arXiv : Sensitivity of future liquid argon dark matter search experiments to core-collapse supernova neutrinos

Agnes, P.; Kim, S.; Arcelli, S.; Pegoraro, P.A.; Nowak, J.; Martínez, M.; Ye, Z.; Cocco, V.; Batignani, G.; Leyton, M.; Viant, T.; Musenich, L.; Dellacasa, G.; Caminata, A.; Tricomi, A.; Steri, A.; Mclaughlin, J.; Viel, S.; De Gruttola, D.; Pira, C.; Machulin, I.N.; Gromov, M.; Garbini, M.; Erjavec, T.; Pagani, L.; Moggi, A.; Guerzoni, M.; McDonald, A.B.; Nessi, M.; Cifarelli, L.; Ghiano, C.; Napolitano, T.; Goicoechea Casanueva, V.; Scioli, G.; Castello, P.; Moioli, S.; Buccino, G.; Hill, S.; Gendotti, A.; Vishneva, A.; Chyhyrynets, E.; Vogelaar, R.B.; Morisi, S.; Zuzel, G.; Zani, A.; Cárdenas-Montes, M.; Khomyakov, A.V.; Rignanese, L.P.; James, C.C.; Davini, S.; Meyers, P.D.; Retiere, F.; Covone, G.; Jillings, C.; Sánchez García, E.; Wojcik, Ma.M.; Albergo, S.; Fiorillo, G.; Di Stefano, P.; Skensved, P.; Szelc, A.M.; Gola, A.; Czudak, P.; Frolov, E.; Wang, H.; Kish, A.; Bonivento, W.M.; Fernandez Diaz, M.; Gulino, M.; Masoni, A.; Cintas, D.; Daniel, M.; Chepurnov, A.; Buzulutskov, A.; Ripoli, C.; Torres-Lara, S.; Kochanek, I.; Mazzi, A.; Corning, J.; Kugathasan, R.; Simeone, M.; Barbarian, V.; Cavalcante, P.; Derbin, A.V.; Consiglio, L.; Hackett, B.R.; Yang, C.; Barrado Olmedo, A.; Lissia, M.; Longo, G.; Di Noto, L.; Santorelli, R.; Shaw, B.; Della Valle, M.; Semenov, D.A.; Sanfilippo, S.; Hubaut, F.; Pelczar, K.; Scapparone, E.; Boulay, M.G.; Dionisi, C.; Alici, A.; Schlitzer, B.; Nikulin, I.; Messina, A.; Cappello, G.; Martinez Rojas, A.D.; Copello, S.; Paternoster, G.; Chashin, S.; De Cecco, S.; Devoto, A.; Lidey, L.; Stringer, M.; Musico, P.; Kendziora, C.L.; Romero, L.; Smirnov, O.; Suvorov, Y.; Azzolini, O.; Maricic, J.; Avetisov, R.I.; Pralavorio, P.; Smith, B.; Dordei, F.; Hungerford, E.V.; D'Auria, S.; Moharana, A.; Borisova, E.; Haranczyk, M.; Cadeddu, M.; Ippolito, V.; Franco, D.; Avetissov, I.Ch.; Pellegrino, C.; Giorgi, M.A.; Pandola, L.; Keppel, G.; Kemp, A.A.; Perotti, F.; De Pasquale, S.; Downing, M.; Grobov, A.; Martoff, C.J.; Ramirez, A.; Oleinik, A.; Unzhakov, E.V.; Price, D.; Galbiati, C.; Zykova, M.P.; Korga, G.; Giganti, C.; Mari, S.M.; Pallavicini, M.; Shchagin, A.; Pocar, A.; Ave, M.; Doria, L.; Westerdale, S.; Conde Vilda, E.; Barrillon, P.; Milincic, R.; Hallin, A.; Rescia, S.; Da Rocha Rolo, M.; Razeto, A.; Pietropaolo, F.; Celano, B.; Garcia Abia, P.; Busto, J.; Franceschi, A.; Cebrian, S.; Li, X.; Pellegrini, L.A.; Kuźniak, M.; Pantic, E.; Wang, Y.; Bussino, S.; Lai, M.; Grigoriev, G.Y.; Balmforth, Z.; Tonazzo, A.; Muratova, V.N.; Coccetti, F.; Cavuoti, S.; Caravati, M.; Wojcik, Ma.; De Candia, A.; Rivetti, A.; Raffaelli, F.; Usai, G.; Razeti, M.; Wheadon, R.J.; Williams, L.; Canci, N.; Mapelli, L.; Cela Ruiz, J.M.; Amaudruz, P.; Catalanotti, S.; Sandford, E.; Cadoni, M.; Nania, R.; Kondo, K.; Vallivilayil John, T.; Navrer Agasson, A.; Dadoun, O.; Giampaolo, R.A.; Rode, J.; Alexander, T.; Cataudella, V.; Graciani Diaz, R.; Miletic, T.; Picciau, E.; Rubbia, A.; Paoloni, E.; De Guido, G.; Savarese, C.; Basco, A.; Monroe, J.; Thorpe, T.N.; De Rosa, G.; Xiao, X.; La Commara, M.; Bondar, A.; Carlini, M.; Albuquerque, I.F.M.; Kubankin, A.; Kachru, P.; Langrock, S.; Samoylov, O.; De Filippis, G.; Horikawa, S.; Renshaw, A.L.; Giovanetti, G.K.; Guan, M.; Carnesecchi, F.; Gabriele, F.; Mróz, T.; Hugues, T.; Testera, G.; Muscas, C.; Sokolov, A.; Ianni, An.; Bottino, B.; Strickland, V.; Back, H.O.; Resnati, F.; Mozhevitina, E.N.; Margotti, A.; Kuss, M.; Rossi, M.; Tartaglia, R.; Poudel, S.S.; Marasciulli, A.; De Falco, A.; Wada, M.; Salatino, P.; Skorokhvatov, M.D.; Guo, C.; Pesudo, V.; Ragusa, F.; Cicalò, C.; Rescigno, M.; Pordes, S.; Alton, A.K.; Oleynikov, V.; Dolganov, G.; Colocci, M.; Sheshukov, A.; Poehlmann, D.M.; Funicello, N.; Santone, D.; Stracka, S.; Sulis, S.; Morrocchi, M.; Zichichi, A.

