KM3NeT Core Collapse Supernovae observation program in standalone and multi-messenger modes

Coleiro, A.; Dornic, D.; Kulikovskiy, V.; Lincetto, M.; Molla, M. C.; Vannoye, G.; Ageron, M.; Aiello, S.; Albert, A.; Alshamsi, M.; Alves Garre, S.; Aly, Z.; Ambrosone, A.; Ameli, F.; Andre, M.; Androulakis, G.; Anghinolfi, M.; Anguita, M.; Anton, G.; Ardid, M.; Ardid, S.; Assal, W.; Aublin, J.; Bagatelas, C.; Baret, B.; du Pree, S. B.; Bendahman, M.; Benfenati, F.; Berbee, E.; van den Berg, A. M.; Bertin, V.; Beurthey, S.; van Beveren, V.; Biagi, S.; Billault, M.; Bissinger, M.; Boettcher, M.; Bou Cabo, M.; Boumaaza, J.; Bouta, M.; Boutonnet, C.; Bouvet, G.; Bouwhuis, M.; Bozza, C.; Branzas, H.; Bruijn, R.; Brunner, J.; Bruno, R.; Buis, E.; Buompane, R.; Busto, J.; Caiffi, B.; Caillat, L.; Calvo, D.; Campion, S.; Capone, A.; Carduner, H.; Carretero, V.; Castaldi, P.; Celli, S.; Cereseto, R.; Chabab, M.; Champion, C.; Chau, N.; Chen, A.; Cherubini, S.; Chiarella, V.; Chiarusi, T.; Circella, M.; Cocimano, R.; Coelho, J. A. B.; Coleiro, A.; Colomer Molla, M.; Colonges, S.; Coniglione, R.; Cosquer, A.; Coyle, P.; Cresta, M.; Creusot, A.; Cruz, A.; Cuttone, G.; D'Amico, A.; Dallier, R.; De Martino, B.; De Palma, 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.; Eljarrari, H.; Elsaesser, D.; Enzenhofer, A.; Espinosa, V.; Fermani, P.; Ferrara, G.; Filipovic, M. D.; Filippini, F.; Fransen, J.; Fusco, L. A.; Gajanana, D.; Gal, T.; Garcia Mendez, J.; Garcia Soto, A.; Garcon, E.; Garufi, F.; Gatius, C.; Geisselbrecht, N.; Gialanella, L.; Giorgio, E.; Gozzini, S. R.; Gracia, R.; Graf, K.; Grella, G.; Guderian, D.; Guidi, C.; Guillon, B.; Gutierrez, M.; Haefner, J.; Hallmann, S.; Hamdaoui, H.; van Haren, H.; Heijboer, A.; Hekalo, A.; Hennig, L.; Henry, S.; Hernandez-Rey, J. J.; Hofestadt, J.; Huang, F.; Idrissi Ibnsalih, W.; Ilioni, A.; Illuminati, G.; James, C. W.; Janezashvili, D.; Jansweijer, P.; de Jong, M.; de Jong, P.; Jung, B. J.; Kadler, M.; Kalaczynski, P.; Kalekin, O.; Katz, U. F.; Kayzel, F.; Keller, P.; Khan Chowdhury, N. R.; Kistauri, G.; van der Knaap, F.; Kooijman, P.; Kouchner, A.; Kreter, M.; Kulikovskiy, V.; Labalme, M.; Lagier, P.; Lahmann, R.; Lamare, P.; Lamoureux, M.; Larosa, G.; Lastoria, C.; Laurence, J.; Lazo, A.; Le Breton, R.; Le Guirriec, E.; Le Stum, S.; Lehaut, G.; Leonardi, O.; Leone, F.; Leonora, E.; Lerouvillois, C.; Lesrel, J.; Lessing, N.; Levi, G.; Lincetto, M.; Lindsey Clark, M.; Lipreau, T.; LLorens Alvarez, C.; Lonardo, A.; Longhitano, F.; Lopez-Coto, D.; Lumb, N.; Maderer, L.; Majumdar, J.; Manczak, J.; Margiotta, A.; Marinelli, A.; Marini, A.; Markou, C.; Martin, L.; Martinez-Mora, J. A.; Martini, A.; Marzaioli, F.; Mastroianni, S.; Melis, K. W.; Miele, G.; Migliozzi, P.; Migneco, E.; Mijakowski, P.; Miranda, L. S.; Mollo, C. M.; Mongelli, M.; Moussa, A.; Muller, R.; Musico, P.; Musumeci, M.; Nauta, L.; Navas, S.; Nicolau, C. A.; Nkosi, B.; Fearraigh, B. O.; O'Sullivan, M.; Orlando, A.; Ottonello, G.; Ottonello, S.; Palacios Gonzalez, J.; Papalashvili, G.; Papaleo, R.; Pastore, C.; Paun, A. M.; Pavalas, G. E.; Pellegrini, G.; Pellegrino, C.; Perrin-Terrin, M.; Pestel, V.; Piattelli, P.; Pieterse, C.; Pisanti, O.; Poire, C.; Popa, V.; Pradier, T.; Pratolongo, F.; Probst, I.; Puhlhofer, G.; Pulvirenti, S.; Quemener, G.; Randazzo, N.; Rapicavoli, A.; Razzaque, S.; Real, D.; Reck, S.; Riccobene, G.; Rigalleau, L.; Romanov, A.; Rovelli, A.; Royon, J.; Salesa Greus, F.; Samtleben, D. F. E.; Sanchez Losa, A.; Sanguineti, M.; Santangelo, A.; Santonocito, D.; Sapienza, P.; Schmelling, J.; Schnabel, J.; Schneider, M. F.; Schumann, J.; Schutte, H. M.; Seneca, J.; Sgura, I.; Shanidze, R.; Sharma, A.; Sinopoulou, A.; Spisso, B.; Spurio, M.; Stavropoulos, D.; Steijger, J.; Stellacci, S. M.; Taiuti, M.; Tatone, F.; Tayalati, Y.; Tenllado, E.; Tezier, D.; Thakore, T.; Theraube, S.; Thiersen, H.; Timmer, P.; Tingay, S.; Tsagkli, S.; Tsourapis, V.; Tzamariudaki, E.; Tzanetatos, D.; Valieri, C.; Van Elewyck, V.; Vasileiadis, G.; Versari, F.; Viola, S.; Vivolo, D.; de Wasseige, G.; Wilms, J.; Wojaczynski, R.; de Wolf, E.; Yousfi, T.; Zavatarelli, S.; Zegarelli, A.; Zito, D.; Zornoza, J. D.; Zuniga, J.; Zywucka, N.

