Abstract
The KM3NeT Collaboration has started the construction of a research infrastructure hosting a network of underwater neutrino detectors in the Mediterranean Sea. Two instruments based on the same technology are being built: KM3NeT/ORCA to measure the neutrino mass hierarchy and to study atmospheric neutrino oscillations and KM3NeT/ARCA to detect high-energy cosmic neutrinos both in diffuse and point source mode. The excellent angular resolution of the ARCA detector, with an instrumented volume of about one Gton, will allow for an unprecedented exploration of the neutrino sky searching for neutrinos coming from defined sources of sky regions, like the Galactic Plane and the Fermi Bubbles. It will also look for diffuse high energy neutrino fluxes following the indication provided by the IceCube signal. This contribution will report on the sensitivity of the KM3NeT/ARCA telescope with particular attention to the region of the Galactic Plane. Comparisons with theoretical expectations are also discussed.
Highlights
The KM3NeT Collaboration has started the construction of the generation neutrino detectors, being built in the Mediterranean Sea
A large volume neutrino telescope, called ARCA [1], will be devoted to the search for high energy cosmic neutrinos while a more dense and compact neutrino detector, ORCA [1], will study the neutrino mass hierarchy looking at low energy atmospheric neutrino oscillations
A further rejection of atmospheric tracks, both from atmospheric muons and neutrinos, via an energy-related cut is obtained cutting on the total time over threshold (ToT) of hits selected by the shower reconstruction algorithm
Summary
The KM3NeT Collaboration has started the construction of the generation neutrino detectors, being built in the Mediterranean Sea. Cherenkov light emitted by charged particles produced by all flavour neutrino interaction will be detected to reconstruct the neutrino direction and energy The observed flux is compatible with isotropic origin and equipartition in the three neutrino flavours as expected from neutrino oscillations in vacuum [5]. Individual sources of this excess could not be identified, nor has the production mechanism for these high energy neutrinos been determined. The results presented here do not depend strongly on the assumed signal flux
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