TY  - JOUR
AU  - KM3NeT Collaboration (Aiello, S. et al
AU  - Barrios-Marti, J.
AU  - Calvo, D.
AU  - Coleiro, A.
AU  - Colomer, M.
AU  - Gozzini, S. R.
AU  - Hernandez-Rey, J. J.
AU  - Illuminati, G.
AU  - Khan Chowdhury, N. R.
AU  - Lotze, M.
AU  - Real, D.
AU  - Thakore, T.
AU  - Zornoza, J. D.
AU  - Zuñiga, J.
PY  - 2019
DA  - 2019//
TI  - Sensitivity of the KM3NeT/ARCA neutrino telescope to point-like neutrino sources
T2  - Astropart Phys.
JO  - Astroparticle Physics
SP  - 100
EP  - 110
VL  - 111
PB  - Elsevier Science Bv
KW  - Astrophysical neutrino sources
KW  - Cherenkov underwater neutrino telescope
KW  - KM3NeT
AB  - 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.
SN  - 0927-6505
UR  - https://arxiv.org/abs/1810.08499
UR  - https://doi.org/10.1016/j.astropartphys.2019.04.002
DO  - 10.1016/j.astropartphys.2019.04.002
LA  - English
N1  - WOS:000470047300008
ID  - KM3NeTCollaborationAiello_etal2019
ER  -