuterons may form by coalescence of an antineutron-antiproton pair that lies very closely together in momentum space Spectral shape of background and dark matter signal are different at low energies Detection of a single antideuteron at low energies could provide important clue David <strong>Tran</strong> Indirect Signatures of Gravitino Dark Matter with Broken R-Parity
Outline 1 Gravitino Dark Matter 2 Gamma Rays 3 Positrons 4 Antiprotons 5 Antideuterons 6 Conclusions David <strong>Tran</strong> Indirect Signatures of Gravitino Dark Matter with Broken R-Parity
Page 1 and 2: Indirect Signatures of Gravitino Da
Page 3 and 4: Outline Based on A. Ibarra and D. T
Page 5 and 6: Indirect Detection Even for graviti
Page 7 and 8: The Gamma-Ray Spectrum The diffuse
Page 9 and 10: The Gamma-Ray Spectrum Calculate de
Page 11 and 12: The Gamma-Ray Spectrum Spectrum for
Page 13 and 14: The Gamma-Ray Spectrum Heavier grav
Page 15 and 16: The Gamma-Ray Spectrum Fragmentatio
Page 23 and 24: Outline 1 Gravitino Dark Matter 2 G
Page 25 and 26: The Positron Fraction Propagation i
Page 27 and 28: The Positron Fraction Experiments u
Page 29 and 30: The Positron Fraction Using the EGR
Page 31 and 32: The Positron Fraction The coinciden
Page 33 and 34: The Antiproton Spectrum Theoretical
Page 35 and 36: The Antiproton Spectrum Primary top
Page 37: Outline 1 Gravitino Dark Matter 2 G
Page 41 and 42: Overview of the Indirect Signatures

Tran - DESY Theory workshop 2008

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