The KM3NeT research infrastructure is under construction in the Mediterranean Sea. It consists of two water Cherenkov neutrino detectors, ARCA and ORCA, aimed at neutrino astrophysics and oscillation research, respectively. Instrumenting a large volume of sea water with ∼ 6200 optical modules comprising a total of ∼ 200 , 000 photomultiplier tubes, KM3NeT will achieve sensitivity to ∼10MeV neutrinos from Galactic and near-Galactic core-collapse supernovae through the observation of coincident hits in photomultipliers above the background. In this paper, the sensitivity of KM3NeT to a supernova explosion is estimated from detailed analyses of background data from the first KM3NeT detection units and simulations of the neutrino signal. The KM3NeT observational horizon (for a 5σ discovery) covers essentially the Milky-Way and for the most optimistic model, extends to the Small Magellanic Cloud (∼60kpc). Detailed studies of the time profile of the neutrino signal allow assessment of the KM3NeT capability to determine the arrival time of the neutrino burst with a few milliseconds precision for sources up to 5–8 kpc away, and detecting the peculiar signature of the standing accretion shock instability if the core-collapse supernova explosion happens closer than 3–5 kpc, depending on the progenitor mass. KM3NeT’s capability to measure the neutrino flux spectral parameters is also presented.

The KM3NeT potential for the next core-collapse supernova observation with neutrinos: KM3NeT Collaboration

Benfenati F.;Castaldi P.;Filippini F.;Illuminati G.;Levi G.;Margiotta A.;Spurio M.;Versari F.;
2021

Abstract

The KM3NeT research infrastructure is under construction in the Mediterranean Sea. It consists of two water Cherenkov neutrino detectors, ARCA and ORCA, aimed at neutrino astrophysics and oscillation research, respectively. Instrumenting a large volume of sea water with ∼ 6200 optical modules comprising a total of ∼ 200 , 000 photomultiplier tubes, KM3NeT will achieve sensitivity to ∼10MeV neutrinos from Galactic and near-Galactic core-collapse supernovae through the observation of coincident hits in photomultipliers above the background. In this paper, the sensitivity of KM3NeT to a supernova explosion is estimated from detailed analyses of background data from the first KM3NeT detection units and simulations of the neutrino signal. The KM3NeT observational horizon (for a 5σ discovery) covers essentially the Milky-Way and for the most optimistic model, extends to the Small Magellanic Cloud (∼60kpc). Detailed studies of the time profile of the neutrino signal allow assessment of the KM3NeT capability to determine the arrival time of the neutrino burst with a few milliseconds precision for sources up to 5–8 kpc away, and detecting the peculiar signature of the standing accretion shock instability if the core-collapse supernova explosion happens closer than 3–5 kpc, depending on the progenitor mass. KM3NeT’s capability to measure the neutrino flux spectral parameters is also presented.
Aiello S.; Albert A.; Garre S.A.; Aly Z.; Ambrosone A.; Ameli F.; Andre M.; Androulakis G.; Anghinolfi M.; Anguita M.; Anton G.; Ardid M.; Ardid S.; Aublin J.; Bagatelas C.; Baret B.; Pree S.B.; Bendahman M.; Benfenati F.; Berbee E.; Berg A.M.; Bertin V.; Biagi S.; Bissinger M.; Boettcher M.; Cabo M.B.; Boumaaza J.; Bouta M.; Bouwhuis M.; Bozza C.; Branzas H.; Bruijn R.; Brunner J.; Buis E.; Buompane R.; Busto J.; Caiffi B.; Calvo D.; Capone A.; Carretero V.; Castaldi P.; Celli S.; Chabab M.; Chau N.; Chen A.; 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.; Dallier R.; De Martino B.; De Palma M.; Di Marino M.; Di Palma I.; Diaz A.F.; Diego-Tortosa D.; Distefano C.; Domi A.; Donzaud C.; Dornic D.; Dorr M.; Drouhin D.; Eberl T.; Eddyamoui A.; van Eeden T.; van Eijk D.; El Bojaddaini I.; Elsaesser D.; Enzenhofer A.; Espinosa V.; Fermani P.; Ferrara G.; Filipovic M.D.; Filippini F.; Fusco L.A.; Gabella O.; Gal T.; Soto A.G.; Garufi F.; Gatelet Y.; Geisselbrecht N.; Gialanella L.; Giorgio E.; Gozzini S.R.; Gracia R.; Graf K.; Grasso D.; Grella G.; Guderian D.; Guidi C.; Haefner J.; Hamdaoui H.; van Haren H.; Heijboer A.; Hekalo A.; Hennig L.; Hernandez-Rey J.J.; Hofestadt J.; Huang F.; Ibnsalih W.I.; Illuminati G.; James C.W.; de Jong M.; de Jong P.; Jung B.J.; Kadler M.; Kalaczynski P.; Kalekin O.; Katz U.F.; Chowdhury N.R.K.; Kistauri G.; van der Knaap F.; Kooijman P.; Kouchner A.; Kreter M.; Kulikovskiy V.; Lahmann R.; Lamoureux M.; Larosa G.; Le Breton R.; Le Stum S.; Leonardi O.; Leone F.; Leonora E.; Lessing N.; Levi G.; Lincetto M.; Clark M.L.; Lipreau T.; Longhitano F.; Lopez-Coto D.; Maderer L.; Manczak J.; Mannheim K.; Margiotta A.; Marinelli A.; Markou C.; Martin L.; Martinez-Mora J.A.; Martini A.; Marzaioli F.; Mastroianni S.; Mazzou S.; Melis K.W.; Miele G.; 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.; Fearraigh B.O.; O'Sullivan M.; Organokov M.; Orlando A.; Gonzalez J.P.; Papalashvili G.; Papaleo R.; Passaro G.; Pastore C.; Paun A.M.; Pavalas G.E.; Pellegrino C.; Perrin-Terrin M.; Pestel V.; Piattelli P.; Pieterse C.; Pikounis K.; Pisanti O.; Poire C.; Popa V.; Pradier T.; Puhlhofer G.; Pulvirenti S.; Rabyang O.; Raffaelli F.; Randazzo N.; Razzaque S.; Real D.; Reck S.; Riccobene G.; Rivoire S.; Romanov A.; Rovelli A.; Greus F.S.; Samtleben D.F.E.; Losa A.S.; Sanguineti M.; Santangelo A.; Santonocito D.; Sapienza P.; Schnabel J.; Schneider M.F.; Schumann J.; Schutte H.M.; Seneca J.; Sgura I.; Shanidze R.; Sharma A.; Simeone F.; Sinopoulou A.; Spisso B.; Spurio M.; Stavropoulos D.; Stellacci S.M.; Taiuti M.; Tayalati Y.; Tenllado E.; Thakore T.; Thiersen H.; Tingay S.; Tsourapis V.; Tzamariudaki E.; Tzanetatos D.; Unbehaun T.; Van Elewyck V.; Vannoye G.; Vasileiadis G.; Versari F.; Viola S.; Vivolo D.; de Wasseige G.; Wilms J.; Wojaczynski R.; de Wolf E.; Zavatarelli S.; Zegarelli A.; Zito D.; Zornoza J.D.; Zuniga J.; Zywucka N.
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11585/835419
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