Aiello S, Domi A, Albert A, Garre SA, 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 SBd, Bendahman M, Benfenati F, Berbee E, Berg AMd, Bertin V, Biagi S, Bissinger M, Boettcher M, Cabo MB, Boumaaza J, Bouta M, Bouwhuis M, Bozza C, Brânzaş 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 JA, Coleiro A, Molla MC, Coniglione R, Coyle P, Creusot A, Cuttone G, Dallier R, De Martino B, De Palma M, Di Marino M, Di Palma I, Díaz AF, Diego-Tortosa D, Distefano C, Domi A, Donzaud C, Dornic D, Dörr M, Drouhin D, Eberl T, Eddyamoui A, van Eeden T, van Eijk D, El Bojaddaini I, Elsaesser D, Enzenhöfer A, Espinosa V, Fermani P, Ferrara G, Filipović MD, Filippini F, Fusco LA, Gabella O, Gál T, Soto AG, Garufi F, Gatelet Y, Geißelbrecht N, Gialanella L, Giorgio E, Gozzini SR, 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, Hernández-Rey JJ, Hofestädt J, Huang F, Ibnsalih WI, Illuminati G, James CW, de Jong M, de Jong P, Jung BJ, Kadler M, Kalaczyński P, Kalekin O, Katz U, Chowdhury NR, 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 ML, Lipreau T, Longhitano F, Lopez-Coto D, Maderer L, Mańczak J, Mannheim K, Margiotta A, Marinelli A, Markou C, Martin L, Martínez-Mora JA, Martini A, Marzaioli F, Mastroianni S, Mazzou S, Melis KW, Miele G, 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, Fearraigh B, O’Sullivan M, Organokov M, Orlando A, González JP, Papalashvili G, Papaleo R, Passaro G, Pastore C, Păun AM, Păvălaş GE, Pellegrino C, Perrin-Terrin M, Pestel V, Piattelli P, Pieterse C, Pikounis K, Pisanti O, Poirè C, Popa V, Pradier T, Pühlhofer G, Pulvirenti S, Rabyang O, Raffaelli F, Randazzo N, Razzaque S, Real D, Reck S, Riccobene G, Rivoire S, Romanov A, Rovelli A, Greus FS, Samtleben DF, Losa AS, Sanguineti M, Santangelo A, Santonocito D, Sapienza P, Schnabel J, Schneider MF, Schumann J, Schutte HM, Seneca J, Sgura I, Shanidze R, Sharma A, Simeone F, Sinopoulou A, Spisso B, Spurio M, Stavropoulos D, Stellacci SM, 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, Wojaczyński R, de Wolf E, Zavatarelli S, Zegarelli A, Zito D, Zornoza JD, Zúñiga J, Zywucka N (2021)
Publication Type: Journal article
Publication year: 2021
Book Volume: 81
Article Number: 445
Journal Issue: 5
DOI: 10.1140/epjc/s10052-021-09187-5
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.
APA:
Aiello, S., Domi, A., Albert, A., Garre, S.A., Aly, Z., Ambrosone, A.,... Zywucka, N. (2021). The KM3NeT potential for the next core-collapse supernova observation with neutrinos: KM3NeT Collaboration. European Physical Journal C: Particles and Fields, 81(5). https://doi.org/10.1140/epjc/s10052-021-09187-5
MLA:
Aiello, S., et al. "The KM3NeT potential for the next core-collapse supernova observation with neutrinos: KM3NeT Collaboration." European Physical Journal C: Particles and Fields 81.5 (2021).
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