The KM3NeT research infrastructure in the Mediterranean is a multi-purpose cubic-kilometre neutrino observatory consisting of two detectors optimised to study cosmic and atmospheric neutrinos between GeV to PeV energies. Additionally, KM3NeT multi-photomultiplier optical modules allow the detection of interaction products from neutrinos with energies of a few MeV by selecting nanosecond coincidences within the photomultipliers of the same module. The distribution of the number of photomultipliers forming a coincidence (multiplicity) for the duration of the supernova emission is used as a proxy of the average neutrino energy. Using an optimised coincidence selection the KM3NeT detectors will be sensitive to supernovae in our Galaxy and beyond. A high number of detected events from a core collapse supernova explosion is expected in KM3NeT thanks to its large effective volume. The measurement of the neutrino light curve properties, such as the light curve start time and the presence of the standing accretion shock instability oscillations is possible with such statistics. Sub-millisecond time synchronisation between KM3NeT detectors allows joint observation. Such a scheme can be also a viable solution to synchronise the KM3NeT telescopes with other detectors aiming to observe neutrino emission from core collapse supernovae through the SNEWS network.

KM3NeT Core Collapse Supernovae observation program in standalone and multi-messenger modes

Coleiro A.;Dornic D.;Kulikovskiy V.;Lincetto M.;Molla M. C.;Vannoye G.;Ageron M.;Aiello S.;Albert A.;Alshamsi M.;Alves Garre S.;Aly Z.;Ambrosone A.;Ameli F.;Andre M.;Androulakis G.;Anghinolfi M.;Anguita M.;Anton G.;Ardid M.;Ardid S.;Assal W.;Aublin J.;Bagatelas C.;Baret B.;du Pree S. B.;Bendahman M.;Benfenati F.;Berbee E.;van den Berg A. M.;Bertin V.;Beurthey S.;van Beveren V.;Biagi S.;Billault M.;Bissinger M.;Boettcher M.;Bou Cabo M.;Boumaaza J.;Bouta M.;Boutonnet C.;Bouvet G.;Bouwhuis M.;Bozza C.;Branzas H.;Bruijn R.;Brunner J.;Bruno R.;Buis E.;Buompane R.;Busto J.;Caiffi B.;Caillat L.;Calvo D.;Campion S.;Capone A.;Carduner H.;Carretero V.;Castaldi P.;Celli S.;Cereseto R.;Chabab M.;Champion C.;Chau N.;Chen A.;Cherubini S.;Chiarella V.;Chiarusi T.;Circella M.;Cocimano R.;Coelho J. A. B.;Coleiro A.;Colomer Molla M.;Colonges S.;Coniglione R.;Cosquer A.;Coyle P.;Cresta M.;Creusot A.;Cruz A.;Cuttone G.;D'Amico A.;Dallier R.;De Martino B.;De Palma 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.;Eljarrari H.;Elsaesser D.;Enzenhofer A.;Espinosa V.;Fermani P.;Ferrara G.;Filipovic M. D.;Filippini F.;Fransen J.;Fusco L. A.;Gajanana D.;Gal T.;Garcia Mendez J.;Garcia Soto A.;Garcon E.;Garufi F.;Gatius C.;Geisselbrecht N.;Gialanella L.;Giorgio E.;Gozzini S. R.;Gracia R.;Graf K.;Grella G.;Guderian D.;Guidi C.;Guillon B.;Gutierrez M.;Haefner J.;Hallmann S.;Hamdaoui H.;van Haren H.;Heijboer A.;Hekalo A.;Hennig L.;Henry S.;Hernandez-Rey J. J.;Hofestadt J.;Huang F.;Idrissi Ibnsalih W.;Ilioni A.;Illuminati G.;James C. W.;Janezashvili D.;Jansweijer P.;de Jong M.;de Jong P.;Jung B. J.;Kadler M.;Kalaczynski P.;Kalekin O.;Katz U. F.;Kayzel F.;Keller P.;Khan Chowdhury N. R.;Kistauri G.;van der Knaap F.;Kooijman