doi:10.1088/1475-7516/2021/03/043

Sensitivity of future liquid argon dark matter search experiments to core-collapse supernova neutrinos - Agnes, P. et al - arXiv:2011.07819

Time evolutions of neutrino luminosity (top) and mean energy (middle) and energy spectrum (bottom) from a core-collapse \LargeSolarMass\ SN for the different neutrino species, using Garching group 1-d simulations \cite{Bruenn_etal_2013}.

Nuclear recoil energy spectrum from neutrino interactions in LAr via \CEnNS\ from a core-collapse \LargeSolarMass\ supernova at \DSkSupernovaBaseline.

Top. Energy spectrum in number of ionization electrons (\nel) per unit of mass of neutrinos from 11-M$_{\odot}$ and 27-M$_{\odot}$ SNe and background from single electron events, \ArThirtyNine\ decays and external background from SiPMs. Bottom. Time evolution of signal and all background components (external background as expected in \Argo) by selecting events in the [3,100]~\nel\ energy range.

Neutrino detection efficiency via \CEnNS\ as a function of neutrino energy, for different \nel\ thresholds and below 100~\nel.

Top. \DSk\ and \Argo\ significance to 11-M$_{\odot}$ and 27-M$_{\odot}$ SNe (top) and to its neutronization burst only (bottom), as a function of the distance, assuming the standard background hypothesis (solid line) and (band) lower contamination of $^{39}$Ar up to a factor of 10 less. Vertical lines represent the distance from the Earth of the Milky Way center and farthest edge, and of Large (LMC) and Small (SMC) Magellanic Clouds.

Time profile of neutrinos from the accretion (left) and cooling (right) phases of a 27-M$_{\odot}$ SN at 10 kpc distance, as detected by \DSk\ and \Argo. The bands represent the statistical uncertainty.

Examples of fit of two toy Monte Carlo neutrino interaction samples in \DSk\ (left) and \Argo\ (right), generated in the [0.02, 8]~s time range, corresponding to the accretion and cooling phases from a 27 M$_{\odot}$ SN burst at 10~kpc.

\DSk\ and \Argo\ sensitivities to mean and integrated neutrino energies of a 27 M$_{\odot}$ SN burst at 10~kpc in the [0.1, 1]~s and [0.02, 8]~s. The two parameters are obtained by fitting 5$\times$10$^4$ toy MC samples with $\alpha_{T}$ equals to 2.3 and 2.0, with respect to each time range. Red crosses represent the true values from the Garching simulation.

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