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Cosmic Ray Backgrounds for Dark Matter Indirect Detection

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If you have a question about this talk, please contact Kazuki Sakurai.

Although cold dark matter has proven successful in explaining astrophysical observations on a wide range of scales, its particle physics nature has so far not been uncovered. If the dark matter particle was in fact weakly interacting one possible way of investigation would be the observation of high energy particles from the dark matter annihilation or decay in the galactic halo. Recently, apparent anomalies in charged lepton cosmic rays as well as in galactic microwaves have been interpreted in terms of such interactions. In this talk I will argue that the standard astrophysical backgrounds considered in these analyses are in fact much more complex than previously thought. In particular, I will explain how the acceleration of secondary leptons produced inside old supernova remnants can explain the observed signatures. I will also discuss how the foreground subtraction employed to reveal the so-called WMAP haze can produce fake signatures.

This talk is part of the HEP phenomenology joint Cavendish-DAMTP seminar series.

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