Expectations for the high-energy neutrino detection from starburst galaxies with KM3NeT/ARCA

Ibnsalih, W. I.; Ambrosone, A.; Marinelli, A.; Miele, G.; Migliozzi, P.; Pisanti, O.; Sharma, A.; 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.; Basegmez du Pree, S.; 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.

Star-forming galaxies (SFGs) and starburst galaxies (SBGs) are extragalactic sources which could produce high-energy neutrinos. In principle, they could play a rather important role for explaining at least a sizeable part of IceCube’s observations of astophysical neutrino. Using a recent theoretical model which implemented a blending of spectral indeces, we present the KM3NeT/ARCA sensitivities for such a diffuse flux from the startburst galaxies. In particular, we provide the 5-year differential sensitivity for the two building blocks of ARCA. We make use only of the track-like events in the range of 100 GeV - 10 PeV differentiate in 11 bins of energy. We show how the upcoming neutrino telescope could observe the diffuse SFG and SBG within 5 years of data taking. We found the minimum of the sensitivity at around 100 TeV, which is also the energy where the SBG contribution is expected to peak. This would not only constrain the multi-component fit of the observed astrophysical neutrino flux at that energy (100 TeV), but would also provide us a direct link between the star-forming activity in the reservoir environments and the hadronic emissions.

Expectations for the high-energy neutrino detection from starburst galaxies with KM3NeT/ARCA

Ibnsalih W. I.;Ambrosone A.;Marinelli A.;Miele G.;Migliozzi P.;Pisanti O.;Sharma A.;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.;Basegmez du Pree S.;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

Star-forming galaxies (SFGs) and starburst galaxies (SBGs) are extragalactic sources which could produce high-energy neutrinos. In principle, they could play a rather important role for explaining at least a sizeable part of IceCube’s observations of astophysical neutrino. Using a recent theoretical model which implemented a blending of spectral indeces, we present the KM3NeT/ARCA sensitivities for such a diffuse flux from the startburst galaxies. In particular, we provide the 5-year differential sensitivity for the two building blocks of ARCA. We make use only of the track-like events in the range of 100 GeV - 10 PeV differentiate in 11 bins of energy. We show how the upcoming neutrino telescope could observe the diffuse SFG and SBG within 5 years of data taking. We found the minimum of the sensitivity at around 100 TeV, which is also the energy where the SBG contribution is expected to peak. This would not only constrain the multi-component fit of the observed astrophysical neutrino flux at that energy (100 TeV), but would also provide us a direct link between the star-forming activity in the reservoir environments and the hadronic emissions.