%0 Journal Article
%T Sensitivity of the KM3NeT/ARCA neutrino telescope to point-like neutrino sources
%A KM3NeT Collaboration (Aiello, S. et al
%A Barrios-Marti, J.
%A Calvo, D.
%A Coleiro, A.
%A Colomer, M.
%A Gozzini, S. R.
%A Hernandez-Rey, J. J.
%A Illuminati, G.
%A Khan Chowdhury, N. R.
%A Lotze, M.
%A Real, D.
%A Thakore, T.
%A Zornoza, J. D.
%A Zuñiga, J.
%J Astroparticle Physics
%D 2019
%V 111
%I Elsevier Science Bv
%@ 0927-6505
%G English
%F KM3NeTCollaborationAiello_etal2019
%O WOS:000470047300008
%O exported from refbase (https://references.ific.uv.es/refbase/show.php?record=4047), last updated on Wed, 02 Oct 2019 07:04:17 +0000
%X KM3NeT will be a network of deep-sea neutrino telescopes in the Mediterranean Sea. The KM3NeT/ARCA detector, to be installed at the Capo Passero site (Italy), is optimised for the detection of high-energy neutrinos of cosmic origin. Thanks to its geographical location on the Northern hemisphere, KM3NeT/ARCA can observe upgoing neutrinos from most of the Galactic Plane, including the Galactic Centre. Given its effective area and excellent pointing resolution, KM3NeT/ARCA will measure or significantly constrain the neutrino flux from potential astrophysical neutrino sources. At the same time, it will test flux predictions based on gamma-ray measurements and the assumption that the gamma-ray flux is of hadronic origin. Assuming this scenario, discovery potentials and sensitivities for a selected list of Galactic sources and to generic point sources with an E(-2 )spectrum are presented. These spectra are assumed to be time independent. The results indicate that an observation with 3 sigma significance is possible in about six years of operation for the most intense sources, such as Supernovae Remnants RX J1713.7-3946 and Vela Jr. If no signal will be found during this time, the fraction of the gamma-ray flux coming from hadronic processes can be constrained to be below 50% for these two objects.
%K Astrophysical neutrino sources
%K Cherenkov underwater neutrino telescope
%K KM3NeT
%R 10.1016/j.astropartphys.2019.04.002
%U https://arxiv.org/abs/1810.08499
%U https://doi.org/10.1016/j.astropartphys.2019.04.002
%P 100-110