Sensitivity of the KM3NeT/ARCA neutrino telescope to point-like neutrino sources

Aiello, S; Akrame, Se; Ameli, F; Anassontzis, Eg; Andre, M; Androulakis, G; Anghinolfi, M; Anton, G; Ardid, M; Aublin, J; Avgitas, T; Bagatelas, C; Barbarino, G; Baret, B; Barrios-Marti, J; Belias, A; Berbee, E; Van Den Berg, A; Bertin, V; Biagi, S; Biagioni, A; Biernoth, C; Boumaaza, J; Bourret, S; Bouta, M; Bouwhuis, M; Bozza, C; Branzas, H; Bruchner, M; Bruijn, R; Brunner, J; Buis, E; Buompane, R; Busto, J; Calvo, D; Capone, A; Celli, S; Chabab, M; Chau, N; Cherubini, S; Chiarella, V; Chiarusi, T; Circella, M; Cocimano, R; Jab, Coelho; Coleiro, A; Molla, Mc; Coniglione, R; Coyle, P; Creusot, A; Cuttone, G; D'Onofrio, A; Dallier, R; De Sio, C; Di Palma, I; Diaz, Af; Diego-Tortosa, D; Distefano, C; Domi, A; Dona, R; Donzaud, C; Dornic, D; Dorr, M; Durocher, M; Eberl, T; Van Eijk, D; El Bojaddaini, I; Eljarrari, H; Elsaesser, D; Enzenhofer, A; Fermani, P; Ferrara, G; Filipovic, Md; Fusco, La; Gal, T; Garcia, A; Garufi, F; Gialanella, L; Giorgio, E; Giuliante, A; Gozzini, Sr; Gracia, R; Graf, K; Grasso, D; Gregoire, T; Grella, G; Hallmann, S; Hamdaoui, H; Van Haren, H; Heid, T; Heijboer, A; Hekalo, A; Hernandez-Rey, Jj; Hofestadt, J; Illuminati, G; James, Cw; Jongen, M; De Jong, M; De Jong, P; Kadler, M; Kalaczynski, P; Kalekin, O; Katz, Uf; Nrk, Chowdhury; Kiessling, D; Koffeman, En; Kooijman, P; Kouchner, A; Kreter, M; Kulikovskiy, V; Kannichankandy, Mk; Lahmann, R; Larosa, G; Le Breton, R; Leone, F; Leonora, E; Levi, G; Lincetto, M; Lonardo, A; Longhitano, F; Coto, Dl; Lotze, M; Maderer, L; Maggi, G; Manczak, J; Mannheim, K; Margiotta, A; Marinelli, A; Markou, C; Martin, L; Martinez-Mora, Ja; Martini, A; Marzaioli, F; Mele, R; Melis, Kw; Migliozzi, P; Migneco, E; Mijakowski, P; Miranda, Ls; Mollo, Cm; Morganti, M; Moser, M; Moussa, A; Muller, R; Musumeci, M; Nauta, L; Navas, S; Nicolau, Ca; Nielsen, C; Fearraigh, Bo; Organokov, M; Orlando, A; Ottonello, S; Panagopoulos, V; Papalashvili, G; Papaleo, R; Pavalas, Ge; Pellegrino, C; Perrin-Terrin, M; Piattelli, P; Pikounis, K; Pisanti, O; Poire, C; Polydefki, G; Popa, V; Post, M; Pradier, T; Puhlhofer, G; Pulvirenti, S; Quinn, L; Raffaelli, F; Randazzo, N; Razzaque, S; Real, D; Resvanis, L; Reubelt, J; Riccobene, G; Richer, M; Rigalleau, L; Rovelli, A; Saffer, M; Salvadori, I; Dfe, Samtleben; Losa, As; Sanguineti, M; Santangelo, A; Santonocito, D; Sapienza, P; Schumann, J; Sciacca, V; Seneca, J; Sgura, I; Shanidze, R; Sharma, A; Simeone, F; Sinopoulou, A; Spisso, B; Spurio, M; Stavropoulos, D; Steijger, J; Stellacci, Sm; Strandberg, B; Stransky, D; Stuven, T; Taiuti, M; Tatone, F; Tayalati, Y; Tenllado, E; Thakore, T; Trovato, A; Tzamariudaki, E; Tzanetatos, D; Van Elewyck, V; Versari, F; Viola, S; Vivolo, D; Wilms, J; De Wolf, E; Zaborov, D; Zornoza, Jd; Zuniga, J

doi:10.1016/j.astropartphys.2019.04.002

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. (C) 2019 The Authors. Published by Elsevier B.V.

