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

[EN] 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 highenergy neutrinos of cosmic origin. Thanks to its geographical location on the Northern hemisphere,...

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Detalles Bibliográficos
Autores: Aiello, S., Akrame, S. E., Ameli, F., Anassontzis, E. G., Andre, M., Androulakis, G., Anghinolfi, M., Anton, G., Aublin, J., Avgitas, T., Bagatelas, C., Barbarino, G., Baret, B., Barrios-Marti, J., Diego-Tortosa, D., Martínez Mora, Juan Antonio, Poirè, Chiara, Ardid, Miguel|||0000-0002-3199-594X
Tipo de recurso: artículo
Fecha de publicación:2019
País:España
Institución:Universitat Politècnica de València (UPV)
Repositorio:RiuNet. Repositorio Institucional de la Universitat Politécnica de Valéncia
Idioma:inglés
OAI Identifier:oai:riunet.upv.es:10251/154099
Acceso en línea:https://riunet.upv.es/handle/10251/154099
Access Level:acceso abierto
Palabra clave:Astrophysical neutrino sources
Cherenkov underwater neutrino telescope
KM3NeT
FISICA APLICADA
Descripción
Sumario:[EN] 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 highenergy 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 inde- pendent. The results indicate that an observation with 3 ¿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.

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