@Article{KM3NeTCollaborationAiello_etal2019,
author="KM3NeT Collaboration (Aiello, S. et al
and Barrios-Marti, J.
and Calvo, D.
and Coleiro, A.
and Colomer, M.
and Gozzini, S. R.
and Hernandez-Rey, J. J.
and Illuminati, G.
and Khan Chowdhury, N. R.
and Lotze, M.
and Real, D.
and Thakore, T.
and Zornoza, J. D.
and Zu{\~{n}}iga, J.",
title="Sensitivity of the KM3NeT/ARCA neutrino telescope to point-like neutrino sources",
journal="Astroparticle Physics",
year="2019",
publisher="Elsevier Science Bv",
volume="111",
pages="100--110",
optkeywords="Astrophysical neutrino sources; Cherenkov underwater neutrino telescope; KM3NeT",
abstract="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.",
optnote="WOS:000470047300008",
optnote="exported from refbase (https://references.ific.uv.es/refbase/show.php?record=4047), last updated on Wed, 02 Oct 2019 07:04:17 +0000",
issn="0927-6505",
doi="10.1016/j.astropartphys.2019.04.002",
opturl="https://arxiv.org/abs/1810.08499",
opturl="https://doi.org/10.1016/j.astropartphys.2019.04.002",
language="English"
}