Sensitivity of the KM3NeT/ARCA neutrino telescope to point-like neutrino sources / Aiello, S; Akrame, Se; Ameli, F; Anassontzis, Eg; Andre, M; Androulakis, G; Anghinolfi, M; Anton, G; Ardid, M; Aublin, J; Avgitas, T; Bagatelas, C; Barbarino, G; Baret, B; Barrios-Marti, J; Belias, A; Berbee, E; van den Berg, A; Bertin, V; Biagi, S; Biagioni, A; Biernoth, C; Boumaaza, J; Bourret, S; Bouta, M; Bouwhuis, M; Bozza, C; Branzas, H; Bruchner, M; Bruijn, R; Brunner, J; Buis, E; Buompane, R; Busto, J; Calvo, D; Capone, A; Celli, S; Chabab, M; Chau, N; Cherubini, S; Chiarella, V; Chiarusi, T; Circella, M; Cocimano, R; Coelho, Jab; Coleiro, A; Molla, Mc; Coniglione, R; Coyle, P; Creusot, A; Cuttone, G; D'Onofrio, A; Dallier, R; De Sio, C; Di Palma, I; Diaz, Af; Diego-Tortosa, D; Distefano, C; Domi, A; Dona, R; Donzaud, C; Dornic, D; Dorr, M; Durocher, M; Eberl, T; van Eijk, D; El Bojaddaini, I; Eljarrari, H; Elsaesser, D; Enzenhofer, A; Fermani, P; Ferrara, G; Filipovic, Md; Fusco, La; Gal, T; Garcia, A; Garufi, F; Gialanella, L; Giorgio, E; Giuliante, A; Gozzini, Sr; Gracia, R; Graf, K; Grasso, D; Gregoire, T; Grella, G; Hallmann, S; Hamdaoui, H; van Haren, H; Heid, T; Heijboer, A; Hekalo, A; Hernandez-Rey, Jj; Hofestadt, J; Illuminati, G; James, Cw; Jongen, M; de Jong, M; de Jong, P; Kadler, M; Kalaczynski, P; Kalekin, O; Katz, Uf; Chowdhury, Nrk; Kiessling, D; Koffeman, En; Kooijman, P; Kouchner, A; Kreter, M; Kulikovskiy, V; Kannichankandy, Mk; Lahmann, R; Larosa, G; Le Breton, R; Leone, F; Leonora, E; Levi, G; Lincetto, M; Lonardo, A; Longhitano, F; Coto, Dl; Lotze, M; Maderer, L; Maggi, G; Manczak, J; Mannheim, K; Margiotta, A; Marinelli, A; Markou, C; Martin, L; Martinez-Mora, Ja; Martini, A; Marzaioli, F; Mele, R; Melis, Kw; Migliozzi, P; Migneco, E; Mijakowski, P; Miranda, Ls; Mollo, Cm; Morganti, M; Moser, M; Moussa, A; Muller, R; Musumeci, M; Nauta, L; Navas, S; Nicolau, Ca; Nielsen, C; Fearraigh, Bo; Organokov, M; Orlando, A; Ottonello, S; Panagopoulos, V; Papalashvili, G; Papaleo, R; Pavalas, Ge; Pellegrino, C; Perrin-Terrin, M; Piattelli, P; Pikounis, K; Pisanti, O; Poire, C; Polydefki, G; Popa, V; Post, M; Pradier, T; Puhlhofer, G; Pulvirenti, S; Quinn, L; Raffaelli, F; Randazzo, N; Razzaque, S; Real, D; Resvanis, L; Reubelt, J; Riccobene, G; Richer, M; Rigalleau, L; Rovelli, A; Saffer, M; Salvadori, I; Samtleben, Dfe; Losa, As; Sanguineti, M; Santangelo, A; Santonocito, D; Sapienza, P; Schumann, J; Sciacca, V; Seneca, J; Sgura, I; Shanidze, R; Sharma, A; Simeone, F; Sinopoulou, A; Spisso, B; Spurio, M; Stavropoulos, D; Steijger, J; Stellacci, Sm; Strandberg, B; Stransky, D; Stuven, T; Taiuti, M; Tatone, F; Tayalati, Y; Tenllado, E; Thakore, T; Trovato, A; Tzamariudaki, E; Tzanetatos, D; Van Elewyck, V; Versari, F; Viola, S; Vivolo, D; Wilms, J; de Wolf, E; Zaborov, D; Zornoza, Jd; Zuniga, J. - In: ASTROPARTICLE PHYSICS. - ISSN 0927-6505. - 111:(2019), pp. 100-110. [10.1016/j.astropartphys.2019.04.002]