Speaker
Description
The method of indirect detection of Dark Matter (DM) in neutrino telescopes involves the observation of a Cherenkov light pattern produced by particles crossing the detector that originate from DM annihilation or decay. A signal of neutrinos produced by these processes is searched for in astrophysical targets such as the Galactic Centre or the Sun, where large amounts of DM are believed to accumulate. The KM3NeT infrastructure, located in abyssal sites of the Mediterranean Sea, includes multiple detectors, among which ORCA is optimized for measuring low-energy neutrinos. In its final configuration, ORCA will consist of 115 vertical detection lines, each containing 18 optical modules with 31 photomultiplier tubes that detect light signals. In this contribution we present an analysis with an unbinned likelihood method looking for WIMP-like DM annihilations occurring at the Galactic Centre, where we consider DM with masses ranging from approximately 1 GeV up to 1 TeV. We use various partial ORCA-detector configurations ranging from 6 to 18 lines to explore low masses.
| Main Contribution topic | Indirect detection |
|---|---|
| Secondary contribution topic | Indirect detection |