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Can Planck constrain indirect detection of dark matter in our Galaxy?

Authors

  • Timur Delahaye,

    Corresponding author
    1. Instituto de Física Teórica UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, 28049 Madrid, Spain
      E-mail: timur.delahaye@uam.es
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  • Céline Bœhm,

    1. Institute for Particle Physics Phenomenology, Durham University, South Road, Durham DH1 3LE
    2. LAPTH, CNRS/UMR 5108, 9 chemin de Bellevue – BP 110, 74941 Annecy-Le-Vieux, France
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  • Joseph Silk

    1. Astrophysics Department, Oxford University, 1 Keble Road, Oxford OX1 3RH
    2. Institut d’Astrophysique de Paris, CNRS/UMR7095, 98 bis Boulevard Arago, 75014 Paris, France
    3. Department of Physics and Astronomy, The Johns Hopkins University, Homewood Campus, Baltimore, MD 21218, USA
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E-mail: timur.delahaye@uam.es

ABSTRACT

We investigate the synchrotron emission (both intensity and morphology) associated with generic dark matter particles and make predictions for the Planck experiment, using the Fermi data and a model for the astrophysical sources. Our results indicate that the morphology (and not only the intensity) of the synchrotron emission from both dark matter annihilations plus astrophysical source is frequency dependent. Expected signals for light and heavy dark matter candidates seem sufficiently different to potentially delineate the value of the dark matter mass using a thorough comparison between LFI and HFI data.

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