Abstract
Neutrino detectors participate in the indirect search for the fundamental constituents of dark matter (DM) in form of weakly interacting massive particles (WIMPs). In WIMP scenarios, candidate DM particles can pair-annihilate into Standard Model products, yielding considerable fluxes of high-energy neutrinos. A detector like ANTARES, located in the Northern Hemisphere, is able to perform a complementary search looking towards the Galactic Centre, where a high density of dark matter is thought to accumulate. Both this directional information and the spectral features of annihilating DM pairs are entered into an unbinned likelihood method to scan the data set in search for DM-like signals in ANTARES data. Results obtained upon unblinding 3170 days of data reconstructed with updated methods are presented, which provides a larger, and more accurate, data set than a previously published result using 2101 days. A non-observation of dark matter is converted into limits on the velocity-averaged cross section for WIMP pair annihilation.
Highlights
With Ω being the solid angle under which the source is observed, and s the radial coordinate integrated over the line of sight (l.o.s.)
We observed a TS smaller than the background median for all cases, we set all limit values equal to the corresponding sensitivities. This measurement sets limits on the cross section for weakly interacting massive particles (WIMPs)-pair annihilation shown in Figure 1 and computed according to Equation (2)
The total amount of dark matter within a 30◦ angle around the Galactic Centre is taken into account, which corresponds to the Burkert τ+ τMcMillan τ+ τNFW τ+ τ
Summary
With Ω being the solid angle under which the source is observed, and s the radial coordinate integrated over the line of sight (l.o.s.) (see [2] for a detailed discussion). The Galactic Centre is a promising source for its large predicted DM density; it is a target of complementary searches for neutrino detectors and γ-ray telescopes, due to the low source contamination that would give way to an unambiguous signal identification. The flux of neutrinos reaching the Earth from a WIMP pair annihilation can be expressed as a function of the thermally averaged cross section σv for WIMP pair annihilation, of the energy distribution of outcoming particles per WIMP pair collision dN/dEν , and of the DM distribution represented by the J-factor: dΦ(Eν ) dEν. The spherically averaged DM density profile ρ contained in the J-factor (Equation (1)) is modelled according to different assumptions, leading to considerably different results. The main assumptions on ρ are based on cosmological N-body simulation results and/or dynamical constraints on the Milky Way or spiral galaxies.
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