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

Aiello, S.; Akrame, S. E.; Ameli, F.; G. Anassontzis E.,; 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, J. A. B.; Coleiro, A.; Molla, M. C.; Coniglione, R.; Coyle, P.; Creusot, A.; Cuttone, G.; D'Onofrio, A.; Dallier, R.; De Sio, C.; Di Palma, I.; Diaz, A. F.; 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.; D. Filipovic M.,; Fusco, L. A.; Gal, T.; Garcia, A.; Garufi, F.; Gialanella, L.; Giorgio, E.; Giuliante, A.; Gozzini, S. R.; 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, J. J.; Hofestadt, J.; Illuminati, G.; James, C. W.; Jongen, M.; de Jong, M.; de Jong, P.; Kadler, M.; Kalaczynski, P.; Kalekin, O.; Katz, U. F.; Khan Chowdhury, N. R.; Kiessling, D.; Koffeman, E. N.; Kooijman, P.; Kouchner, A.; Kreter, M.; Kulikovskiy, V.; Kunhikannan Kannichankandy, M.; Lahmann, R.; Larosa, G.; Le Breton, R.; Leone, F.; Leonora, E.; Levi, G.; Lincetto, M.; Lonardo, A.; Longhitano, F.; Lopez Coto, D.; Lotze, M.; Maderer, L.; Maggi, G.; Manczak, J.; Mannheim, K.; Margiotta, A.; Marinelli, A.; Markou, C.; Martin, L.; Martinez-Mora, J. A.; Martini, A.; Marzaioli, F.; Mele, R.; Melis, K. W.; Migliozzi, P.; Migneco, E.; Mijakowski, P.; Miranda, L. S.; Mollo, C. M.; Morganti, M.; Moser, M.; Moussa, A.; Muller, R.; Musumeci, M.; Nauta, L.; Navas, S.; Nicolau, C. A.; Nielsen, C.; O Fearraigh, B.; Organokov, M.; Orlando, A.; Ottonello, S.; Panagopoulos, V.; Papalashvili, G.; Papaleo, R.; Pavalas, G. E.; 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, D. F. E.; Sanchez Losa, A.; 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, S. M.; 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, J. D.; 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 S. E.;Ameli F.;G. Anassontzis E.;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 J. A. B.;Coleiro A.;Molla M. C.;Coniglione R.;Coyle P.;Creusot A.;Cuttone G.;D'Onofrio A.;Dallier R.;De Sio C.;Di Palma I.;Diaz A. F.;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.;D. Filipovic M.;Fusco L. A.;Gal T.;Garcia A.;Garufi F.;Gialanella L.;Giorgio E.;Giuliante A.;Gozzini S. R.;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 J. J.;Hofestadt J.;Illuminati G.;James C. W.;Jongen M.;de Jong M.;de Jong P.;Kadler M.;Kalaczynski P.;Kalekin O.;Katz U. F.;Khan Chowdhury N. R.;Kiessling D.;Koffeman E. N.;Kooijman P.;Kouchner A.;Kreter M.;Kulikovskiy V.;Kunhikannan Kannichankandy M.;Lahmann R.;Larosa G.;Le Breton R.;Leone F.;Leonora E.;Levi G.;Lincetto M.;Lonardo A.;Longhitano F.;Lopez Coto D.;Lotze M.;Maderer L.;Maggi G.;Manczak J.;Mannheim K.;Margiotta A.;Marinelli A.;Markou C.;Martin L.;Martinez-Mora J. A.;Martini A.;Marzaioli F.;Mele R.;Melis K. W.;Migliozzi P.;Migneco E.;Mijakowski P.;Miranda L. S.;Mollo C. M.;Morganti M.;Moser M.;Moussa A.;Muller R.;Musumeci M.;Nauta L.;Navas S.;Nicolau C. A.;Nielsen C.;O Fearraigh B.;Organokov M.;Orlando A.;Ottonello S.;Panagopoulos V.;Papalashvili G.;Papaleo R.;Pavalas G. E.;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 D. F. E.;Sanchez Losa A.;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 S. M.;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 J. D.;Zuniga J.

2019-01-01

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