Abstract
We present a search for a neutrino signal from dark matter self-annihilations in the Milky Way using the IceCube Neutrino Observatory (IceCube). In 1005 days of data we found no significant excess of neutrinos over the background of neutrinos produced in atmospheric air showers from cosmic ray interactions. We derive upper limits on the velocity averaged product of the dark matter self-annihilation cross section and the relative velocity of the dark matter particles langle sigma _{text {A}}vrangle . Upper limits are set for dark matter particle candidate masses ranging from 10 GeV up to 1 TeV while considering annihilation through multiple channels. This work sets the most stringent limit on a neutrino signal from dark matter with mass between 10 and 100 GeV, with a limit of 1.18cdot 10^{-23}text { cm}^3text {s}^{-1} for 100 GeV dark matter particles self-annihilating via tau ^+tau ^- to neutrinos (assuming the Navarro–Frenk–White dark matter halo profile).
Highlights
With the increasingly strong indications of the existence of extended halos of dark matter surrounding galaxies and galaxy clusters [1], there is much interest within the particle physics community to determine the nature and properties of dark matter [2]
We present a search for a neutrino signal from dark matter self-annihilations in the Milky Way using the IceCube Neutrino Observatory (IceCube)
In 1005 days of data we found no significant excess of neutrinos over the background of neutrinos produced in atmospheric air showers from cosmic ray interactions
Summary
With the increasingly strong indications of the existence of extended halos of dark matter surrounding galaxies and galaxy clusters [1], there is much interest within the particle physics community to determine the nature and properties of dark matter [2]. If WIMPs can self-annihilate into Standard Model particles and the dark matter density is sufficiently high, an excess of neutrinos and photons should be observed from parts of the sky with a large amount of dark matter, above the background of muons and neutrinos produced in the Earth’s atmosphere. The array consists of 78 vertical strings in a hexagonal grid with 60 digital optical modules (DOMs) [20] spaced evenly on each string every 17 m between 1450 and 2450 m below the surface. The strings outside the DeepCore sub-detector volume (indicated with a blue line in Fig. 1) are only used in the initial filtering of triggered data, and are chosen to be shielded by three rows of DOMs from the edge of the array
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
