Next : Why neutrino astronomy?


The ANTARES Collaboration is operating since 2008 a large area water Cherenkov detector in the deep Mediterranean Sea, optimised for the detection of muons from high-energy astrophysical neutrinos. It is located at the coordinates 4248'N, 610'E (40 km off the coast of Toulon (Fr)).

ANTARES is composed of 12 lines of about 350m each, covering a surface area of 0.1 km2 : a first step toward the network of kilometric scale detectors KM3NeT, composed of ARCA (in Italy, dedicated to high energy neutrinos), and ORCA (in France, dedicated to low energy neutrinos).

(c) J. A. Aguilar (2010)

The observation of high energy neutrinos will open a new window on the universe. The primary aim of the experiment is to use neutrinos as a tool to study particle acceleration mechanisms in energetic astrophysical objects such as active galactic nuclei and gamma-ray bursts, which may also shed light on the origin of ultra-high-energy cosmic rays. At somewhat lower energies, non-baryonic dark matter (WIMPs) may be detected through the neutrinos produced when gravitationally captured WIMPs annihilate in the cores of the Earth and the Sun, and neutrino oscillations can be measured by studying distortions in the energy spectrum of upward-going atmospheric neutrinos.

You can choose one of these links, or start from the first link and browse page per page. Explanations about the images can be obtained when the mouse pointer is over it.

Picture : Antares and the Rho Ophiuchi Dark Cloud 
AAO image reference UKS 4 

Top left is NE. Image width is about 3.5 degrees
Anglo-Australian Observatory, Photograph from UK Schmidt plates by David Malin


Next : Why neutrino astronomy?

Author : Thierry Stolarczyk