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Search for hep solar neutrinos and the diffuse supernova neutrino background using all three phases of the Sudbury Neutrino Observatory

  • Author(s): Aharmim, B;
  • Ahmed, SN;
  • Anthony, AE;
  • Barros, N;
  • Beier, EW;
  • Bellerive, A;
  • Beltran, B;
  • Bergevin, M;
  • Biller, SD;
  • Blucher, E;
  • Bonventre, R;
  • Boudjemline, K;
  • Boulay, MG;
  • Cai, B;
  • Callaghan, EJ;
  • Caravaca, J;
  • Chan, YD;
  • Chauhan, D;
  • Chen, M;
  • Cleveland, BT;
  • Cox, GA;
  • Dai, X;
  • Deng, H;
  • Descamps, FB;
  • Detwiler, JA;
  • Doe, PJ;
  • Doucas, G;
  • Drouin, PL;
  • Dunford, M;
  • Elliott, SR;
  • Evans, HC;
  • Ewan, GT;
  • Farine, J;
  • Fergani, H;
  • Fleurot, F;
  • Ford, RJ;
  • Formaggio, JA;
  • Gagnon, N;
  • Gilje, K;
  • Goon, JTM;
  • Graham, K;
  • Guillian, E;
  • Habib, S;
  • Hahn, RL;
  • Hallin, AL;
  • Hallman, ED;
  • Harvey, PJ;
  • Hazama, R;
  • Heintzelman, WJ;
  • Heise, J;
  • Helmer, RL;
  • Hime, A;
  • Howard, C;
  • Huang, M;
  • Jagam, P;
  • Jamieson, B;
  • Jelley, NA;
  • Jerkins, M;
  • Keeter, KJ;
  • Klein, JR;
  • Kormos, LL;
  • Kos, M;
  • Kraus, C;
  • Krauss, CB;
  • Krüger, A;
  • Kutter, T;
  • Kyba, CCM;
  • Labe, K;
  • Land, BJ;
  • Lange, R;
  • Latorre, A;
  • Law, J;
  • Lawson, IT;
  • Lesko, KT;
  • Leslie, JR;
  • Levine, I;
  • Loach, JC;
  • Maclellan, R;
  • Majerus, S;
  • Mak, HB;
  • Maneira, J;
  • Martin, RD;
  • Mastbaum, A;
  • McCauley, N;
  • McDonald, AB;
  • McGee, SR;
  • Miller, ML;
  • Monreal, B;
  • Monroe, J;
  • Nickel, BG;
  • Noble, AJ;
  • O'Keeffe, HM;
  • Oblath, NS;
  • Okada, CE;
  • Ollerhead, RW;
  • Orebi Gann, GD;
  • Oser, SM;
  • Ott, RA;
  • Peeters, SJM;
  • Poon, AWP
  • et al.
Abstract

A search has been performed for neutrinos from two sources, the hep reaction in the solar pp fusion chain and the νe component of the diffuse supernova neutrino background (DSNB), using the full dataset of the Sudbury Neutrino Observatory with a total exposure of 2.47 kton-years after fiducialization. The hep search is performed using both a single-bin counting analysis and a likelihood fit. We find a best-fit flux that is compatible with solar model predictions while remaining consistent with zero flux, and set a one-sided upper limit of φhep<30×103 cm-2 s-1 [90% credible interval (CI)]. No events are observed in the DSNB search region, and we set an improved upper bound on the νe component of the DSNB flux of φνeDSNB<19 cm-2 s-1 (90% CI) in the energy range 22.9

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