P.;Kouchner A.;Kreter M.;Kulikovskiy V.;Labalme M.;Lagier P.;Lahmann R.;Lamare P.;Lamoureux M.;Larosa G.;Lastoria C.;Laurence J.;Lazo A.;Le Breton R.;Le Guirriec E.;Le Stum S.;Lehaut G.;Leonardi O.;Leone F.;Leonora E.;Lerouvillois C.;Lesrel J.;Lessing N.;Levi G.;Lincetto M.;Lindsey Clark M.;Lipreau T.;LLorens Alvarez C.;Lonardo A.;Longhitano F.;Lopez-Coto D.;Lumb N.;Maderer L.;Majumdar J.;Manczak J.;Margiotta A.;Marinelli A.;Marini A.;Markou C.;Martin L.;Martinez-Mora J. A.;Martini A.;Marzaioli F.;Mastroianni S.;Melis K. W.;Miele G.;Migliozzi P.;Migneco E.;Mijakowski P.;Miranda L. S.;Mollo C. M.;Mongelli M.;Moussa A.;Muller R.;Musico P.;Musumeci M.;Nauta L.;Navas S.;Nicolau C. A.;Nkosi B.;Fearraigh B. O.;O'Sullivan M.;Orlando A.;Ottonello G.;Ottonello S.;Palacios Gonzalez J.;Papalashvili G.;Papaleo R.;Pastore C.;Paun A. M.;Pavalas G. E.;Pellegrini G.;Pellegrino C.;Perrin-Terrin M.;Pestel V.;Piattelli P.;Pieterse C.;Pisanti O.;Poire C.;Popa V.;Pradier T.;Pratolongo F.;Probst I.;Puhlhofer G.;Pulvirenti S.;Quemener G.;Randazzo N.;Rapicavoli A.;Razzaque S.;Real D.;Reck S.;Riccobene G.;Rigalleau L.;Romanov A.;Rovelli A.;Royon J.;Salesa Greus F.;Samtleben D. F. E.;Sanchez Losa A.;Sanguineti M.;Santangelo A.;Santonocito D.;Sapienza P.;Schmelling J.;Schnabel J.;Schneider M. F.;Schumann J.;Schutte H. M.;Seneca J.;Sgura I.;Shanidze R.;Sharma A.;Sinopoulou A.;Spisso B.;Spurio M.;Stavropoulos D.;Steijger J.;Stellacci S. M.;Taiuti M.;Tatone F.;Tayalati Y.;Tenllado E.;Tezier D.;Thakore T.;Theraube S.;Thiersen H.;Timmer P.;Tingay S.;Tsagkli S.;Tsourapis V.;Tzamariudaki E.;Tzanetatos D.;Valieri C.;Van Elewyck V.;Vasileiadis G.;Versari F.;Viola S.;Vivolo D.;de Wasseige G.;Wilms J.;Wojaczynski R.;de Wolf E.;Yousfi T.;Zavatarelli S.;Zegarelli A.;Zito D.;Zornoza J. D.;Zuniga J.;Zywucka N.

2022

Abstract

The KM3NeT research infrastructure in the Mediterranean is a multi-purpose cubic-kilometre neutrino observatory consisting of two detectors optimised to study cosmic and atmospheric neutrinos between GeV to PeV energies. Additionally, KM3NeT multi-photomultiplier optical modules allow the detection of interaction products from neutrinos with energies of a few MeV by selecting nanosecond coincidences within the photomultipliers of the same module. The distribution of the number of photomultipliers forming a coincidence (multiplicity) for the duration of the supernova emission is used as a proxy of the average neutrino energy. Using an optimised coincidence selection the KM3NeT detectors will be sensitive to supernovae in our Galaxy and beyond. A high number of detected events from a core collapse supernova explosion is expected in KM3NeT thanks to its large effective volume. The measurement of the neutrino light curve properties, such as the light curve start time and the presence of the standing accretion shock instability oscillations is possible with such statistics. Sub-millisecond time synchronisation between KM3NeT detectors allows joint observation. Such a scheme can be also a viable solution to synchronise the KM3NeT telescopes with other detectors aiming to observe neutrino emission from core collapse supernovae through the SNEWS network.